@article{ji_curtis_storm_chandra_c. schlaufman_g. stassun_heger_pignatari_price-whelan_bergemann_et al._2024, title={Spectacular Nucleosynthesis from Early Massive Stars}, volume={961}, ISSN={["2041-8213"]}, DOI={10.3847/2041-8213/ad19c4}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL LETTERS}, author={Ji, Alexander P. and Curtis, Sanjana and Storm, Nicholas and Chandra, Vedant and C. Schlaufman, Kevin and G. Stassun, Keivan and Heger, Alexander and Pignatari, Marco and Price-Whelan, Adrian M. and Bergemann, Maria and et al.}, year={2024}, month={Feb} }
 @article{wolfe_frohlich_miller_torres-forne_cerda-duran_2023, title={Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae}, volume={954}, ISSN={["1538-4357"]}, url={https://doi.org/10.3847/1538-4357/ace693}, DOI={10.3847/1538-4357/ace693}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Wolfe, Noah E. and Frohlich, Carla and Miller, Jonah M. and Torres-Forne, Alejandro and Cerda-Duran, Pablo}, year={2023}, month={Sep} }
 @article{curtis_miller_frohlich_sprouse_lloyd-ronning_mumpower_2023, title={Nucleosynthesis in Outflows from Black Hole-Neutron Star Merger Disks with Full GR(nu)RMHD}, volume={945}, ISSN={["2041-8213"]}, url={https://doi.org/10.3847/2041-8213/acba16}, DOI={10.3847/2041-8213/acba16}, abstractNote={Abstract}, number={1}, journal={ASTROPHYSICAL JOURNAL LETTERS}, author={Curtis, Sanjana and Miller, Jonah M. and Frohlich, Carla and Sprouse, Trevor and Lloyd-Ronning, Nicole and Mumpower, Matthew}, year={2023}, month={Mar} }
 @article{reichert_winteler_korobkin_arcones_bliss_eichler_frischknecht_froehlich_hirschi_jacobi_et al._2023, title={The Nuclear Reaction Network WinNet}, volume={268}, ISSN={["1538-4365"]}, url={https://doi.org/10.3847/1538-4365/acf033}, DOI={10.3847/1538-4365/acf033}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES}, author={Reichert, M. and Winteler, C. and Korobkin, O. and Arcones, A. and Bliss, J. and Eichler, M. and Frischknecht, U. and Froehlich, C. and Hirschi, R. and Jacobi, M. and et al.}, year={2023}, month={Oct} }
 @article{meskhi_wolfe_dai_frohlich_miller_wong_vilalta_2022, title={A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae}, volume={932}, ISSN={["2041-8213"]}, url={https://doi.org/10.3847/2041-8213/ac7054}, DOI={10.3847/2041-8213/ac7054}, abstractNote={Abstract}, number={1}, journal={ASTROPHYSICAL JOURNAL LETTERS}, author={Meskhi, Mikhail M. and Wolfe, Noah E. and Dai, Zhenyu and Frohlich, Carla and Miller, Jonah M. and Wong, Raymond K. W. and Vilalta, Ricardo}, year={2022}, month={Jun} }
 @article{schatz_becerril reyes_best_brown_chatziioannou_chipps_deibel_ezzeddine_galloway_hansen_et al._2022, title={Horizons: nuclear astrophysics in the 2020s and Beyond}, volume={49}, ISSN={["1361-6471"]}, DOI={10.1088/1361-6471/ac8890}, abstractNote={Abstract}, number={11}, journal={Journal of Physics G: Nuclear and Particle Physics}, author={Schatz, H. and Becerril Reyes, A.D. and Best, A. and Brown, E.F. and Chatziioannou, K. and Chipps, K.A. and Deibel, C.M. and Ezzeddine, R. and Galloway, D.K. and Hansen, C.J. and et al.}, year={2022}, pages={110502} }
 @article{myers_cooper_warren_kneller_mclaughlin_richers_grohs_frohlich_2022, title={Neutrino flavor mixing with moments}, volume={105}, ISSN={["2470-0029"]}, url={https://doi.org/10.1103/PhysRevD.105.123036}, DOI={10.1103/PhysRevD.105.123036}, abstractNote={The successful transition from core-collapse supernova simulations using classical neutrino transport to simulations using quantum neutrino transport will require the development of methods for calculating neutrino flavor transformations that mitigate the computational expense. One potential approach is the use of angular moments of the neutrino field, which has the added appeal that there already exist simulation codes which make use of moments for classical neutrino transport. Evolution equations for quantum moments based on the quantum kinetic equations can be straightforwardly generalized from the evolution of classical moments based on the Boltzmann equation. We present an efficient implementation of neutrino transformation using quantum angular moments in the free streaming, spherically symmetric bulb model. We compare the results against analytic solutions and the results from more exact multi-angle neutrino flavor evolution calculations. We find that our moment-based methods employing scalar closures predict, with good accuracy, the onset of collective flavor transformations seen in the multi-angle results. However in some situations they overestimate the coherence of neutrinos traveling along different trajectories. More sophisticated quantum closures may improve the agreement between the inexpensive moment-based methods and the multi-angle approach.}, number={12}, journal={PHYSICAL REVIEW D}, author={Myers, McKenzie and Cooper, Theo and Warren, MacKenzie and Kneller, Jim and McLaughlin, Gail and Richers, Sherwood and Grohs, Evan and Frohlich, Carla}, year={2022}, month={Jun} }
 @article{ghosh_wolfe_frohlich_2022, title={PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. V. Equation of State Dependency of Explosion Properties, Nucleosynthesis Yields, and Compact Remnants}, volume={929}, ISSN={["1538-4357"]}, url={https://doi.org/10.3847/1538-4357/ac4d20}, DOI={10.3847/1538-4357/ac4d20}, abstractNote={Abstract}, number={1}, journal={ASTROPHYSICAL JOURNAL}, publisher={American Astronomical Society}, author={Ghosh, Somdutta and Wolfe, Noah and Frohlich, Carla}, year={2022}, month={Apr} }
 @article{meskhi_wolfe_dai_frohlich_miller_wong_vilalta_2021, title={A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae}, volume={11}, journal={arXiv e-prints}, author={Meskhi, Mikhail M. and Wolfe, Noah E. and Dai, Zhenyu and Frohlich, Carla and Miller, Jonah M. and Wong, Raymond K. W. and Vilalta, Ricardo}, year={2021}, month={Nov}, pages={arXiv:2111.01815} }
 @article{curtis_wolfe_frohlich_miller_wollaeger_ebinger_2021, title={Core-collapse Supernovae: From Neutrino-driven 1D Explosions to Light Curves and Spectra}, volume={921}, ISSN={["1538-4357"]}, url={http://dx.doi.org/10.3847/1538-4357/ac0dc5}, DOI={10.3847/1538-4357/ac0dc5}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, publisher={American Astronomical Society}, author={Curtis, Sanjana and Wolfe, Noah and Frohlich, Carla and Miller, Jonah M. and Wollaeger, Ryan and Ebinger, Kevin}, year={2021}, month={Nov} }
 @article{pushing core-collapse supernovae to explosions in spherical symmetry v: equation of state dependency of explosion properties, nucleosynthesis yields, and compact remnants_2021, year={2021}, month={Jul} }
 @article{stone_johnson_blondin_watson_borkowski_frohlich_seitenzahl_reynolds_2021, title={Type Ia Supernova Models: Asymmetric Remnants and Supernova Remnant G1.9+0.3}, volume={923}, ISSN={["1538-4357"]}, url={http://dx.doi.org/10.3847/1538-4357/ac300f}, DOI={10.3847/1538-4357/ac300f}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, publisher={American Astronomical Society}, author={Stone, Alice G. and Johnson, Heather T. and Blondin, John M. and Watson, Richard A. and Borkowski, Kazimierz J. and Frohlich, Carla and Seitenzahl, Ivo R. and Reynolds, Stephen P.}, year={2021}, month={Dec} }
 @article{stapleford_froehlich_kneller_2020, title={Coupling neutrino oscillations and simulations of core-collapse supernovae}, volume={102}, ISSN={["1550-2368"]}, url={http://dx.doi.org/10.1103/physrevd.102.081301}, DOI={10.1103/physrevd.102.081301}, abstractNote={At the present time even the most sophisticated, multi-dimensional simulations of core-collapse supernovae do not (self-consistently) include neutrino flavor transformation. This physics is missing despite the importance of neutrinos in the core-collapse explosion paradigm. Because of this dependence, any flavor transformation that occurs in the region between the proto-neutron star and the shock could result in major effects upon the dynamics of the explosion. We present the first hydrodynamic core-collapse supernova simulation which simultaneously includes flavor transformation of the free-streaming neutrinos in the neutrino transport. These oscillation calculations are dynamically updated and evolve self-consistently alongside the hydrodynamics. Using a $M=20\;{\rm M_{\odot}}$ progenitor, we find that while the oscillations have an effect on the neutrino emission and the heating rates, flavor transformation alone does not lead to a successful explosion of this progenitor in spherical symmetry.}, number={8}, journal={PHYSICAL REVIEW D}, publisher={American Physical Society (APS)}, author={Stapleford, Charles J. and Froehlich, Carla and Kneller, James P.}, year={2020}, month={Oct} }
 @article{mattoni_ahn_frohlich_frohlich_2020, title={Exploring the relationship between geomagnetic activity and human heart rate variability}, volume={120}, ISSN={["1439-6327"]}, url={http://dx.doi.org/10.1007/s00421-020-04369-7}, DOI={10.1007/s00421-020-04369-7}, abstractNote={Both geomagnetic and solar activity fluctuate over time and have been proposed to affect human physiology. Heart rate variability (HRV) has substantial health implications regarding the ability to adapt to stressors and has been shown to be altered in many cardiovascular and neurological disorders. Intriguingly, previous work found significant, strong correlations between HRV and geomagnetic/solar activity. The purpose of this study to replicate these findings. We simultaneously measured HRV during a 30-day period. We recruited 20 healthy participants and measured their HRV for a 30-day period. We also collected geomagnetic and solar activity during this period for investigating their relationship with the HRV data. In agreement with previous work, we found several significant correlations between short-term HRV and geophysical time-series. However, after correction for autocorrelation, which is inherent in time-series, the only significant results were an increase in very low frequency during higher local geomagnetic activity and a geomagnetic anticipatory decrease in heart rate a day before the higher global geomagnetic activity. Both correlations were very low. The loss of most significant effects after this correction suggests that previous findings may be a result of autocorrelation. A further note of caution is required since our and the previous studies in the field do not correct for multiple comparisons given the exploratory analysis strategy. We thus conclude that the effects of geomagnetic and solar activity are (if present) most likely of very small effect size and we question the validity of the previous studies given the methodological concerns we have uncovered with our work.}, number={6}, journal={EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY}, publisher={Springer Science and Business Media LLC}, author={Mattoni, Matthew and Ahn, Sangtae and Frohlich, Carla and Frohlich, Flavio}, year={2020}, month={Jun}, pages={1371–1381} }
 @article{ebinger_curtis_ghosh_fröhlich_hempel_perego_liebendörfer_thielemann_2020, title={PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. IV. Explodability, Remnant Properties, and Nucleosynthesis Yields of Low-metallicity Stars*}, url={https://doi.org/10.3847/1538-4357/ab5dcb}, DOI={10.3847/1538-4357/ab5dcb}, abstractNote={Abstract}, journal={The Astrophysical Journal}, author={Ebinger, Kevin and Curtis, Sanjana and Ghosh, Somdutta and Fröhlich, Carla and Hempel, Matthias and Perego, Albino and Liebendörfer, Matthias and Thielemann, Friedrich-Karl}, year={2020}, month={Jan} }
 @article{timmes_fryer_timmes_hungerford_couture_adams_aoki_arcones_arnett_auchettl_et al._2019, title={Catching Element Formation In The Act ; The Case for a New MeV Gamma-Ray Mission: Radionuclide Astronomy in the 2020s}, journal={Bulletin of the American Astronomical Society}, author={Timmes, Frank and Fryer, Chris and Timmes, Frank and Hungerford, Aimee L. and Couture, Aaron and Adams, Fred and Aoki, Wako and Arcones, Almudena and Arnett, David and Auchettl, Katie and et al.}, year={2019}, month={May} }
