@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} }
 @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} }
 @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} }
 @article{gilmer_kozyreva_hirschi_frohlich_yusof_2017, title={Pair-instability supernova simulations: Progenitor evolution, explosion, and light curves}, volume={846}, number={2}, journal={Astrophysical Journal}, author={Gilmer, M. S. and Kozyreva, A. and Hirschi, R. and Frohlich, C. and Yusof, N.}, year={2017} }