Bulletin of the American Physical Society
APS April Meeting 2021
Volume 66, Number 5
Saturday–Tuesday, April 17–20, 2021; Virtual; Time Zone: Central Daylight Time, USA
Session B10: SupernovaeLive
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Sponsoring Units: DAP Chair: Sherwood Richers, UCB |
Saturday, April 17, 2021 10:45AM - 10:57AM Live |
B10.00001: Mass ejection in failed supernovae: equation of state and neutrino loss dependence Mario Ivanov, Rodrigo Fernandez A failed core-collapse supernova from a non-rotating progenitor can eject mass due to a weakening of gravity associated to neutrino emission by the protoneutron star. This mass ejection mechanism yields observable transients and sets an upper limit to the mass of the remnant black hole (BH). Here we report on global hydrodynamic simulations of this mechanism that evolve the inner supernova core with a spherically-symmetric, general-relativistic neutrino radiation-hydrodynamic code until BH formation, and the outer stellar layers with a Newtonian code that captures the response of the star to the change in gravity. We find that the dense-matter equation of state (EOS) can introduce a factor of about 2 variation in gravitational mass lost to neutrinos, with a stiff EOS matching previous parametric results, and a soft EOS yielding lower ejecta masses and energies by a factor of several. With a soft EOS, our red and yellow supergiant progenitors fail to unbind mass if hydrogen recombination energy is not included. Our results imply quantitative but not qualitative modifications to previous predictions for shock breakout, plateau emission, and final BH masses from these events. [Preview Abstract] |
Saturday, April 17, 2021 10:57AM - 11:09AM Live |
B10.00002: Possible neutrino signature of hadron-quark phase transition in failing core-collapse supernovae Shuai Zha, Evan O'Connor, André Schneider We study the consequence of a hadron-quark phase transition in failing core-collapse supernovae, which give birth to stellar-mass black holes. In models with a range of progenitor compactness, the protoneutron star collapses and bounces for a second time due to the phase transition. However, this second bounce cannot revive the supernova shock. Instead, the protoneutron star oscillates with the excess kinetic energy and emits a train of neutrino pulses with a period of $\sim$ms. Black-hole formation takes place in a third collapse. The periodic neutrino signal can be a strong indicator for the hadron-quark phase transition in failing core-collapse supernovae if detected in the future. [Preview Abstract] |
Saturday, April 17, 2021 11:09AM - 11:21AM Live |
B10.00003: General Relativistic Neutrino-Driven Turbulence in One-Dimensional Core-Collapse Supernovae Luca Boccioli, Grant Mathews, Evan O'Connor Convection and turbulence in core-collapse supernovae (CCSNe) are inherently three-dimensional in nature. However, 3D simulations of CCSNe are computationally demanding. Thus, it is valuable to modify simulations in spherical symmetry to incorporate 3D effects using some parametric model. In this talk, we report on the formulation and implementation of general relativistic neutrino-driven turbulent convection in the spherically symmetric core-collapse supernova code \texttt{GR1D}. This is based upon the recently proposed method of Supernova Turbulence in Reduced-dimensionality (\textit{STIR}) in Newtonian simulations from Couch et al.~(2020). When the parameters of this model are calibrated to 3D simulations, we find that our GR formulation of \textit{STIR} requires larger turbulent eddies to achieve a shock evolution similar to the original \textit{STIR} model. We also find that general relativity may alter the correspondence between progenitor mass and successful vs.~failed explosions. [Preview Abstract] |
Saturday, April 17, 2021 11:21AM - 11:33AM Live |
B10.00004: Impact of neutrino pair-production rates in Core-Collapse Supernovae Aurore Betranhandy Neutrinos are the main vector of energy transport in the revival process of a stalled supernova shock through the neutrino-driven mechanism. The treatment of their interactions with the medium is therefore an important part of our simulations. Some of these interactions are the pair processes, nucleon-nucleon bremsstrahlung and electron-positron annihilation, which will create or annihilate a neutrino/anti-neutrino pair. In this talk, I will present the results of our latest paper on the impact of pair process treatments in the GR1D supernova evolution code. I will talk about simulations from two different progenitors, one of which producing a successful explosion. These simulations showed that the way of treating nucleon-nucleon bremsstrahlung and electron-positron annihilation has a significant impact on the shock evolution as well as on the neutrino luminosities. [Preview Abstract] |
Saturday, April 17, 2021 11:33AM - 11:45AM Live |