 @article{frohlich_curtis_ebinger_ghosh_menon_heger_perego_thielemann_2019, title={Nucleosynthesis for SN 1987A from single-star and binary-merger progenitors}, volume={46}, ISSN={["1361-6471"]}, url={https://doi.org/10.1088/1361-6471/ab1ff7}, DOI={10.1088/1361-6471/ab1ff7}, abstractNote={We apply the parametrized, spherically symmetric explosion method PUSH to two sets of pre-explosion models suitable for SN 1987A: blue supergiants (BSGs) resulting from the merger of a main sequence star with a giant and red supergiants (RSGs) representing the end point of single-star stellar evolution. For each model, we perform a calibration of the PUSH method to the observational properties of SN 1987A and calculate the detailed explosive nucleosynthesis yields. We find that such a calibration to SN 1987A is only possible for one of the BSG models. We compare the yields from this model with the yields from the best-fit RSG model. The largest differences are found for nuclei in the mass range of 20 ≤ A ≤ 40 which are mostly synthesized pre-explosion. We predict a neutron star with a gravitational mass of 1.48 M ⊙ from the BSG model and a neutron star of 1.41 M ⊙ from the RSG model.}, number={8}, journal={JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS}, author={Frohlich, C. and Curtis, S. and Ebinger, K. and Ghosh, S. and Menon, A. and Heger, A. and Perego, A. and Thielemann, F-K}, year={2019}, month={Aug} }
 @article{ebinger_curtis_froehlich_hempel_perego_liebendoerfer_thielemann_2019, title={PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. II. Explodability and Remnant Properties}, volume={870}, ISSN={["1538-4357"]}, url={https://doi.org/10.3847/1538-4357/aae7c9}, DOI={10.3847/1538-4357/aae7c9}, abstractNote={Abstract}, number={1}, journal={ASTROPHYSICAL JOURNAL}, author={Ebinger, Kevin and Curtis, Sanjana and Froehlich, Carla and Hempel, Matthias and Perego, Albino and Liebendoerfer, Matthias and Thielemann, Friedrich-Karl}, year={2019}, month={Jan} }
 @article{curtis_ebinger_fröhlich_hempel_perego_liebendörfer_thielemann_2019, title={PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields}, url={https://doi.org/10.3847/1538-4357/aae7d2}, DOI={10.3847/1538-4357/aae7d2}, abstractNote={Abstract}, journal={The Astrophysical Journal}, author={Curtis, Sanjana and Ebinger, Kevin and Fröhlich, Carla and Hempel, Matthias and Perego, Albino and Liebendörfer, Matthias and Thielemann, Friedrich-Karl}, year={2019}, month={Jan} }
 @article{chatzopoulos_gilmer_wollaeger_frohlich_even_2019, title={Synthetic Spectra of Pair-instability Supernovae in 3D}, volume={875}, ISSN={["1538-4357"]}, url={https://doi.org/10.3847/1538-4357/ab1082}, DOI={10.3847/1538-4357/ab1082}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Chatzopoulos, E. and Gilmer, Matthew S. and Wollaeger, Ryan T. and Frohlich, Carla and Even, Wesley P.}, year={2019}, month={Apr} }
 @book{frohlich_2019, title={The Origin of Chemical Elements: Connecting Laboratory Nuclear Astrophysics with Astronomical Observations through Nucleosynthesis Modeling}, url={https://doi.org/10.2172/1496039}, DOI={10.2172/1496039}, abstractNote={The final report for the award “The Origin of Chemical Elements: Connecting Laboratory Nuclear Astrophysics with Astronomical Observations through Nucleosynthesis Modeling” is given. The goals of this work were the following: Develop new effective models for core-collapse supernovae that include all relevant physics and remain computationally efficient; Implement these models in computer codes to study the outcome of stellar collapse; Increase the realism of nucleosynthesis predictions for supernovae and other hot, dense environments; Study the synthesis of the lightest heavy elements to extract information about the conditions under which they are synthesized, to identify the critical nuclear physics inputs and to provide support and guidance for nuclear physics experiments; and finally, simulate the explosions of the most massive stars to predict their light curves and other signals. Accomplishments made in these areas are described.}, institution={Office of Scientific and Technical Information  (OSTI)}, author={Frohlich, Carla}, year={2019}, month={Feb} }
 @article{nishimura_rauscher_hirschi_cescutti_murphy_fröhlich_2019, title={Uncertainties in νp-process nucleosynthesis from Monte Carlo variation of reaction rates}, volume={489}, url={http://dx.doi.org/10.1093/mnras/stz2104}, DOI={10.1093/mnras/stz2104}, abstractNote={ABSTRACT}, number={1}, journal={Monthly Notices of the Royal Astronomical Society}, publisher={Oxford University Press (OUP)}, author={Nishimura, N and Rauscher, T and Hirschi, R and Cescutti, G and Murphy, A St J and Fröhlich, C}, year={2019}, month={Aug}, pages={1379–1396} }
 @article{wehmeyer_froehlich_cote_pignatari_thielemann_2019, title={Using failed supernovae to constrain the Galactic r-process element production}, volume={487}, ISSN={["1365-2966"]}, url={https://doi.org/10.1093/mnras/stz1310}, DOI={10.1093/mnras/stz1310}, abstractNote={ABSTRACT}, number={2}, journal={MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}, publisher={Oxford University Press (OUP)}, author={Wehmeyer, B. and Froehlich, C. and Cote, B. and Pignatari, M. and Thielemann, F. -K.}, year={2019}, month={Aug}, pages={1745–1753} }
 @inproceedings{gastis_perdikakis_fröhlich_alt_davison_dombos_estrade_falduto_horoi_lyons_et al._2018, title={A new experimental technique for measuring (p,n) reactions relevant to the neutrino-p process in the ReA3 facility}, booktitle={APS April Meeting Abstracts}, author={Gastis, Panagiotis and Perdikakis, George and Fröhlich, Carla and Alt, Daniel and Davison, Jacob and Dombos, Alexander and Estrade, Alfredo and Falduto, Ashton and Horoi, Mihai and Lyons, Stephanie and et al.}, year={2018} }
 @inproceedings{ebinger_perego_hempel_fröhlich_eichler_casanova_liebendörfer_thielemann_2018, title={Explosion dynamics of parametrized spherically symmetric core-collapse supernova simulations}, DOI={10.1088/1742-6596/940/1/012039}, abstractNote={We analyze the explosion properties and dynamics of spherically symmetric, parametrized core-collapse supernovae derived with the new PUSH method. To this end, we explore the progenitor mass range between 18 and 21 M⨀. We find that it is possible to suggest a distinction between low and high compactness progenitors. We discuss the differences on the example of two reference runs.}, booktitle={Journal of Physics Conference Series}, author={Ebinger, K. and Perego, A. and Hempel, M. and Fröhlich, C. and Eichler, M. and Casanova, J. and Liebendörfer, M. and Thielemann, F. -K.}, year={2018}, month={Jan} }
 @inproceedings{eichler_perego_hempel_fröhlich_ebinger_casanova_liebendörfer_thielemann_2018, title={Explosive nucleosynthesis in core-collapse supernovae and the titanium problem}, DOI={10.1088/1742-6596/940/1/012040}, abstractNote={Based on a new mechanism to drive spherically symmetric core-collapse supernovae, PUSH, we perform full network nucleosynthesis calculations for different progenitors. While the 56–58Ni yields match the observational data very well for certain progenitors, the ejected titanium masses in our calculations are lower than the values inferred from observations. We demonstrate the dependence of ejecta composition on the progenitor structure and the mass cut. Furthermore, we discuss possible solutions to the well-known problem of titanium underproduction.}, booktitle={Journal of Physics Conference Series}, author={Eichler, M. and Perego, A. and Hempel, M. and Fröhlich, C. and Ebinger, K. and Casanova, J. and Liebendörfer, M. and Thielemann, F. -K.}, year={2018}, month={Jan} }
 @article{xing_li_zhang_zhou_wang_litvinov_blaum_wanajo_kubono_martinez-pinedo_et al._2018, title={Mass measurements of neutron-deficient Y, Zr, and Nb isotopes and their impact on rp and nu p nucleosynthesis processes}, volume={781}, ISSN={["1873-2445"]}, url={http://dx.doi.org/10.1016/j.physletb.2018.04.009}, DOI={10.1016/j.physletb.2018.04.009}, abstractNote={Using isochronous mass spectrometry at the experimental storage ring CSRe in Lanzhou, the masses of $^{82}$Zr and $^{84}$Nb were measured for the first time with an uncertainty of $\sim 10$ keV, and the masses of $^{79}$Y, $^{81}$Zr, and $^{83}$Nb were re-determined with a higher precision. %The latter differ significantly from their literature values. The latter are significantly less bound than their literature values. Our new and accurate masses remove the irregularities of the mass surface in this region of the nuclear chart. Our results do not support the predicted island of pronounced low $\alpha$ separation energies for neutron-deficient Mo and Tc isotopes, making the formation of Zr-Nb cycle in the $rp$-process unlikely. The new proton separation energy of $^{83}$Nb was determined to be 490(400)~keV smaller than that in the Atomic Mass Evaluation 2012. This partly removes the overproduction of the $p$-nucleus $^{84}$Sr relative to the neutron-deficient molybdenum isotopes in the previous $\nu p$-process simulations.}, journal={PHYSICS LETTERS B}, author={Xing, Y. M. and Li, K. A. and Zhang, Y. H. and Zhou, X. H. and Wang, M. and Litvinov, Yu. A. and Blaum, K. and Wanajo, S. and Kubono, S. and Martinez-Pinedo, G. and et al.}, year={2018}, month={Jun}, pages={358–363} }
 @inproceedings{gilmer_kozyreva_hirschi_fröhlich_wright_kneller_yusof_2018, title={Multidimensional pair-instability supernova simulations and their multi-messenger signals}, booktitle={American Astronomical Society Meeting Abstracts #231}, author={Gilmer, Matthew and Kozyreva, Alexandra and Hirschi, Raphael and Fröhlich, Carla and Wright, Warren and Kneller, James P. and Yusof, Norhasliza}, year={2018}, month={Jan} }
 @inproceedings{fröhlich_perego_hempe_ebinger_eichler_casanova_liebendörfer_thielemann_2018, title={PUSHing core-collapse simulations to explosion}, DOI={10.1088/1742-6596/940/1/012001}, abstractNote={We report on the PUSH method for artificially triggering core-collapse supernova explosions of massive stars in spherical symmetry. The PUSH method increases the energy deposition in the gain region proportionally to the heavy flavor neutrino fluxes.We summarize the parameter dependence of the method and calibrate PUSH to reproduce SN 1987A observables. We identify a best-fit progenitor and set of parameters that fit the explosion properties of SN 1987A, assuming 0.1 M⊙ of fallback. For the explored progenitor range of 18-21 M⊙, we find correlations between explosion properties and the compactness of the progenitor model.}, booktitle={Journal of Physics Conference Series}, author={Fröhlich, C. and Perego, A. and Hempe, M. and Ebinger, K. and Eichler, M. and Casanova, J. and Liebendörfer, M. and Thielemann, F. -K.}, year={2018}, month={Jan} }
