Bulletin of the American Physical Society
2019 Annual Meeting of the APS Four Corners Section
Volume 64, Number 16
Friday–Saturday, October 11–12, 2019; Prescott, Arizona
Session J01: Astrophysics II |
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Chair: Stacy Palen, Weber State University Room: AC1 107 |
Saturday, October 12, 2019 8:00AM - 8:24AM |
J01.00001: The Core Collapse Supernova Gravitational Wave Frontier Invited Speaker: Michele Zanolin The detection of gravitational waves (GWs) from binary systems with laser interferometers has opened a new era of Astronomy. GWs from Core collapse supernovae could provide drastically new knowledge. In this talk I will review the challenges and opportunities of the CCSN research program, including the landscape of the progenitors, data analysis methodologies and hardware requirements. [Preview Abstract] |
Saturday, October 12, 2019 8:24AM - 8:36AM |
J01.00002: Detectability of the SASI Activity of Supernova Neutrino Fluxes Colter Richardson, Zidu Lin, Cecilia Lunardini, Michele Zanolin, Kei Kotake In this presentation we discuss the detectability of the Standing Accretion Shock Instability (SASI) signatures in the neutrino luminosity in Core-Collapse Supernovae (CCSN) and the capability to estimate some of its physical parameters. We apply the methodology to the luminosity as computed by numerical simulations of the CCSN, and the distortions that IceCube and Hyper-K would induce at different distances. [Preview Abstract] |
Saturday, October 12, 2019 8:36AM - 8:48AM |
J01.00003: Shocked Electrons: Determination of the Heating Mechanism in Abell 665 Vivek Vankayalapati, Daniel Wik Mergers between galaxy clusters drive shock fronts in the intracluster medium (ICM), heating thermal electrons, causing an increase in their temperature. The mechanism by which this occurs is undetermined, with two models being proposed to explain the phenomenon. One proposes direct shock-heating and the other suggests indirect adiabatic compression with subsequent ion-equilibration. We utilize NuSTAR observations of a shock in the merging cluster Abell 665 in order to discriminate between the models. A temperature profile was constructed across the shock in order to compare against the models' predictions. In addition, temperature maps across the cluster are generated in order to understand merger activity. We find that the temperature profile is suggestive of the shock model but is not statistically significant, due to NuSTAR's comparatively worse spatial resolution. Current work is joint fitting the NuSTAR data with Chandra observations in order to statistically distinguish between the models for the first time. Understanding these processes increases our understanding of the magnetic field of the ICM, allowing galaxy clusters to be used to constrain cosmology. [Preview Abstract] |
Saturday, October 12, 2019 8:48AM - 9:00AM |
J01.00004: Conversion electron detector for Laboratory Nuclear Astrophysics Reactions John E. Ellsworth The role electrons play in enhancing nucleosynthesis reactions is of great interest. There is also some interest in the possibility of electrons acting as a catalyst. Steven Jones, after having observed the ultimate fusion rate for muon catalyzed fusion, posited in 1986 the possibility of electrons catalyzing fusion reactions, which prompted the BYU Geo-Fusion Hypothesis. In 2017, Matej Lipoglavsek reported the `Observation of electron emission in the nuclear reaction between protons and deuterons.' To investigate the possibility of an enhanced rate of conversion electrons from other reactions an accelerator target chamber is being constructed. Described here is the target chamber and its charged particle detector designed to include electrons up to 25MeV. [Preview Abstract] |
Saturday, October 12, 2019 9:00AM - 9:12AM |
J01.00005: Introducing the Model-Agnostic Dark Halo Analysis Tool (\texttt{MADHAT}) Pearl Sandick, Kimberly Boddy, Stephen Hill, Jason Kumar, Barmak Shams Es Haghi We present a brief overview of the Model-Agnostic Dark Halo Analysis Tool (\texttt{MADHAT}), a numerical tool that implements a Fermi-LAT data-driven, model-independent analysis of gamma-ray emission due to dark matter annihilation in dwarf spheroidal galaxies. This tool efficiently provides statistical upper bounds on dark matter annihilation using a stacked analysis of any selected set of dwarf spheroidal galaxy targets, under any assumptions the user makes regarding dark sector particle physics or astrophysics. [Preview Abstract] |
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