@article{wright_kneller_2018, title={Feasibility of using neutrino intensity interferometry to measure protoneutron star radii}, volume={98}, ISSN={["2470-0029"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-85052648061&partnerID=MN8TOARS}, DOI={10.1103/PhysRevD.98.043016}, abstractNote={It has recently been demonstrated analytically that the two-point correlation function for pairs of neutrinos may contain information about the size of the protoneutron star formed in a Galactic core-collapse supernova. The information about the size of the source emerges via the neutrino equivalent of intensity interferometry originally used by Hanbury-Brown and Twiss with photons to measure the radii of stars. However the analytic demonstration of neutrino intensity interferometry with supernova neutrinos made a number of approximations: that the two neutrinos had equal energies, that the neutrinos were emitted at simultaneous times from two points and that they were detected simultaneously at two detection points that formed a plane with the emission points. These approximations need to be relaxed in order to better determine the feasibility of neutrino intensity interferometry for supernovae neutrinos in a more realistic scenario. In this paper we further investigate the feasibility of intensity interferometry for supernova neutrinos by relaxing all the approximations made in the earlier study. We find that, while relaxing any one assumption reduces the correlation signal, the relaxation of the assumption of equal times of detection is by far the largest detrimental factor. For neutrino energies of order ∼15  MeV and a supernova distance of L=10  kpc, we show that in order to observe the interference pattern in the two-point correlation function of the neutrino pairs, the timing resolution of a detector needs to be on the order of ≲10-21  s if the initial neutrino wave packet has a size of σx∼10-11  cm.}, number={4}, journal={PHYSICAL REVIEW D}, author={Wright, Warren P. and Kneller, James P.}, year={2018}, month={Aug} }
 @article{wright_kneller_2017, title={Neutrino Intensity Interferometry: Measuring Protoneutron Star Radii During Core-Collapse Supernovae}, volume={119}, ISSN={["1079-7114"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-85026815010&partnerID=MN8TOARS}, DOI={10.1103/physrevlett.119.051101}, abstractNote={Intensity interferometry is a technique that has been used to measure the size of sources ranging from the quark-gluon plasma formed in heavy ion collisions to the radii of stars. We investigate using the same technique to measure protoneutron star (PNS) radii with the neutrino signal received from a core-collapse supernovae. Using a full wave-packet analysis, including the neutrino mass for the first time, we derive criteria where the effect can be expected to provide the desired signal, and find that neutrinos from the next Galactic supernova should contain extractable PNS radius information.}, number={5}, journal={PHYSICAL REVIEW LETTERS}, author={Wright, Warren P. and Kneller, James P.}, year={2017}, month={Aug} }
 @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{wright_kneller_ohlmann_roepke_scholberg_seitenzahl_2017, title={Neutrinos from type Ia supernovae: The gravitationally confined detonation scenario}, volume={95}, ISSN={["2470-0029"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-85021867099&partnerID=MN8TOARS}, DOI={10.1103/physrevd.95.043006}, abstractNote={Despite their use as cosmological distance indicators and their importance in the chemical evolution of galaxies, the unequivocal identification of the progenitor systems and explosion mechanism of normal type Ia supernova (SN Ia) remains elusive. The leading hypothesis is that such a supernova is a thermonuclear explosion of a carbon-oxygen white dwarf, but the exact explosion mechanism is still a matter of debate. Observation of a galactic SN Ia would be of immense value in answering the many open questions related to these events. One potentially useful source of information about the explosion mechanism and progenitor is the neutrino signal. 
In this paper we compute the expected neutrino signal from a gravitationally confined detonation (GCD) explosion scenario for a SN~Ia and show how the flux at Earth contains features in time and energy unique to this scenario. We then calculate the expected event rates in the Super-K, Hyper-K, JUNO, DUNE, and IceCube detectors and find both Hyper-K and IceCube would see a few events for a GCD supernova at 1 kpc or closer, while Super-K, JUNO, and DUNE would see a events if the supernova were closer than ${\sim}0.3$ kpc. The distance and detector criteria needed to resolve the time and spectral features arising from the explosion mechanism, neutrino production, and neutrino oscillation processes are also discussed. 