 @inproceedings{gilmer_kozyreva_hirschi_fröhlich_2017, title={Effects of Dimensionality on Pair-Instability Supernova Explosions}, DOI={10.7566/JPSCP.14.020601}, abstractNote={Since the emergence of the new class of extremely bright transients, super-luminous supernovae (SLSNe), three main mechanisms to power their light curves (LCs) have been discussed. They are the spin-down of a magnetar, interaction with circumstellar material, and the decay of large amounts of radioactive nickel in pair-instability supernovae (PISNe). Given the high degree of diversity seen within the class, it is possible that all three mechanisms are at work. PISN models can be self- consistently simulated from the main sequence phase of very massive stars (VMS) through to their explosion. These models robustly predict large amounts of radioactive nickel and thus very luminous SN events. However, PISN model LCs evolve more slowly than even the slowest evolving SLSNe. Multidimensional effects on the ejecta structure, specifically the mixing of radioactive nickel out to large radii, could alleviate this discrepancy with observation. Here we explore the multidimensional effects on the LC evolution by simulating the explosion phase in 1D, 2D, and 3D. We find that the ejecta from the multidimensional simulations have slightly shallower abundance gradients due to mixing at shell boundaries. We compute synthetic LCs whose shapes show no discernible differences due to the multidimensional effects.}, booktitle={14th International Symposium on Nuclei in the Cosmos (NIC2016)}, author={Gilmer, Matthew S. and Kozyreva, Alexandra and Hirschi, Raphael and Fröhlich, Carla}, year={2017} }
 @inproceedings{ebinger_sinha_fröhlich_perego_hempel_eichler_casanova_liebendörfer_thielemann_2017, title={Explosion Dynamics of Parametrized Spherically Symmetric Core-Collapse Supernova Simulations}, DOI={10.7566/JPSCP.14.020611}, abstractNote={We report on a method, PUSH, for triggering core-collapse supernova (CCSN) explosions of massive stars in spherical symmetry. This method provides a framework to study many important aspects of core collapse supernovae: the effects of the shock passage through the star, explosive supernova nucleosynthesis and the progenitor-remnant connection. Here we give an overview of the method, compare the results to multi-dimensional simulations and investigate the effects of the progenitor and the equation of state on black hole formation.}, booktitle={14th International Symposium on Nuclei in the Cosmos (NIC2016)}, author={Ebinger, Kevin and Sinha, Sanjana and Fröhlich, Carla and Perego, Albino and Hempel, Matthias and Eichler, Marius and Casanova, Jordi and Liebendörfer, Matthias and Thielemann, Friedrich-Karl}, year={2017} }
 @article{kozyreva_gilmer_hirschi_frohlich_blinnikov_wollaeger_noebauer_rossum_heger_even_et al._2017, title={Fast evolving pair-instability supernova models: evolution, explosion, light curves}, volume={464}, ISSN={["1365-2966"]}, url={http://dx.doi.org/10.1093/mnras/stw2562}, DOI={10.1093/mnras/stw2562}, abstractNote={With an increasing number of superluminous supernovae (SLSNe) discovered the question of their origin remains open and causes heated debates in the supernova community. Currently, there are three proposed mechanisms for SLSNe: (1) pair-instability supernovae (PISN), (2) magnetar-driven supernovae, and (3) models in which the supernova ejecta interacts with a circumstellar material ejected before the explosion. Based on current observations of SLSNe, the PISN origin has been disfavoured for a number of reasons. Many PISN models provide overly broad light curves and too reddened spectra, because of massive ejecta and a high amount of nickel. In the current study we re-examine PISN properties using progenitor models computed with the GENEC code. We calculate supernova explosions with FLASH and light curve evolution with the radiation hydrodynamics code STELLA. We find that high-mass models (200 and 250 solar masses) at relatively high metallicity (Z=0.001) do not retain hydrogen in the outer layers and produce relatively fast evolving PISNe Type I and might be suitable to explain some SLSNe. We also investigate uncertainties in light curve modelling due to codes, opacities, the nickel-bubble effect and progenitor structure and composition.}, number={3}, journal={MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}, author={Kozyreva, Alexandra and Gilmer, Matthew and Hirschi, Raphael and Frohlich, Carla and Blinnikov, Sergey and Wollaeger, Ryan T. and Noebauer, Ulrich M. and Rossum, Daniel R. and Heger, Alexander and Even, Wesley P. and et al.}, year={2017}, month={Jan}, pages={2854–2865} }
 @inproceedings{gastis_perdikakis_frohlich_alt_horoi_kontos_liddick_lin_montes_nikas_et al._2017, title={Investigating the Role of νp-Process: Preparations for the Measurement of the <SUP>56</SUP>Co(p, n)<SUP>56</SUP>Ni Reaction}, DOI={10.7566/JPSCP.14.020511}, abstractNote={A cross section measurement of the 56 Co(p,n) 56 Ni reaction in inverse kinematics, will take place in the new ReA3 facility at the National Superconducting Cyclotron Laboratory (NSCL).The result will constrain the reaction rate of the 56 Ni(n,p) 56 Co reaction and will provide significant information about the role of the νp-process in the synthesis of heavy elements.In this report, a possible test experiment in the ReA3 setup using a 40 Ar beam is investigated.The experimental technique and results from beam dynamics simulations for the 40 Ar(p,n) 40 K reaction are shown.}, booktitle={14th International Symposium on Nuclei in the Cosmos (NIC2016)}, author={Gastis, Panagiotis and Perdikakis, George and Frohlich, Carla and Alt, Daniel and Horoi, Mihai and Kontos, Antonios and Liddick, Sean and Lin, Ling-Ying and Montes, Fernando and Nikas, Stylianos and et al.}, year={2017} }
 @article{wright_gilmer_frohlich_kneller_2017, title={Neutrino signal from pair-instability supernovae}, volume={96}, ISSN={["2470-0029"]}, url={http://dx.doi.org/10.1103/physrevd.96.103008}, DOI={10.1103/physrevd.96.103008}, abstractNote={A very massive star with a carbon-oxygen core in the range of $64$ M$_{\odot}<M_{\mathrm{CO}}<133$ M$_{\odot}$ is expected to undergo a very different kind of explosion known as a pair instability supernova. Pair instability supernovae are candidates for superluminous supernovae due to the prodigious amounts of radioactive elements they create. While the basic mechanism for the explosion is understood, how a star reaches a state is not, thus observations of a nearby pair-instability supernova would allow us to test current models of stellar evolution at the extreme of stellar masses. Much will be sought within the electromagnetic radiation we detect from such a supernova but we should not forget that the neutrinos from a pair-instability supernova contain unique signatures of the event that unambiguously identify this type of explosion. We calculate the expected neutrino flux at Earth from two, one-dimensional pair-instability supernova simulations which bracket the mass range of stars which explode by this mechanism taking into account the full time and energy dependence of the neutrino emission and the flavor evolution through the outer layers of the star. We calculate the neutrino signals in five different detectors chosen to represent present or near future designs. We find the more massive progenitors explode as pair-instability supernova which can easily be detected in multiple different neutrino detectors at the `standard' supernova distance of $10\;{\rm kpc}$ producing several events in DUNE, JUNE and SuperKamiokande, while the lightest progenitors only produce a handful of events (if any) in the same detectors. The proposed HyperKamiokande detector would detect neutrinos from a large pair-instability supernova as far as $\sim 50\;{\rm kpc}$ allowing it to reach the Megallanic Clouds and the several very high mass stars known to exist there.}, number={10}, journal={PHYSICAL REVIEW D}, author={Wright, Warren P. and Gilmer, Matthew S. and Frohlich, Carla and Kneller, James P.}, year={2017}, month={Nov} }
 @inproceedings{fröhlich_hatcher_perdikakis_nikas_2017, title={Nuclear Reactions and the ν p-Process}, DOI={10.7566/JPSCP.14.010505}, booktitle={14th International Symposium on Nuclei in the Cosmos (NIC2016)}, author={Fröhlich, Carla and Hatcher, Daniel and Perdikakis, Georgios and Nikas, Stylianos}, year={2017} }
 @inproceedings{sinha_ebinger_frohlich_perego_hempel_liebendoerfer_thielemann_2017, title={PUSHing Core-Collapse Supernovae to Explosions in Spherical Symmetry: Explodability and Nucleosynthesis Yields}, booktitle={APS April Meeting Abstracts}, author={Sinha, Sanjana and Ebinger, Kevin and Frohlich, Carla and Perego, Albino and Hempel, Matthias and Liebendoerfer, Matthias and Thielemann, F. -K.}, year={2017}, month={Jan} }
 @inproceedings{sinha_fröhlich_ebinger_perego_hempel_eichler_liebendörfer_thielemann_2017, title={PUSHing Core-Collapse Supernovae to Explosions in Spherical Symmetry: Nucleosynthesis Yields}, DOI={10.7566/JPSCP.14.020608}, abstractNote={Core-collapse supernovae (CCSNe) are the extremely energetic deaths of massive stars. They play a vital role in the synthesis and dissemination of many heavy elements in the universe. In the past, CCSN nucleosynthesis calculations have relied on artificial explosion methods that do not adequately capture the physics of the innermost layers of the star. The PUSH method, calibrated against SN1987A, utilizes the energy of heavy-flavor neutrinos emitted by the proto-neutron star (PNS) to trigger parametrized explosions. This makes it possible to follow the consistent evolution of the PNS and to ensure a more accurate treatment of the electron fraction of the ejecta. Here, we present the Iron group nucleosynthesis results for core-collapse supernovae, exploded with PUSH, for two different progenitor series. Comparisons of the calculated yields to observational metal-poor star data are also presented. Nucleosynthesis yields will be calculated for all elements and over a wide range of progenitor masses. These yields can be immensely useful for models of galactic chemical evolution.}, booktitle={14th International Symposium on Nuclei in the Cosmos (NIC2016)}, author={Sinha, Sanjana and Fröhlich, Carla and Ebinger, Kevin and Perego, Albino and Hempel, Matthias and Eichler, Marius and Liebendörfer, Matthias and Thielemann, Friedrich-Karl}, year={2017} }
 @article{gilmer_kozyreva_hirschi_fröhlich_yusof_2017, title={Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves}, volume={846}, url={https://doi.org/10.3847/1538-4357/aa8461}, DOI={10.3847/1538-4357/aa8461}, abstractNote={Abstract}, number={2}, journal={The Astrophysical Journal}, author={Gilmer, Matthew S. and Kozyreva, Alexandra and Hirschi, Raphael and Fröhlich, Carla and Yusof, Norhasliza}, year={2017}, month={Sep} }
 @inproceedings{perdikakis_gastis_frohlich_horoi_kontos_liddick_lin_montes_nikas_redpath_et al._2017, title={Towards an experimental constraint for the <SUP>56</SUP>Ni(n,p)<SUP>56</SUP>Co reaction rate which is key for the astrophysical νp process}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Perdikakis, Georgios and Gastis, Panagiotis and Frohlich, Carla and Horoi, Mihai and Kontos, Antonios and Liddick, Sean and Lin, Ling-Ying and Montes, Fernando and Nikas, Stelios and Redpath, Thomas and et al.}, year={2017}, month={Sep} }
