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 B11: Dark Matter: Stars & DetectorsLive
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Sponsoring Units: DAP Chair: Louis Strigari, TAMU |
Saturday, April 17, 2021 10:45AM - 10:57AM Live |
B11.00001: Stellar Cooling, Inelastic Dark Matter, and XENON Wai-Yee Keung, Danny Marfatia, Po-Yan Tseng We consider a novel scenario of dark photon-mediated inelastic dark matter to explain the white dwarf cooling excess suggested by its luminosity function, and the excess in electron recoil events at XENON1T. In the Sun, the dark photon $A'$ is produced mainly via thermal processes, and the heavier dark matter $\chi_2$ is produced by the scattering of halo dark matter $\chi_1$ with electrons. The XENON1T signal arises primarily by solar $A'$ scattering, and $A'$ emission by white dwarfs accommodates the extra cooling while maintaining consistency with other stellar cooling observations. A tritium component in the XENON1T detector is also required. We show for parameters that explain the XENON1T data, but not the white dwarf cooling anomaly, that a second signal peak may be buried in the XENON1T data and revealable at XENON1T. However, the parameters that give the double peak in the spectrum are incompatible with constraints from horizontal branch stars. [Preview Abstract] |
Saturday, April 17, 2021 10:57AM - 11:09AM Live |
B11.00002: Searching for Solar WIMPs with Ten Years of IceCube Data Jeffrey Lazar, Carlos Argüelles, Qinrui Liu, Ali Kheirandish The existence of dark matter (DM) has been well-established by repeated experiments probing many length scales. Even though DM is expected to make up 85\% of the current matter content of the Universe, its nature remains unknown. One broad class of corpuscular DM motivated by Standard Model (SM) extensions is weakly interacting massive particles (WIMPs). WIMPs can generically have a non-zero cross-section with SM nuclei, which allows them to scatter- off nuclei in large celestial bodies such as the Sun, losing energy and becoming gravitationally bound in the process. After repeated scattering, WIMPs can sink to the solar center, leading to an excess of WIMPs there. Furthermore, WIMPs can annihilate to unstable SM particles, which will eventually create stable SM particles. Only neutrinos can escape the dense solar core. Thus, neutrino observatories may look for these neutrinos as evidence of WIMPs. In this talk, I will present the current status of IceCube's solar WIMP search, which covers the range from 10~GeV to 1~TeV [Preview Abstract] |
Saturday, April 17, 2021 11:09AM - 11:21AM Live |
B11.00003: Self interacting dark matter halo and binary neutron star mergers. Lan Nguyen We study the gravitational effect of dark matter on compact astronomical objects. The MeV dark matter model in which dark matter self-interaction can be constrained by observation of gravitational wave from binary neutron star mergers and how the density of the dark matter affects the physical properties of the neutron star and its tidal deformability. [Preview Abstract] |
Saturday, April 17, 2021 11:21AM - 11:33AM Live |
B11.00004: Asymmetric dark stars and neutron star stability Moira Gresham We describe gravitationally bound states of fermionic asymmetric dark matter (ADM stars), and the impact of ADM capture on the stability of neutron stars. We describe and motivate equations of state describing fermionic ADM with generic attractive and repulsive interactions, and the corresponding equilibrium sequences and maximum masses of fermionic ADM stars. Gravitational wave searches can utilize our solutions to model exotic compact objects (ECOs). Contrary to some previous claims in the literature, we also argue that fermionic ADM with an attractive interaction is no more effective in destabilizing neutron stars than fermionic ADM with no self-interactions. [Preview Abstract] |
Saturday, April 17, 2021 11:33AM - 11:45AM Live |
B11.00005: A Proposal to Use MiX for a Low Energy Nuclear Recoil Calibration Yi Liu, Chami Amarasinghe, Dongqing Huang Dual-phase xenon time projection chamber (TPC) detectors are leading the weakly interacting massive particle (WIMP) dark matter searches. A better understanding of the low energy nuclear recoil (NR) response in liquid xenon (LXe) will allow experiments to be increasingly sensitive to light dark matter and coherent neutrino-nucleus scattering. The Michigan Xenon detector (MiX) is a small dual-phase TPC (140 g active volume) with 3D position sensitivity. MiX possesses light gains of (0.239\textpm 0.012) pe/photon and charge signal gains of (16.1\textpm 0.6) pe/electron, and therefore provides a great opportunity to calibrate LXe response to lower energies than previously achieved. We will discuss recent studies to use the MiX detector to perform a low energy NR calibration using thermal neutron capture in LXe with a pulsed deuterium-deuterium (D-D) neutron source. [Preview Abstract] |