B10.00005: Early emission from supernova explosions through dense porous shells Shane Coffing, Chris Fryer, Suzannah Woods, Carolyn Kuranz During supernova shock breakout, radiation from the supernova shock pours out into the surrounding circumstellar medium. The resulting emission and its interaction with this media can be used to probe stellar and explosion characteristics. Many calculations assume a smooth transition between the outer atmosphere of the star and its wind, however, radiatively-driven instabilities, mass eruptions, convective instabilities, and other mechanisms can produce large-scale inhomogeneous structures such as dense shells and clumps in the wind. The interaction of the breakout emission with these structures can lead to widely varying spectral signatures, particularly in UV and X-ray, unique to the density, composition, state, and distributions of these inhomogeneities. In this work, we present results of 2D multi-group radiation hydrodynamic simulations of supernova shock breakout through inhomogeneous winds, focusing on interaction with dense porous shells that are clumpy, irregular, and optically porous. [Preview Abstract] |
Saturday, April 17, 2021 11:45AM - 11:57AM Live |
B10.00006: Radio observations confirm rebrightening of SN2004dk Arvind Balasubramanian, Dr. Alessandra Corsi, Dr. Tracy Clarke, Dr. Namir Kassim, Dr. Emil Polisensky The study of core collapse supernovae (SNe) provides insights into the physics of such explosions in multiple ways. In particular, radio observations of the SN ejecta can help provide clues about the mass loss history of the progenitor. SN2004dk, a Type Ibc supernova, was first observed in August 2004. \~15 years later, radio observations with both the Very Large Array Low Band Ionosphere and Transient Experiment (VLITE) and the Jansky Very Large Array (VLA), confirm a rebrightening accompanied by H-$\alpha$ emission. This points to a progenitor that emitted its H-rich shell $<1000$ years before the explosion. Here, we discuss our VLITE/VLA observations and conclusions. [Preview Abstract] |
Saturday, April 17, 2021 11:57AM - 12:09PM Live |
B10.00007: Observation of Supernova Neutrino Bursts via CEvNS Adryanna Major, Kate Scholberg Coherent elastic neutrino-nucleus scattering (CEvNS) is a neutral-current process in which a neutrino scatters off an entire nucleus, depositing a tiny recoil energy. The process is important in core-collapse supernovae and also presents an opportunity for detection of the burst of neutrinos ejected in the collapse. The CEvNS process dominates low-energy interactions (tens of MeV) but produces very little energy deposition from the target nuclear recoil. The challenge of its observation is reduced somewhat if a nearby core-collapse supernova acts as a high-flux source, producing thousands of CEvNS events in larger detector volumes over mere seconds. For detectors making use of scintillation to record particle energy loss, the effect would be a uniformly distributed, isotropic scintillation, a "CEvNS glow", throughout the detector. This overall time-localized increase in photon activity could be measurable, giving us critical constraints on the total energy and flux of the explosion. This talk will cover prospects for supernova burst detection via CEvNS in existing and future large detectors of liquid argon and organic liquid scintillator and present a semi-analytic method for obtaining the detected photon spectra of both the CEvNS signal and major expected backgrounds. [Preview Abstract] |
Saturday, April 17, 2021 12:09PM - 12:21PM Not Participating |
B10.00008: CSP-II SE-SNe spectroscopy in the NIR Melissa Shahbandeh, Eric Hsiao, Chris Ashall, Peter Hoeflich I will present a sample of 109 near-infrared (NIR) spectra of 40 Stripped Envelope Core Collapse Supernovae (SESNe), obtained by the Carnegie Supernova Project II (CSP-II). This diverse dataset constitutes the largest NIR sample of SESNe. NIR spectroscopy provides a unique probe for SN physics with several advantages over observations in the optical. Specifically, the He I and C I lines are stronger and more isolated in the NIR. This advantage combined with our large sample allows us to investigate long-standing issues. For example, are SNe Ic truly stripped of their helium or are their helium shells not being sufficiently excited by gamma-rays? We found that all subclasses show a strong profile at 1.05 micron. By using different constraints including velocity and line strength of this feature for selected SNe within the sample, we show that the 1.05 micron feature is most probably carbon in Type Ic SNe. This result indicates that in SNe Ic there is no significant amount of helium shell present. We also detect CO in 8 SNe within the sample, which appears as early as 50 days. CO is an effective cooler and can help us understand the dust production in SESNe. [Preview Abstract] |
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