 @article{arcones_bardayan_beers_bernstein_blackmon_messer_brown_brown_brune_champagne_et al._2017, title={White paper on nuclear astrophysics and low energy nuclear physics Part 1: Nuclear astrophysics}, volume={94}, ISSN={["1873-2224"]}, url={http://dx.doi.org/10.1016/j.ppnp.2016.12.003}, DOI={10.1016/j.ppnp.2016.12.003}, abstractNote={This white paper informs the nuclear astrophysics community and funding agencies about the scientific directions and priorities of the field and provides input from this community for the 2015 Nuclear Science Long Range Plan. It summarizes the outcome of the nuclear astrophysics town meeting that was held on August 21–23, 2014 in College Station at the campus of Texas A&M University in preparation of the NSAC Nuclear Science Long Range Plan. It also reflects the outcome of an earlier town meeting of the nuclear astrophysics community organized by the Joint Institute for Nuclear Astrophysics (JINA) on October 9–10, 2012 Detroit, Michigan, with the purpose of developing a vision for nuclear astrophysics in light of the recent NRC decadal surveys in nuclear physics (NP2010) and astronomy (ASTRO2010). The white paper is furthermore informed by the town meeting of the Association of Research at University Nuclear Accelerators (ARUNA) that took place at the University of Notre Dame on June 12–13, 2014. In summary we find that nuclear astrophysics is a modern and vibrant field addressing fundamental science questions at the intersection of nuclear physics and astrophysics. These questions relate to the origin of the elements, the nuclear engines that drive life and death of stars, and the properties of dense matter. A broad range of nuclear accelerator facilities, astronomical observatories, theory efforts, and computational capabilities are needed. With the developments outlined in this white paper, answers to long standing key questions are well within reach in the coming decade.}, journal={PROGRESS IN PARTICLE AND NUCLEAR PHYSICS}, author={Arcones, Almudena and Bardayan, Dan W. and Beers, Timothy C. and Bernstein, Lee A. and Blackmon, Jeffrey C. and Messer, Bronson and Brown, B. Alex and Brown, Edward F. and Brune, Carl R. and Champagne, Art E. and et al.}, year={2017}, month={May}, pages={1–67} }
 @unpublished{arcones_bardayan_beers_berstein_blackmon_messer_brown_brown_brune_champagne_et al._2016, title={White Paper on Nuclear Astrophysics}, journal={arXiv e-prints}, author={Arcones, Almudena and Bardayan, Dan W. and Beers, Timothy C. and Berstein, Lee A. and Blackmon, Jeffrey C. and Messer, Bronson and Brown, B. Alex and Brown, Edward F. and Brune, Carl R. and Champagne, Art E. and et al.}, year={2016}, month={Mar} }
 @article{shafer_engel_frohlich_mclaughlin_mumpower_surman_2016, title={beta decay of deformed r-process nuclei near A=80 and A=160, including odd-A and odd-odd nuclei, with the Skyrme finite-amplitude method}, volume={94}, ISSN={["2469-9993"]}, url={http://dx.doi.org/10.1103/physrevc.94.055802}, DOI={10.1103/physrevc.94.055802}, abstractNote={After identifying the nuclei in the regions near A =80 and A = 160 for which beta-decay rates have the greatest effect on weak and main r-process abundance patterns, we apply the finite-amplitude method (FAM) with Skyrme energy-density functionals (EDFs) to calculate beta-decay half-lives of those nuclei in the quasiparticle random-phase approximation (QRPA). We use the equal filling approximation to extend our implementation of the charge-changing FAM, which incorporates pairing correlations and allows axially symmetric deformation, to odd-A and odd-odd nuclei. Within this framework we find differences of up to a factor of seven between our calculated beta-decay half-lives and those of previous efforts. Repeated calculations with nuclei near A = 160 and multiple EDFs show a spread of two to four in beta-decay half-lives, with differences in calculated Q values playing an important role. We investigate the implications of these results for r-process simulations.}, number={5}, journal={PHYSICAL REVIEW C}, author={Shafer, T. and Engel, J. and Frohlich, C. and McLaughlin, G. C. and Mumpower, M. and Surman, R.}, year={2016}, month={Nov} }
 @inproceedings{fröhlich_hatcher_2015, title={Influence of nuclear reaction rates on the nucleosynthesis in neutrino-driven winds}, volume={93}, DOI={10.1051/epjconf/20159303008}, abstractNote={We study the sensitivity of the νp-process abundance pattern to (n,p), (p,γ), and (n,γ) rates for nuclei between Ni and Sn. We illustrate our findings for two different initial electron fractions and a representative trajectory. We discuss how these rates influence the abundance pattern and the nuclear flow. Core-collapse supernovae are important contributors to the chemical enrichment of galaxies. They synthesize heavy elements and eject these newly synthesized elements (iron and heavier elements) into the interstellar medium to- gether with elements produced during the star's lifetime. After the explosion, the nascent, hot neutron star cools by emitting neutrinos. These neutrinos interact with the stellar matter and deposit energy, resulting in a supersonic outflow, the neutrino-driven wind. The conditions in the winds are not suitable for the synthesis of the heaviest ele- ments by the r-process. However, lighter heavy elements, such as Sr, Y, Zr, can be formed. Recent hydrodynamic models suggest that very outward in a neutrino wind, the large proton density allows for a small number of neutrons to be produced by νe cap- tures on protons. This permits neutron-induced reactions - such as (n,γ) and (n,p) - to compete with proton cap- tures, electron captures, and β + -decays. Especially (n,p) reactions on proton-rich nuclei have cross sections 10 − 12 orders of magnitude larger than proton captures. There- fore, already a tiny neutron abundance can cause neutron- induced reaction flows competing with proton captures. The (n,p) reactions in the νp-process overcome the wait- ing points in the rp-process which are characterized by slow proton capture rates and long β-decay (electron cap- ture) lifetimes. Depending on the neutron density ρn, the (n,p) reactions regulate the flow from one isotonic chain to the next higher as they are faster than the β + -decays or electron captures. The path of the νp-process lies initially close to the N = Z line and moves towards stability at higher masses.}, booktitle={European Physical Journal Web of Conferences}, author={Fröhlich, Carla and Hatcher, Daniel}, year={2015}, month={May} }
 @inproceedings{hatcher_frohlich_perdikakis_2015, title={Nuclear reaction rates and their influence on nucleosynthesis in the neutrino-p-process}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Hatcher, Daniel and Frohlich, Carla and Perdikakis, Georgios}, year={2015}, month={Oct} }
 @article{perego_hempel_froehlich_ebinger_eichler_casanova_liebendoerfer_thielemann_2015, title={PUSHING CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY. I. THE MODEL AND THE CASE OF SN 1987A}, volume={806}, ISSN={["1538-4357"]}, url={http://dx.doi.org/10.1088/0004-637x/806/2/275}, DOI={10.1088/0004-637x/806/2/275}, abstractNote={We report on a method, PUSH, for artificially triggering core-collapse supernova explosions of massive stars in spherical symmetry. We explore basic explosion properties and calibrate PUSH to reproduce SN 1987A observables. Our simulations are based on the GR hydrodynamics code AGILE combined with the neutrino transport scheme isotropic diffusion source approximation for electron neutrinos and advanced spectral leakage for the heavy flavor neutrinos. To trigger explosions in the otherwise non-exploding simulations, the PUSH method increases the energy deposition in the gain region proportionally to the heavy flavor neutrino fluxes. We explore the progenitor range 18–21 M ⊙ ?> . Our studies reveal a distinction between high compactness (HC; compactness parameter &xgr; 1.75 > 0.45 ?> ) and low compactness (LC; &xgr; 1.75 < 0.45 ?> ) progenitor models, where LC models tend to explode earlier, with a lower explosion energy, and with a lower remnant mass. HC models are needed to obtain explosion energies around 1 Bethe, as observed for SN 1987A. However, all the models with sufficiently high explosion energy overproduce 56Ni and fallback is needed to reproduce the observed nucleosynthesis yields. 57–58Ni yields depend sensitively on the electron fraction and on the location of the mass cut with respect to the shell structure of the progenitor. We identify a progenitor and a suitable set of parameters that fit the explosion properties of SN 1987A assuming 0.1 M ⊙ ?> of fallback. We predict a neutron star with a gravitational mass of 1.50 M ⊙ ?> . We find correlations between explosion properties and the compactness of the progenitor model in the explored mass range. However, a more complete analysis will require exploring of a larger set of progenitors.}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Perego, A. and Hempel, M. and Froehlich, C. and Ebinger, K. and Eichler, M. and Casanova, J. and Liebendoerfer, M. and Thielemann, F. -K.}, year={2015}, month={Jun} }
 @inproceedings{johnson_reynolds_frohlich_blondin_2014, title={3D Simulations of Supernova Remnants from Type Ia Supernova Models}, booktitle={American Astronomical Society Meeting Abstracts #223}, author={Johnson, Heather and Reynolds, S. P. and Frohlich, C. and Blondin, J. M.}, year={2014}, month={Jan} }
 @inproceedings{casanova_frohlich_perego_hempel_2014, title={Core Collapse Supernova Models For Nucleosynthesis}, booktitle={American Astronomical Society Meeting Abstracts #223}, author={Casanova, Jordi and Frohlich, C. and Perego, A. and Hempel, M.}, year={2014}, month={Jan} }
 @inproceedings{frohlich_2014, title={Core-collapse supernovae and nucleosynthesis}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Frohlich, Carla}, year={2014}, month={Sep} }
 @article{froehlich_casanova_hempel_liebendoerfer_melton_perego_2014, title={Neutrinos and nucleosynthesis in core-collapse supernovae}, volume={1604}, ISSN={["0094-243X"]}, DOI={10.1063/1.4883428}, abstractNote={Massive stars (M > 8-10 M⊙) undergo core collapse at the end of their life and explode as supernova with ∼ 1051 erg of kinetic energy. While the detailed supernova explosion mechanism is still under investigation, reliable nucleosynthesis calculations based on successful explosions are needed to explain the observed abundances in metal-poor stars and to predict supernova yields for galactic chemical evolution studies. To predict nucleosynthesis yields for a large number of progenitor stars, computationally efficient explosion models are required. We model the core collapse, bounce and subsequent explosion of massive stars assuming spherical symmetry and using detailed microphysics and neutrino physics combined with a novel method to artificially trigger the explosion (PUSH). We discuss the role of neutrinos, the conditions in the ejecta, and the resulting nucleosynthesis.}, journal={WORKSHOP ON DARK MATTER, NEUTRINO PHYSICS AND ASTROPHYSICS CETUP 2013: VIITH INTERNATIONAL CONFERENCE ON INTERCONNECTIONS BETWEEN PARTICLE PHYSICS AND COSMOLOGY PPC 2013}, author={Froehlich, C. and Casanova, J. and Hempel, M. and Liebendoerfer, M. and Melton, C. A. and Perego, A.}, year={2014}, pages={178–184} }
 @inbook{heger_fröhlich_truran_2014, title={Origin of the Elements}, volume={2}, booktitle={Planets, Asteriods, Comets and The Solar System, Volume 2 of Treatise on Geochemistry (Second Edition).  Edited by Andrew M. Davis.  Elsevier, 2014., p.1-14}, author={Heger, A. and Fröhlich, C. and Truran, J. W.}, editor={Davis, Andrew M.Editor}, year={2014}, pages={1–14} }
 @inproceedings{ebinger_perego_hempel_frohlich_eichler_casanova_liebendörfer_thielemann_2014, title={Parametrized Spherically Symmetric Core Collapse Supernova Simulations: Push}, booktitle={XIII Nuclei in the Cosmos (NIC XIII)}, author={Ebinger, K. and Perego, A. and Hempel, M. and Frohlich, C. and Eichler, M. and Casanova, J. and Liebendörfer, M. and Thielemann, F. K.}, year={2014} }
 @article{froehlich_2014, title={Supernovae, neutrinos, and nucleosynthesis}, volume={41}, ISSN={["1361-6471"]}, url={http://dx.doi.org/10.1088/0954-3899/41/4/044003}, DOI={10.1088/0954-3899/41/4/044003}, abstractNote={Core-collapse supernovae are the violent explosions at the end of the life of massive stars (? 8 ? 10?M?). In these explosions a wide range of elements are synthesized and ejected: low-mass elements (O and Mg) from the hydrostatic evolution, intermediate-mass elements and Fe-group elements from explosive nucleosynthesis, and elements heavier than iron from the ?p-process and potentially an r-process. However, supernova nucleosynthesis predictions are hampered by the not yet fully understood supernova explosion mechanism. In addition, recent progress in observational astronomy paints a fascinating picture for the origin of heavy elements, which is more complicated than the traditional s-, r-, and ?-processes. In this paper, we summarize the status of core-collapse supernova nucleosynthesis.}, number={4}, journal={JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS}, author={Froehlich, Carla}, year={2014}, month={Apr} }