Saturday, April 17, 2021 11:45AM - 11:57AM Live |
B11.00006: New Experimental Phenomena That The Photo-Voltages Be Remotely Changed At Same Rate Dayong Cao In our experiments, the light of the lamp radiated on four solar cells to produce four different photo-voltages such asV1, V2, V3, V4 . The tester used consciousness to think to increase the four photo-voltages, and got four new photo-voltages such asV'1, V'2, V'3, V'4 . The special Phenomena is there is the same rate for four changed photo-voltages. (V'1-V1)/V1$=$ (V'2-V2)/V2$=$ (V'3-V3)/V3$=$ (V'4-V4)/V4$=$64{\%} . In another experiment, the rate is240{\%} . A idea is there is physical thought waves. By experimental Phenomena, the thought waves are slow waves (as low frequency waves and gravitational waves), and it is not bright waves. How can the thought waves increase the photo-voltages which were produced by the light of the lamp? If there was light of another lamp to instead of the thought waves to increase ``the four photo-voltages'' (such as V1, V2, V3, V4), and got four new photo-voltages such as V''1, V''2, V''3, V''4. And (V''1-V1)/V1$\ne $ (V''2-V2)/V2$\ne $ (V''3-V3)/V3$\ne $ (V''4-V4)/V4 . The thought waves (as gravitational waves) which is spacetime radiations is radiations of the dark matter-dark energy . That is a method to observe the dark matter-dark energy and the dark comets of the dark matter who will impact to our earth. The new solar cell could produce enough power of the photo-voltage at night. [Preview Abstract] |
Saturday, April 17, 2021 11:57AM - 12:09PM Live |
B11.00007: Re-analysis of 3.5 keV line Yujin Park, Benjamin Safdi, Joshua Foster, Christopher Dessert I describe a reanalysis of data sets that have previously been found to harbor evidence for an unidentified X-ray line at 3.5 keV in order to quantify the robustness of earlier results that found significant evidence for a new X-ray line at this energy. The 3.5 keV line is intriguing in part because of possible connections to dark matter. We analyze observations from the XMM-Newton and Chandra telescopes. We investigate the robustness of the evidence for the 3.5 keV line to variations in the analysis framework and also to numerical error in the chi-square minimization process. For example, we consider narrowing the energy band for the analysis in order to minimize mismodeling effects. The results of our analyses indicate that many of the original 3.5 keV studies (i) did not have fully converged statistical analyses, and (ii) were subject to large systematic uncertainties from background mismodeling. Accounting for these issues we find no statistically significant evidence for a 3.5 keV line in any X-ray data set. [Preview Abstract] |
Saturday, April 17, 2021 12:09PM - 12:21PM Live |
B11.00008: An Optimized Search for Dark Matter in the Galactic Halo with HAWC Joseph Lundeen The Galactic Halo is the closest known large dark matter halo and a prime candidate for indirect dark matter detection. The High Altitude Water Cherenkov Observatory (HAWC) is a high energy (300 GeV to 100 TeV) gamma ray detector located in central Mexico. HAWC operates via the water Cherenkov technique and has both a wide (~2 sr) field of view and near continuous duty cycle, making it ideal for analysis of highly extended sources. We made use of HAWC's field of view and a background-estimation technique optimized for extended sources to probe a large region of the Galactic Halo for dark matter signals. With these results, we are able to set improved constraints on dark matter annihilation and decay over the HAWC energy range, taking into account electroweak corrections to the gamma-ray spectra. Our constraints also take into account detector simulation systematics and are robust against uncertainties in the Galactic dark matter spatial profile. [Preview Abstract] |
Saturday, April 17, 2021 12:21PM - 12:33PM Live |
B11.00009: Charcoal-based Radon Reduction for Rare Event Detectors Maris Arthurs, Dongqing Huang, Chamindu Amarasinghe, Eric Miller, Wolfgang Lorenzon Radon and its daughters constitute the most significant background in many rare event searches, since they are continuously re-supplied from detector materials. The principle challenge for radon reduction of multi-tonne noble-liquid detector systems using charcoal-based systems is the intrinsic radon activity of the charcoal adsorbent itself. In this presentation, we will discuss radon dynamics in vacuum swing adsorption systems, and show that it appears possible to build effective radon mitigation systems, if adsorbents with about three times lower intrinsic radon activity than in currently available activated charcoals are available. [Preview Abstract] |
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