Bulletin of the American Physical Society
APS April Meeting 2019
Volume 64, Number 3
Saturday–Tuesday, April 13–16, 2019; Denver, Colorado
Session D03: Wilson Prize and Dissertation AwardsInvited
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Sponsoring Units: DPB DPF Chair: Michael Witherell, Lawrence Berkeley National Laboratory Room: Sheraton Plaza E |
Saturday, April 13, 2019 3:30PM - 3:50PM |
D03.00001: Wilson Prize -- Wakefield Acceleration (WFA) in Laboratories and Beyond Invited Speaker: Toshiki Tajima Wakefields excited by laser or beams of particles are a robustly stable, energetically elevated entity in plasma capable of accelerating particles in high gradients [1]. Since the first laser WFA (LWFA) demonstration in 1994 [2], spectacular experimental developments around the world ensued, showing a variety of possible applications to future high energy accelerators, ultrafast radiolysis, intraoperative radiation therapy, betatron X-ray measurements, etc. LWFA also has driven the peak performance of the CPA laser technology, spawning out High Field Science. We now consider the possibility of X-ray nanotube/crystal wakefield acceleration. Meanwhile, the Mother Nature has far along created (we learned in 2017) astrophysical wakefields that produced gamma bursts in such events as the simultaneous gravitational wave emission from compact objects.
[1] Tajima, T. and Dawson, J.M., Laser Electron Accelerator, Phys. Rev. Lett. 43, 267 (1979).
[2] Nakajima, K., Kawakubo, T., Nakanishi, H., Ogata, A., Kato, Y., Kitagawa, Y., Kodama, R., Mima, K., Shiraga, H., Suzuki, K., Zhang, T., Sakawa, Y., Shoji, T., Nishida, Y., Yugami, N., Downer, M., Fisher, D., Newberger, B., and Tajima, T., A Proof-of Principle Experiment of Laser Wakefield Acceleration, Phys. Scripta T52, 61 (1994). |
Saturday, April 13, 2019 3:50PM - 4:10PM |
D03.00002: Mitsuyoshi Tanaka Dissertation Award Talk: First results from the HAYSTAC axion search Invited Speaker: Benjamin M Brubaker Hypothetical particles called axions are among the leading candidates for the mysterious cold dark matter (CDM) that binds galaxies together and constitutes more than 80% of the matter in the universe. CDM axions may be detected via their resonant conversion into photons in a "haloscope" detector: a tunable, high-$Q$ microwave cavity maintained at cryogenic temperature, immersed a strong magnetic field, and coupled to a low-noise receiver. At the limits of current technology, the conversion power in such a detector is $\lesssim 10^{-22}\mathrm{ W}$ for $\mu\mathrm{eV}$-mass axions, and drops rapidly with increasing axion mass, because higher frequency cavities with smaller resonant volumes are required. In this talk I will introduce the essential physics of CDM axion detection, and review the main results of my doctoral research with HAYSTAC (the Haloscope at Yale Sensitive to Axion CDM), for which I received the 2019 Tanaka award. HAYSTAC is the first detector to achieve sensitivity to viable axion models in the $10\mathrm{ }\mu\mathrm{eV}$ mass decade, and the first to demonstrate noise performance limited by the laws of quantum mechanics. I will end the talk with a brief preview of next steps for HAYSTAC specifically and a broader outlook for the field of light dark matter detection. |
Saturday, April 13, 2019 4:10PM - 4:30PM |
D03.00003: Evidence the 3.5 keV line is not from dark matter decay Invited Speaker: Nicholas Rodd X-ray observations of nearby clusters and galaxies have reported an unexpected X-ray line around 3.5 keV. This line has received significant attention due to its possible explanation through decaying dark matter; in particular, decaying sterile neutrino models, with a sterile neutrino mass around 7 keV, provide a good fit to the available data. We use over 30 Ms of XMM-Newton blank-sky observations to search for evidence of the 3.5 keV line consistent with arising from decaying dark matter within the ambient halo of the Milky Way. We find the strongest limits to-date on the lifetime of dark matter in this mass range, strongly disfavoring the possibility that the 3.5 keV line originates from dark matter decay. |
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