 @inproceedings{seadrow_frohlich_duan_friedland_mclaughlin_keohane_2014, title={The Effects of Collective Neutrino Oscillations on Supernova Nucleosynthesis}, booktitle={American Astronomical Society Meeting Abstracts #223}, author={Seadrow, Shaquann and Frohlich, C. and Duan, H. and Friedland, A. and McLaughlin, G. and Keohane, J. W.}, year={2014}, month={Jan} }
 @misc{rauscher_dauphas_dillmann_froehlich_fueloep_gyuerky_2013, title={Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data}, volume={76}, ISSN={["1361-6633"]}, url={http://dx.doi.org/10.1088/0034-4885/76/6/066201}, DOI={10.1088/0034-4885/76/6/066201}, abstractNote={A small number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in the s- and r-processes. Their origin is not well understood. Massive stars can produce p-nuclei through photodisintegration of pre-existing intermediate and heavy nuclei. This so-called γ-process requires high stellar plasma temperatures and occurs mainly in explosive O/Ne burning during a core-collapse supernova. Although the γ-process in massive stars has been successful in producing a large range of p-nuclei, significant deficiencies remain. An increasing number of processes and sites has been studied in recent years in search of viable alternatives replacing or supplementing the massive star models. A large number of unstable nuclei, however, with only theoretically predicted reaction rates are included in the reaction network and thus the nuclear input may also bear considerable uncertainties. The current status of astrophysical models, nuclear input and observational constraints is reviewed. After an overview of currently discussed models, the focus is on the possibility to better constrain those models through different means. Meteoritic data not only provide the actual isotopic abundances of the p-nuclei but can also put constraints on the possible contribution of proton-rich nucleosynthesis. The main part of the review focuses on the nuclear uncertainties involved in the determination of the astrophysical reaction rates required for the extended reaction networks used in nucleosynthesis studies. Experimental approaches are discussed together with their necessary connection to theory, which is especially pronounced for reactions with intermediate and heavy nuclei in explosive nuclear burning, even close to stability.}, number={6}, journal={REPORTS ON PROGRESS IN PHYSICS}, author={Rauscher, T. and Dauphas, N. and Dillmann, I. and Froehlich, C. and Fueloep, Zs and Gyuerky, Gy}, year={2013}, month={Jun} }
 @inproceedings{melton_frohlich_2013, title={Core-Collapse Supernova Nucleosynthesis of Promptly Ejected Material}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Melton, Cody and Frohlich, Carla}, year={2013}, month={Oct} }
 @inproceedings{perdikakis_almus_avetisyan_bataglia_bucher_casarella_fröhlich_lipschutz_long_lyons_et al._2013, title={Experimental Investigation of (p,n) reactions relevant to the astrophysical νp process}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Perdikakis, G. and Almus, R. M. and Avetisyan, R. and Bataglia, A. A. and Bucher, B. M. and Casarella, C. R. and Fröhlich, C. and Lipschutz, S. and Long, A. M. and Lyons, S. and et al.}, year={2013}, month={Oct} }
 @article{simon_spyrou_rauscher_froehlich_quinn_battaglia_best_bucher_couder_deyoung_et al._2013, title={Systematic study of (p, gamma) reactions on Ni isotopes}, volume={87}, ISSN={["1089-490X"]}, url={http://dx.doi.org/10.1103/physrevc.87.055802}, DOI={10.1103/physrevc.87.055802}, abstractNote={A systematic study of the radiative proton capture reaction for all stable nickel isotopes is presented. The results were obtained using 2.0–6.0 MeV protons from the 11-MV tandem Van de Graaff accelerator at the University of Notre Dame. The γ rays were detected by the NSCL-SuN detector utilizing the γ -summing technique. The results are compared to a compilation of earlier measurements and discrepancies between the previous data are resolved. The experimental results are also compared to the theoretical predictions obtained using the NON-SMOKER and SMARAGD codes. Based on these comparisons an improved set of astrophysical reaction rates is proposed for the (p, γ) reactions on the stable nickel isotopes as well as for the 56 Ni(p, γ) 57 Cu reaction.}, number={5}, journal={PHYSICAL REVIEW C}, author={Simon, A. and Spyrou, A. and Rauscher, T. and Froehlich, C. and Quinn, S. J. and Battaglia, A. and Best, A. and Bucher, B. and Couder, M. and DeYoung, P. A. and et al.}, year={2013}, month={May} }
 @inproceedings{casanova_frohlich_perego_hempel_liebendoerfer_2013, title={Towards Core Collapse Supernova Models for Nucleosynthesis}, booktitle={American Astronomical Society Meeting Abstracts #221}, author={Casanova, Jordi and Frohlich, C. and Perego, A. and Hempel, M. and Liebendoerfer, M.}, year={2013}, month={Jan} }
 @article{rauscher_kiss_szuecs_fueloep_froehlich_gyuerky_halasz_kertesz_somorjai_2012, title={Astrophysical analysis of the measurement of (alpha,gamma) and (alpha,n) cross sections of Tm-169}, volume={86}, ISSN={["1089-490X"]}, url={http://dx.doi.org/10.1103/physrevc.86.015804}, DOI={10.1103/physrevc.86.015804}, abstractNote={energy range 12.6 ≤ E� ≤ 17.5 MeV and 11.5 ≤ E� ≤ 17.5 MeV, respectively, using the recently introduced method of combining activation with X-ray counting. Improved shielding allowed to measure the (�,) to lower energy than previously possible. The combination of (�,) and (�,n) data made it possible to study the energy dependence of thewidth. While absolute value and energy dependence are perfectly reproduced by theory at the energies above 14 MeV, the observed change in energy dependence at energies below 14 MeV requires a modification of the predicted � width. Using an effective, energy-dependent, local optical �+nucleus potential it is possible to reproduce the data but the astrophysical rate is still not well constrained at -process temperatures. The additional uncertainty stemming from a possible modification of the compound formation cross section is discussed. Including the remaining uncertainties, the recommended range of astrophysical reaction rate values at 2 GK is higher than the previously used values by factors of 2 − 37.}, number={1}, journal={PHYSICAL REVIEW C}, author={Rauscher, T. and Kiss, G. G. and Szuecs, T. and Fueloep, Zs. and Froehlich, C. and Gyuerky, Gy. and Halasz, Z. and Kertesz, Zs. and Somorjai, E.}, year={2012}, month={Jul} }
 @article{arcones_froehlich_martinez-pinedo_2012, title={IMPACT OF SUPERNOVA DYNAMICS ON THE nu p-PROCESS}, volume={750}, ISSN={["0004-637X"]}, url={http://dx.doi.org/10.1088/0004-637x/750/1/18}, DOI={10.1088/0004-637x/750/1/18}, abstractNote={We study the impact of the late-time dynamical evolution of ejecta from core-collapse supernovae on νp-process nucleosynthesis. Our results are based on hydrodynamical simulations of neutrino-driven wind ejecta. Motivated by recent two-dimensional wind simulations, we vary the dynamical evolution during the νp-process and show that final abundances strongly depend on the temperature evolution. When the expansion is very fast, there is not enough time for antineutrino absorption on protons to produce enough neutrons to overcome the β+-decay waiting points and no heavy elements beyond A = 64 are produced. The wind termination shock or reverse shock dramatically reduces the expansion speed of the ejecta. This extends the period during which matter remains at relatively high temperatures and is exposed to high neutrino fluxes, thus allowing for further (p, γ) and (n, p) reactions to occur and to synthesize elements beyond iron. We find that the νp-process starts to efficiently produce heavy elements only when the temperature drops below ∼3 GK. At higher temperatures, due to the low alpha separation energy of 60Zn (Sα = 2.7 MeV) the reaction 59Cu(p, α)56Ni is faster than the reaction 59Cu(p, γ)60Zn. This results in the closed NiCu cycle that we identify and discuss here for the first time. We also investigate the late phase of the νp-process when the temperatures become too low to maintain proton captures. Depending on the late neutron density, the evolution to stability is dominated by β+ decays or by (n, γ) reactions. In the latter case, the matter flow can even reach the neutron-rich side of stability and the isotopic composition of a given element is then dominated by neutron-rich isotopes.}, number={1}, journal={ASTROPHYSICAL JOURNAL}, author={Arcones, A. and Froehlich, C. and Martinez-Pinedo, G.}, year={2012}, month={May} }
 @article{nucleosynthesis in core-collapse supernova explosions triggered by a quark-hadron phase transition_2012, url={http://dx.doi.org/10.1088/0004-637x/758/1/9}, DOI={10.1088/0004-637x/758/1/9}, abstractNote={We explore heavy-element nucleosynthesis in the explosion of massive stars that are triggered by a quark–hadron phase transition during the early post-bounce phase of core-collapse supernovae. The present study is based on general-relativistic radiation hydrodynamics simulations with three-flavor Boltzmann neutrino transport in spherical symmetry, which utilize a quark–hadron hybrid equation of state based on the MIT bag model for strange quark matter. The quark–hadron phase transition inside the stellar core forms a shock wave propagating toward the surface of the proto-neutron star. This shock wave results in an explosion and ejects neutron-rich matter from the outer accreted layers of the proto-neutron star. Later, during the cooling phase, the proto-neutron star develops a proton-rich neutrino-driven wind. We present a detailed analysis of the nucleosynthesis outcome in both neutron-rich and proton-rich ejecta and compare our integrated nucleosynthesis with observations of the solar system and metal-poor stars. For our standard scenario, we find that a “weak” r-process occurs and elements up to the second peak (A ∼ 130) are successfully synthesized. Furthermore, uncertainties in the explosion dynamics could barely allow us to obtain the strong r-process which produces heavier isotopes, including the third peak (A ∼ 195) and actinide elements.}, year={2012}, month={Oct} }
 @inproceedings{rauscher_fröhlich_2012, title={Proton-rich nucleosynthesis and nuclear physics}, DOI={10.1063/1.4763376}, abstractNote={Although the detailed conditions for explosive nucleosynthesis are derived from astrophysical modeling, nuclear physics determines fundamental patterns in abundance yields, not only for equilibrium processes. Focussing on the νp- and the γ-process, general nucleosynthesis features within the range of astrophysical models, but (mostly) independent of details in the modelling, are presented. Remaining uncertainties due to uncertain Q-values and reaction rates are discussed.}, booktitle={American Institute of Physics Conference Series}, author={Rauscher, T. and Fröhlich, C.}, year={2012}, month={Nov} }
 @inproceedings{fröhlich_rauscher_2012, title={Reaction rate uncertainties and the ν p-process}, DOI={10.1063/1.4763400}, abstractNote={Current hydrodynamical simulations of core collapse supernovae find proton-rich early ejecta. At the same time, the models fail to eject neutron-rich matter, thus leaving the origin of the main r-process elements unsolved. However, the proton-rich neutrino-driven winds from supernovae have been identified as a possible production site for light n-capture elements beyond iron (such as Ge, Sr, Y, Zr) through the νp-process. The detailed nucleosynthesis patterns of the νp-process depend on the hydrodynamic conditions and the nuclear reaction rates of key reactions. We investigate the impact of reaction rate uncertainties on the νp-process nucleosynthesis.}, booktitle={American Institute of Physics Conference Series}, author={Fröhlich, C. and Rauscher, T.}, year={2012}, month={Nov} }