The neutrino signal from the GCD is then compared with the signal from a deflagration-to-detonation transition (DDT) explosion model computed previously. We find the overall event rate is the most discriminating feature between the two scenarios followed by the event rate time structure. Using the event rate in the Hyper-K detector alone, the DDT can be distinguished from the GCD at 2$\sigma$ if the distance to the supernova is less than $2.3\;{\rm kpc}$ for a normal mass ordering and $3.6\;{\rm kpc}$ for an inverted ordering.}, number={4}, journal={PHYSICAL REVIEW D}, author={Wright, Warren P. and Kneller, James P. and Ohlmann, Sebastian T. and Roepke, Friedrich K. and Scholberg, Kate and Seitenzahl, Ivo R.}, year={2017}, month={Feb} }
 @article{wright_nagaraj_kneller_scholberg_seitenzahl_2016, title={Neutrinos from type Ia supernovae: The deflagration-to-detonation transition scenario}, volume={94}, ISSN={["2470-0029"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-84979671235&partnerID=MN8TOARS}, DOI={10.1103/physrevd.94.025026}, abstractNote={It has long been recognized that the neutrinos detected from the next core-collapse supernova in the Galaxy have the potential to reveal important information about the dynamics of the explosion and the nucleosynthesis conditions as well as allowing us to probe the properties of the neutrino itself. The neutrinos emitted from thermonuclear—type Ia—supernovae also possess the same potential, although these supernovae are dimmer neutrino sources. For the first time, we calculate the time, energy, line of sight, and neutrino-flavor-dependent features of the neutrino signal expected from a three-dimensional delayed-detonation explosion simulation, where a deflagration-to-detonation transition triggers the complete disruption of a near-Chandrasekhar mass carbon-oxygen white dwarf. We also calculate the neutrino flavor evolution along eight lines of sight through the simulation as a function of time and energy using an exact three-flavor transformation code. We identify a characteristic spectral peak at ˜10 MeV as a signature of electron captures on copper. This peak is a potentially distinguishing feature of explosion models since it reflects the nucleosynthesis conditions early in the explosion. We simulate the event rates in the Super-K, Hyper-K, JUNO, and DUNE neutrino detectors with the SNOwGLoBES event rate calculation software and also compute the IceCube signal. Hyper-K willmore » be able to detect neutrinos from our model out to a distance of ˜10 kpc. Here, at 1 kpc, JUNO, Super-K, and DUNE would register a few events while IceCube and Hyper-K would register several tens of events.« less}, number={2}, journal={PHYSICAL REVIEW D}, author={Wright, Warren P. and Nagaraj, Gautam and Kneller, James P. and Scholberg, Kate and Seitenzahl, Ivo R.}, year={2016}, month={Jul} }
 @inproceedings{wright_2016, title={Oscillation degeneracy in non-standard neutrino interactions}, volume={1743}, DOI={10.1063/1.4953291}, abstractNote={The standard theory describing neutrino oscillations only uses the interactions predicted by the Standard Model of particle physics. However, there is plenty of room for non-standard interactions (NSI) to exist. This is because extra interactions are allowed by experimental error bars and even expected at some level from effective theory arguments. This research is focused on examining the phenomenological consequences of the new physics of NSI at large atmospheric neutrino detectors like IceCube DeepCore. Of particular focus are the degeneracies between and within the standard neutrino oscillation parameters and the NSI parameters. These degeneracies will be explored both analytically and numerically, and strategies to lift them will also be discussed. This research is largely based on [1].}, booktitle={Cetup 2015 - workshop on dark matter, neutrino physics and astrophysics & ppc 2015 - ixth international conference on interconnections between particle physics and cosmology}, author={Wright, W.}, year={2016} }