 @article{froehlich_2012, title={The nu p-process: critical nuclear physics and astrophysical implications}, volume={403}, ISSN={["1742-6596"]}, url={http://dx.doi.org/10.1088/1742-6596/403/1/012034}, DOI={10.1088/1742-6596/403/1/012034}, abstractNote={The neutrino-p-process is thought to occur in the innermost proton-rich layers ejected in core-collapse supernovae. The importance of the vp-process lies in the fact that it may contribute to the abundances of elements above Nickel and possibly the light p-nuclei. The reaction path of the vp-process lies in a region where nuclear masses are partly unknown and all involved reaction rates are based on theoretical predictions. Detailed studies of the vp-process nucleosynthesis and its uncertainty due to the nuclear physics are presented, with a focus on the reaction path at and above 56Ni. The vp-process path is found to be mainly determined by nuclear structure and thus is trajectory independent. Critical nuclear physics input are identified and the impact of uncertainties on the resulting nucleosynthesis is discussed.}, journal={HITES 2012: HORIZONS OF INNOVATIVE THEORIES, EXPERIMENTS, AND SUPERCOMPUTING IN NUCLEAR PHYSICS}, author={Froehlich, Carla}, year={2012} }
 @inproceedings{frohlich_2012, title={The synthesis of light n-capture elements at low metallicity}, booktitle={Nuclei in the Cosmos (NIC XII)}, author={Frohlich, C.}, year={2012} }
 @article{kiss_szuecs_gyuerky_fueloep_farkas_kertesz_somorjai_laubenstein_froehlich_rauscher_2011, title={Activation method combined with characteristic X-ray counting: A possibility to measure (alpha, gamma) cross sections on heavy p-nuclei}, volume={867}, ISSN={["1873-1554"]}, url={http://dx.doi.org/10.1016/j.nuclphysa.2011.07.003}, DOI={10.1016/j.nuclphysa.2011.07.003}, abstractNote={For an improved modeling of the astrophysical nucleosynthesis of p-nuclei, low energy cross section data of alpha-induced reactions on heavy isotopes are needed. Technical difficulties hamper the experimental determination of these cross sections, therefore the relevant experimental data are almost completely missing. Here we present a new method for the cross section measurements, the activation technique based on the detection of characteristic X-ray radiation. The feasibility of the method is illustrated through the measurement of the 169Tm(α,γ)173Lu and 169Tm(α,n)172Lu reaction cross sections. Despite the relatively long half-life of the reaction products (T1/2=500 and 6.7 days, respectively) it was possible to measure the cross section of the 169Tm(α,γ)173Lu reaction between Ec.m.=13.16 and 17.08 MeV. The 169Tm(α,n)172Lu reaction cross section was derived from close above the threshold up to Ec.m.=17.08 MeV. Details of the new method and the experimental results are presented.}, number={1}, journal={NUCLEAR PHYSICS A}, author={Kiss, G. G. and Szuecs, T. and Gyuerky, Gy. and Fueloep, Zs. and Farkas, J. and Kertesz, Zs. and Somorjai, E. and Laubenstein, M. and Froehlich, C. and Rauscher, T.}, year={2011}, month={Oct}, pages={52–65} }
 @article{kiss_rauscher_szuecs_kertesz_fueloep_gyuerky_froehlich_farkas_elekes_somorjai_2011, title={Determining reaction cross sections via characteristic X-ray detection: alpha-induced reactions on Tm-169 for the astrophysical gamma-process}, volume={695}, ISSN={["1873-2445"]}, url={http://dx.doi.org/10.1016/j.physletb.2010.11.052}, DOI={10.1016/j.physletb.2010.11.052}, abstractNote={The cross sections of the Tm169(α,γ)Lu173 and Tm169(α,n)Lu172 reactions have been measured first time using a new method, by detecting the characteristic X-ray radiation following the electron capture-decay of 172,173Lu. Despite the relatively long half-life of the reaction products (T1/2=500 and 6.7 days, respectively) it was possible to measure the cross section of the Tm169(α,γ)Lu173 reaction close to the Gamow window (T9=3.5 GK), between Ec.m.=13.16 and 17.08 MeV. The Tm169(α,n)Lu172 reaction cross section was measured from Ec.m.=11.21 MeV up to Ec.m.=17.08 MeV. The experimental results have been compared to theoretical predictions.}, number={5}, journal={PHYSICS LETTERS B}, author={Kiss, G. G. and Rauscher, T. and Szuecs, T. and Kertesz, Zs and Fueloep, Zs and Gyuerky, Gy and Froehlich, C. and Farkas, J. and Elekes, Z. and Somorjai, E.}, year={2011}, month={Jan}, pages={419–423} }
 @inproceedings{griffeth_reynolds_frohlich_blondin_2011, title={Hydrodynamic Modeling of Supernova Remnant G1.9+0.3}, booktitle={AAS/High Energy Astrophysics Division #12}, author={Griffeth, Alice and Reynolds, S. P. and Frohlich, C. and Blondin, J. M.}, year={2011}, month={Sep} }
 @article{what are the astrophysical sites for the r-process and the production of heavy elements?_2011, url={http://dx.doi.org/10.1016/j.ppnp.2011.01.032}, DOI={10.1016/j.ppnp.2011.01.032}, abstractNote={This article addresses three of the four nucleosynthesis processes involved in producing heavy nuclei beyond Fe (with a main focus on the r-process). Opposite to the fourth process (the s-process), which operates in stellar evolution during He- and C-burning, they are all related to explosive burning phases, (presumably) linked to core collapse supernova events of massive stars. The (classical) p-process is identified with explosive Ne/O-burning in outer zones of the progenitor star. It is initiated by the passage of the supernova shock wave and acts via photodisintegration reactions like a spallation process which produces neighboring (proton-rich) isotopes from pre-existing heavy nuclei. The reproduction of some of the so-called lighter p-isotopes with A<100 faces problems in this environment. The only recently discovered νp-process is related to the innermost ejecta, the neutrino wind expelled from the hot proto-neutron star after core collapse and the supernova explosion. This neutrino wind is proton-rich in its early phase, producing nuclei up to 64Ge. Reactions with neutrinos permit to overcome decay/reaction bottlenecks for the flow beyond 64Ge, thus producing light p-isotopes, which face problems in the classical p-process scenario. The understanding of the r-process, being identified for a long time with rapid neutron captures and passing through nuclei far from stability, is still experiencing major problems. These are on the one hand related to nuclear uncertainties far from stability (masses, half-lives, fission barriers), affecting the process speed and abundance peaks. On the other hand the site is still not definitely located, yet. (i) Later, possibly neutron-rich, high entropy phases of the neutrino wind (if they materialize!) could permit its operation. (ii) Other options include the ejection of very neutron-rich neutron star-like matter, occurring possibly in neutron star mergers or core collapse supernova events with jets, related to prior stellar evolution with high rotation rates and magnetic fields. Two different environments are required for a weak and a main/strong r-process, witnessed by observations of low metallicity stars and meteoritic inclusions, which could possibly be identified with the two options listed above, i.e. the weak r-process could be related to the neutrino wind when changing from p-rich to n-rich conditions.}, year={2011}, month={Apr} }
 @inproceedings{sobeck_frohlich_truran_kim_2010, title={Galactic Chemical Evolution of the Iron Peak Elements in the Lowest Metallicity Regimes}, DOI={10.1063/1.3518880}, abstractNote={We use the nucleosynthetic yields of Chieffi & Limongi (2004) in conjunction with a Salpeter initial mass function (IMF) to determine the evolution of iron peak element abundances (Z = 21–28) as a function of metallicity. Since we will focus on the extremely metal poor region below [Fe/H] = −1.5, we will consider input from core collapse supernovae (SNe) only, as chemical enrichment from Type Ia SNe is minimal at low metallicities (e. g. Kobayashi & Nomoto (2009) and references therein). For the Fe‐peak elements, we will evaluate the relative agreement between theoretical yield calculations and recently‐acquired observational data. We will determine the yield dependence on metallicity and compare our results to those of Kobayashi et al.. (2006). It is our eventual goal to employ alternate IMF’s in order to examine the resulting effects on the iron group abundance ratios.}, booktitle={American Institute of Physics Conference Series}, author={Sobeck, Jennifer and Frohlich, Carla and Truran, Jim and Kim, Yeunjin}, year={2010}, month={Nov} }
 @inproceedings{thielemann_dillmann_farouqi_fischer_fröhlich_kelic-heil_korneev_kratz_langanke_liebendörfer_et al._2010, title={The r-, p-, and νp-Process}, DOI={10.1088/1742-6596/202/1/012006}, abstractNote={The processes discussed in this review are three of the four nucleosynthesis processes involved in producing heavy nuclei beyond Fe (not counting the rp-process in X-ray bursts). Opposite to the fourth process (the s-process), which operates in stellar evolution during He- and C-burning, they are all related to explosive burning phases, (presumably) linked to core collapse supernova events of massive stars. The (classical) p-process is identified with explosive Ne/O-burning in outer zones of the progenitor star. It is intitiated by the passage of the supernova shock wave and acts via photodisintegration reactions like a spallation process which produces neighboring (proton-rich) isotopes from pre-existing heavy nuclei. The reproduction of some of the so-called lighter p-isotopes with A < 100 faces problems in this environment. The only recently discovered νp-process is related to the innermost ejecta, the neutrino wind expelled from the hot proto-neutron star after core collapse in the supernova explosion. This neutrino wind is proton-rich in its early phase and reactions with neutrinos permit to overcome decay/reaction bottlenecks for the flow beyond the Fe-group, thus permitting the production of those p-isotopes, which face problems in the classical p-process scenario. The understanding of the r-process, being identified for a long time with rapid neutron captures – and passing through nuclei far from stability – is still experiencing major problems. These are on the one hand related to nuclear uncertainties far from stability (masses and half-lives), affecting the process speed and abundance peaks, on the other hand the site is still not definitely located, yet. Later neutron-rich, high entropy phases of the neutrino wind could permit its operation, other options include the ejection of very neutron-rich neutron star matter. Two different environments are required for a weak and a main/strong r-process, witnessed by observations of low metallicity stars.}, booktitle={Journal of Physics Conference Series}, author={Thielemann, F. -K. and Dillmann, I. and Farouqi, K. and Fischer, T. and Fröhlich, C. and Kelic-Heil, A. and Korneev, I. and Kratz, K. -L. and Langanke, K. and Liebendörfer, M. and et al.}, year={2010}, month={Jan} }
 @article{erratum: “iron-60 evidence for early injection and efficient mixing of stellar debris in the protosolar nebula” (2008, apj, 686, 560)_2009, url={http://dx.doi.org/10.1088/0004-637x/691/2/1943}, DOI={10.1088/0004-637x/691/2/1943}, abstractNote={Due to an error in processing the data, some values of 60 Ni corrected for instrumental mass fractionation using 61Ni/58Ni ratios are incorrect. The corrected Table 2 is appended below. Nevertheless, the shifts that result from this correction are all within error bars and do not affect the conclusions of the paper. The figures are also unaffected.}, year={2009}, month={Feb} }
 @inproceedings{frohlich_tang_truran_2009, title={The Impact of Reaction Rate Uncertainties (and other nuclear physics inputs) on Nucleosynthesis in the Neutrino-p Process}, booktitle={APS Meeting Abstracts}, author={Frohlich, Carla and Tang, X. and Truran, J. W.}, year={2009}, month={Oct} }
 @article{dauphas_cook_sacarabany_fröhlich_davis_wadhwa_pourmand_rauscher_gallino_2008, title={<SUP>60</SUP>Fe in the cosmic blender}, journal={Geochimica et Cosmochimica Acta Supplement}, author={Dauphas, N. and Cook, D. L. and Sacarabany, A. and Fröhlich, C. and Davis, A. M. and Wadhwa, M. and Pourmand, A. and Rauscher, T. and Gallino, R.}, year={2008}, month={Jul} }
 @inproceedings{fröhlich_fischer_liebendörfer_thielemann_truran_2008, title={Detailed Nucleosynthesis Yields from the Explosion of Massive Stars}, DOI={10.1017/S1743921308020759}, abstractNote={Abstract}, booktitle={Massive Stars as Cosmic Engines}, author={Fröhlich, Carla and Fischer, T. and Liebendörfer, M. and Thielemann, F. -K. and Truran, J. W.}, year={2008}, month={Jun} }
 @article{iron 60 evidence for early injection and efficient mixing of stellar debris in the protosolar nebula_2008, url={http://dx.doi.org/10.1086/589959}, DOI={10.1086/589959}, abstractNote={Among extinct radioactivities present in meteorites,60Fe (t1/2 = 1.49 Myr) plays a key role as a high-resolution chronometer, a heat source in planetesimals, and a fingerprint of the astrophysical setting of solar system formation. A critical issue with 60Fe is that it could have been heterogeneously distributed in the protoplanetary disk, calling into question the efficiency of mixing in the solar nebula or the timing of 60Fe injection relative to planetesimal formation. If this were the case, one would expect meteorites that did not incorporate 60Fe (either because of late injection or incomplete mixing) to show 60Ni deficits (from lack of 60Fe decay) and collateral effects on other neutron-rich isotopes of Fe and Ni (coproduced with 60Fe in core-collapse supernovae and AGB stars). Here, we show that measured iron meteorites and chondrites have Fe and Ni isotopic compositions identical to Earth. This demonstrates that 60Fe must have been injected into the protosolar nebula and mixed to less than 10% heterogeneity before formation of planetary bodies.}, year={2008}, month={Oct} }
 @inproceedings{dauphas_cook_sacarabany_frohlich_davis_wadhwa_pourmand_rauscher_gallino_2008, title={Iron-60 Injection in the Protosolar Nebula: How Early and How Well Mixed?}, booktitle={Lunar and Planetary Science Conference}, author={Dauphas, N. and Cook, D. L. and Sacarabany, A. and Frohlich, C. and Davis, A. M. and Wadhwa, M. and Pourmand, A. and Rauscher, T. and Gallino, R.}, year={2008}, month={Mar} }
 @article{mass measurements in the vicinity of ther p-process and theν p-process paths with the penning trap facilities jyfltrap and shiptrap_2008, url={http://dx.doi.org/10.1103/physrevc.78.054310}, DOI={10.1103/physrevc.78.054310}, abstractNote={The masses of very neutron-deficient nuclides close to the astrophysical r p- and {nu} p-process paths have been determined with the Penning trap facilities JYFLTRAP at JYFL/Jyvaeskylae and SHIPTRAP at GSI/Darmstadt. Isotopes from yttrium (Z=39) to palladium (Z=46) have been produced in heavy-ion fusion-evaporation reactions. In total, 21 nuclides were studied, and almost half of the mass values were experimentally determined for the first time: {sup 88}Tc, {sup 90-92}Ru, {sup 92-94}Rh, and {sup 94,95}Pd. For the {sup 95}Pd{sup m}, (21/2{sup +}) high-spin state, a first direct mass determination was performed. Relative mass uncertainties of typically {delta}m/m=5x10{sup -8} were obtained. The impact of the new mass values has been studied in {nu} p-process nucleosynthesis calculations. The resulting reaction flow and the final abundances are compared with those obtained with the data of the Atomic Mass Evaluation 2003.}, year={2008}, month={Nov} }
 @article{nuclear physics in core-collapse supernovae_2008, url={http://dx.doi.org/10.1016/j.newar.2008.05.006}, DOI={10.1016/j.newar.2008.05.006}, abstractNote={Core-collapse and the launch of a supernova explosion form a very short episode of few seconds in the evolution of a massive star, during which an enormous gravitational energy of several times 1053 erg is transformed into observable neutrino-, kinetic-, and electromagnetic radiation energy. We emphasize the wide range of matter conditions that prevail in a supernova event and sort the conditions into distinct regimes in the density and entropy phase diagram to briefly discuss their different impact on the neutrino signal, gravitational wave emission, and ejecta.}, year={2008}, month={Oct} }
 @article{nuclear physics with spherically symmetric supernova models_2008, url={http://dx.doi.org/10.1088/0954-3899/35/1/014056}, DOI={10.1088/0954-3899/35/1/014056}, abstractNote={In recent years, Boltzmann neutrino transport led to a new and reliable generation of spherically symmetric models of stellar core-collapse and postbounce evolution. After the failure to prove the principles of the supernova explosion mechanism, these sophisticated models continue to illuminate the close interaction between high-density matter under extreme conditions and the transport of leptons and energy, in general, relativistically curved spacetime. We emphasize that very different input physics is likely to be relevant for the different evolutionary phases, e.g. nuclear structure for weak rates in collapse, the equation of state of bulk nuclear matter during bounce, multidimensional plasma dynamics in the postbounce evolution and neutrino cross sections in the explosive nucleosynthesis. We illustrate the complexity of the dynamics using preliminary 3D MHD high-resolution simulations based on parametrized deleptonization. With established spherically symmetric models we show that typical features of the different phases are reflected in the predicted neutrino signal and that a consistent neutrino flux leads to electron fractions larger than 0.5 in neutrino-driven supernova ejecta.}, year={2008}, month={Jan} }
 @inproceedings{frohlich_fischer_liebendoerfer_thielemann_truran_2008, title={Nucleosynthesis Yields from the Explosion of Massive Stars}, booktitle={APS April Meeting Abstracts}, author={Frohlich, Carla and Fischer, T. and Liebendoerfer, M. and Thielemann, F. -K. and Truran, J. W.}, year={2008}, month={Apr} }
 @inproceedings{fröhlich_hirschi_liebendörfer_thielemann_martínez pinedo_bravo_2008, title={Supernovae in Galactic evolution: direct and indirect metallicity effects}, booktitle={The Metal-Rich Universe}, author={Fröhlich, C. and Hirschi, R. and Liebendörfer, M. and Thielemann, F. -K. and Martínez Pinedo, G. and Bravo, E.}, year={2008} }
 @inproceedings{martínez-pinedo_kelić_langanke_schmidt_mocelj_fröhlich_thielemann_panov_rauscher_liebendörfer_et al._2007, title={Astrophysical Challenges to Ria:. Explosive Nucleosynthesis in Supernovae}, DOI={10.1142/9789812708250_0017}, booktitle={Opportunities with Exotic Beams}, author={Martínez-Pinedo, G. and Kelić, A. and Langanke, K. and Schmidt, K. -H. and Mocelj, D. and Fröhlich, C. and Thielemann, F. -K. and Panov, I. and Rauscher, T. and Liebendörfer, M. and et al.}, year={2007}, month={Mar} }
 @article{production of intermediate-mass and heavy nuclei_2007, url={http://dx.doi.org/10.1016/j.ppnp.2006.12.019}, DOI={10.1016/j.ppnp.2006.12.019}, abstractNote={Nucleosynthesis is the science related to all astrophysical processes which are responsible for the abundances of the elements and their isotopes in the universe. The astrophysical sites are the big bang and stellar objects. The working of nucleosynthesis processes is presented in a survey of events which act as abundance sources. For intermediate-mass and heavy elements, these are stellar evolution, type Ia and core collapse supernovae as well as hypernovae. We discuss successes and failures of existing processes and possible solutions via new (hitherto unknown) processes. Finally an analysis of their role is given in the puzzle to explain the evolution of the elemental and isotopic compositions found in galaxies, and especially the mixture found in the solar system. Different timescales due to the progenitor mass dependence of the endpoints of stellar evolution (type II supernova explosions — SNe II vs. planetary nebulae) or single vs. binary stellar systems (the latter being responsible for novae, type Ia supernovae — SNe Ia, or X-ray bursts) are the keys to understand galactic evolution. At very early times, the role of explosion energies of events, polluting pristine matter with a composition originating only from the big bang, might also play a role. We also speculate on the role of very massive stars not undergoing SN II explosions but rather causing “hypernovae” after the formation of a central black hole via core collapse.}, year={2007}, month={Jul} }
 @inproceedings{frohlich_2007, title={The Neutrino p-Process}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Frohlich, Carla}, year={2007}, month={Oct} }
 @inproceedings{fröhlich_liebendörfer_martínez-pinedo_thielemann_bravo_zinner_hix_langanke_mezzacappa_nomoto_2006, title={Composition of the Innermost Core Collapse Supernova Ejecta and the νp-Process}, DOI={10.1063/1.2234421}, abstractNote={With presently known input physics and computer simulations in 1D, a self‐consistent treatment of core collapse supernovae does not lead to explosions, while 2D models show some promise. Thus, there are strong indications that the delayed neutrino mechanism works combined with a multi‐D convection treatment for unstable layers. On the other hand there is a need to provide correct nucleosynthesis abundances for the progressing field of galactic evolution and observations of low metallicity stars. The innermost ejecta is directly affected by the explosion mechanism, i.e. most strongly the yields of Fe‐group nuclei for which an induced piston or thermal bomb treatment will not provide the correct yields because the effect of neutrino interactions is not included. We apply parameterized variations to the neutrino scattering cross sections and alternatively, parameterized variations to the neutrino absorption cross sections on nucleons in the “gain region”. We find that both measures lead to similar results, causing explosions and a Ye larger than 0.5 in the innermost ejected layers, due to the combined effect of a short weak interaction time scale and a negligible electron degeneracy, unveiling the proton‐neutron mass difference. The proton‐rich environment results in enhanced abundances of 45Sc, 49Ti, and 64Zn as requested by chemical evolution studies and observations of low metallicity stars. Moreover, antineutrino capture on the free protons allows for an appreciable production of nuclei in the mass range up to A = 80 by the νp‐process.}, booktitle={Origin of Matter and Evolution of Galaxies}, author={Fröhlich, C. and Liebendörfer, M. and Martínez-Pinedo, G. and Thielemann, F. -K. and Bravo, E. and Zinner, N. T. and Hix, W. R. and Langanke, K. and Mezzacappa, A. and Nomoto, K.}, year={2006}, month={Jul} }
 @article{composition of the innermost core‐collapse supernova ejecta_2006, url={http://dx.doi.org/10.1086/498224}, DOI={10.1086/498224}, abstractNote={With currently known input physics and computer simulations in one dimension, a self-consistent treatment of core-collapse supernovae does not yet lead to successful explosions, while two-dimensional models show some promise. Thus, there are strong indications that the delayed neutrino mechanism works combined with a multidimensional convection treatment for unstable layers (possibly with the aid of rotation, magnetic fields and/or still existent uncertainties in neutrino opacities). On the other hand, there is a need to provide correct nucleosynthesis abundances for the progressing field of galactic evolution and observations of low-metallicity stars. The innermost ejecta is directly affected by the explosion mechanism, i.e., most strongly, the yields of Fe group nuclei for which an induced piston or thermal bomb treatment will not provide the correct yields because the effect of neutrino interactions is not included. We apply parameterized variations to the neutrino-scattering cross sections in order to mimic in one dimension the possible increase of neutrino luminosities caused by uncertainties in proto-neutron star convection. Alternatively, parameterized variations are applied to the neutrino absorption cross sections on nucleons in the "gain region" to mimic the increase in neutrino energy deposition enabled by convective turnover. We find that both measures lead to similar results, causing explosions and a Ye > 0.5 in the innermost ejected layers, due to the combined effect of a short weak-interaction timescale and a negligible electron degeneracy, unveiling the proton-neutron mass difference. We include all weak interactions (electron and positron capture, β-decay, neutrino and antineutrino capture on nuclei, and neutrino and antineutrino capture on nucleons) and present first nucleosynthesis results for these innermost ejected layers to discuss how they improve predictions for Fe group nuclei. The proton-rich environment results in enhanced abundances of 45Sc, 49Ti, and 64Zn as required by chemical evolution studies and observations of low-metallicity stars, as well as appreciable production of nuclei in the mass range up to A = 80.}, year={2006}, month={Jan} }
 @article{neutrino-induced nucleosynthesis ofa>64nuclei: theνpprocess_2006, url={http://dx.doi.org/10.1103/physrevlett.96.142502}, DOI={10.1103/physrevlett.96.142502}, abstractNote={We present a new nucleosynthesis process that we denote as the nu p process, which occurs in supernovae (and possibly gamma-ray bursts) when strong neutrino fluxes create proton-rich ejecta. In this process, antineutrino absorptions in the proton-rich environment produce neutrons that are immediately captured by neutron-deficient nuclei. This allows for the nucleosynthesis of nuclei with mass numbers A>64, , making this process a possible candidate to explain the origin of the solar abundances of (92,94)Mo and (96,98)Ru. This process also offers a natural explanation for the large abundance of Sr seen in a hyper-metal-poor star.}, year={2006}, month={Apr} }
 @unpublished{martínez-pinedo_kelic_langanke_schmidt_mocelj_fröhlich_thielemann_panov_rauscher_liebendörfer_et al._2006, title={Nucleosynthesis in neutrino heated matter: The vp-process and the r-process}, journal={arXiv e-prints}, author={Martínez-Pinedo, G. and Kelic, A. and Langanke, K. and Schmidt, K. -H. and Mocelj, D. and Fröhlich, C. and Thielemann, F. -K. and Panov, I. and Rauscher, T. and Liebendörfer, M. and et al.}, year={2006}, month={Aug} }
 @article{nucleosynthesis in neutrino-driven supernovae_2006, url={http://dx.doi.org/10.1016/j.newar.2006.06.003}, DOI={10.1016/j.newar.2006.06.003}, abstractNote={Core collapse supernovae are the leading actor in the story of the cosmic origin of the chemical elements. Existing models, which generally assume spherical symmetry and parameterize the explosion, have been able to broadly replicate the observed elemental pattern. However, inclusion of neutrino interactions produces noticeable improvement in the composition of the ejecta when compared to observations. Neutrino interactions may also provide a supernova source for light p-process nuclei.}, year={2006}, month={Oct} }
 @inproceedings{fröhlich_liebendörfer_thielemann_martinez pinedo_langanke_zinner_hix_bravo_2006, title={The Role of Neutrinos in Explosive Nucleosynthesis}, booktitle={International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos}, author={Fröhlich, Carla and Liebendörfer, M. and Thielemann, F. -K. and Martinez Pinedo, G. and Langanke, K. and Zinner, N. T. and Hix, W. R. and Bravo, E.}, year={2006} }
 @inproceedings{martinez-pinedo_kelic_langanke_schmidt_mocelj_fröhlich_thielemann_panov_rauscher_liebendörfer_et al._2006, title={Weak interaction rates}, booktitle={International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos}, author={Martinez-Pinedo, Gabriel and Kelic, A. and Langanke, K. and Schmidt, K. -H. and Mocelj, D. and Fröhlich, C. and Thielemann, F. -K. and Panov, I. and Rauscher, T. and Liebendörfer, M. and et al.}, year={2006} }
 @article{hix_fröhlich_martìnex-pinedo_liebendörfer_thielemann_2005, title={Influence of the Explosion Mechanism on the Ejecta of Core Collapse Supernovae}, journal={Meteoritics and Planetary Science Supplement}, author={Hix, W. R. and Fröhlich, C. and Martìnex-Pinedo, G. and Liebendörfer, M. and Thielemann, F. -K.}, year={2005}, month={Sep} }
 @article{nuclear physics: a key ingredient in astrophysical modeling_2005, url={http://dx.doi.org/10.1016/j.nuclphysa.2005.02.111}, DOI={10.1016/j.nuclphysa.2005.02.111}, abstractNote={Nuclear physics is a basic ingredient in a large number of energetic astrophysical environments which are characterized by sufficient temperatures and densities to permit scattering events among particles, leading to nuclear reactions and possibly the production of unstable reaction poducts. Strong, electromagnetic and weak interactions (fusion, exchange reactions, photodisintegrations, beta-decays, electron [and positron] captures on nucleons and nuclei, neutrino scattering and captures [i.e. neutral and charged current reactions]) can produce nuclei far form stability and require extended knowledge of nuclear structure near and far from stability, including decay and fission properties. Last, but not least, the nucleon-nucleon interaction determines the nuclear equation of state at and beyond nuclear densities and is ultimately connected to the question under which conditions a phase transitions from hadrons to the quark-gluon plasma occurs. In this review we will survey how these aspects of nuclear physics enter the modeling of astrophysical objects.}, year={2005}, month={Apr} }
 @inproceedings{frohlich_thielemann_martinez-pinedo_liebendoerfer_2005, title={Nucleosynthesis in the Innermost Supernovae Ejecta}, booktitle={American Astronomical Society Meeting Abstracts #206}, author={Frohlich, C. and Thielemann, F. -K. and Martinez-Pinedo, G. and Liebendoerfer, M.}, year={2005}, month={May} }
 @inproceedings{hix_parete-koon_fröhlich_thielemann_martínez-pinedo_2005, title={The Challenges of Coupling Supernova Nucleosynthesis to the Central Engine}, DOI={10.1142/9789812703446_0019}, booktitle={Open Issues in Core Collapse Supernova Theory}, author={Hix, W. R. and Parete-Koon, S. and Fröhlich, C. and Thielemann, F. -K. and Martínez-Pinedo, G.}, year={2005}, month={Dec} }
 @article{the innermost ejecta of core collapse supernovae_2005, url={http://dx.doi.org/10.1016/j.nuclphysa.2005.05.009}, DOI={10.1016/j.nuclphysa.2005.05.009}, abstractNote={We ensure successful explosions (of otherwise non-explosive models) by enhancing the neutrino luminosity via reducing the neutrino scattering cross sections or by increasing the heating efficiency via enhancing the neutrino absorption cross sections in the heating region. Our investigations show that the resulting electron fraction Ye in the innermost ejecta is close to 0.5, in some areas even exceeding 0.5. We present the effects of the resulting values for Ye on the nucleosynthesis yields of the innermost zones of core collapse Supernovae.}, year={2005}, month={Jul} }
 @inproceedings{fröhlich_hauser_thielemann_liebendörfer_pinedo_2005, title={The Innermost Zones of Core Collapse Supernovae}, booktitle={1604-2004: Supernovae as Cosmological Lighthouses}, author={Fröhlich, C. and Hauser, P. and Thielemann, F. -K. and Liebendörfer, M. and Pinedo, G. M.}, year={2005}, month={Dec} }
 @inproceedings{fröhlich_thielemann_martínez pinedo_liebendörfer_2005, title={The influence of the explosion Mechanism on the Fe-group ejecta of core collapse supernovae}, DOI={10.1017/S1743921305005879}, abstractNote={Core collapse supernovae are responsible for at least half of the galactic inventory of Fe-group elements and probably for most of the Fe-group abundances seen in metal poor stars. Recent simulations show the emergence of a proton-rich ($Y_e>0.5$) region in the innermost ejected mass zones due to the neutrino interaction with matter. We explore the nucleosynthesis implications of these findings that result in enhanced abundances of 45Sc, 49Ti, and 64Zn, which is consistent with chemical evolution studies and observations of low metallicity stars.}, booktitle={From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution}, author={Fröhlich, Carla and Thielemann, F. -K. and Martínez Pinedo, G. and Liebendörfer, M.}, year={2005} }
 @article{resonance analysis ofsm147(n,α)cross sections: comparison to optical model calculations and indications of nonstatistical effects_2004, url={http://dx.doi.org/10.1103/physrevc.69.015803}, DOI={10.1103/physrevc.69.015803}, abstractNote={We have measured the Sm-147(n,alpha) cross section from 3 eV to 500 keV and performed an R-matrix analysis in the resolved region (En>700 eV) to extract α widths for 104 resonances. We computed strength functions from these resonance parameters and compared them to transmission coefficients calculated using optical model potentials similar to those employed as inputs to statistical model calculations. The statistical model often is used to predict cross sections and astrophysical reaction rates. Comparing resonance parameters rather than cross sections allows more direct tests of potentials used in the model and hence should offer greater insight into possible improvements. In particular, an improved α+nucleus potential is needed for applications in nuclear astrophysics. In addition to providing a more direct test of the α+nucleus potential, the α-width distributions show indications of nonstatistical effects.}, year={2004}, month={Jan} }
 @inproceedings{rauscher_fröhlich_guber_2003, title={Reaction Rates and Nuclear Properties Relevant for Nucleosynthesis in Massive Stars and Far from Stability}, DOI={10.1142/9789812795151_0043}, abstractNote={Explosive nuclear burning in astrophysical environments produces unstable nuclei which again can be targets for subsequent reactions. In addition, it involves a large number of stable nuclides which are not fully explored by experiments, yet. Thus, it is necessary to be able to predict reaction cross sections and thermonuclear rates with the aid of theoretical models. Such predictions are also of interest for investigations at radioactive ion beam facilities. An extended library of theoretical cross sections and reaction rates is presented. The problem of alpha+nucleus potentials is addressed and new parametrizations presented. The problem of properly predicting cross sections at low level densities is illustrated by the Ni-62(n,gamma) reaction.}, booktitle={Capture Gamma-Ray Spectroscopy and Related Topics}, author={Rauscher, T. and Fröhlich, C. and Guber, K. H.}, year={2003}, month={Jun} }
 @inproceedings{koehler_gledenov_rauscher_fröhlich_2003, title={Resonance analysis of ^147Sm(n,α ) cross sections: Comparison to statistical model calculations and possible indications of non-statistical effects}, booktitle={APS Division of Nuclear Physics Meeting Abstracts}, author={Koehler, P. E. and Gledenov, Yu. M. and Rauscher, T. and Fröhlich, C.}, year={2003}, month={Oct} }