Bulletin of the American Physical Society
APS April Meeting 2010
Volume 55, Number 1
Saturday–Tuesday, February 13–16, 2010; Washington, DC
Session Y1: Neutrino Astrophysics |
Hide Abstracts |
Sponsoring Units: DPF DAP Chair: Kara Hoffman, University of Maryland Room: Marriott Ballroom Salon 2 |
Tuesday, February 16, 2010 1:30PM - 2:06PM |
Y1.00001: Results from the ANITA search for Ultra-High Energy Neutrinos and Cosmic Rays using the Radio detection technique Invited Speaker: ANITA is a balloon-borne radio telescope flown on Long Duration Balloons in Antarctica. The payload looks for Ultra-high energy cosmic neutrinos striking the ice via their emission of radio-Cherenkov radiation. I will present the results of our neutrino searches in the data from ANITA's two full flights. In a different polarization, ANITA observes the radio emission of extensive air showers via their radio emission in the atmosphere below the payload. I will present evidence for these events being induced by cosmic rays and discuss their properties. [Preview Abstract] |
Tuesday, February 16, 2010 2:06PM - 2:42PM |
Y1.00002: Cosmic Rays and Neutrinos above 10$^{21}$ eV - the NuMoon experiment with WSRT and LOFAR Invited Speaker: Ultra-High Energy Cosmic Ray particles (UHECR) are known to reach energies at least up to 10$^{20}$ eV, providing potential insight into physics that cannot be studied by current or upcoming particle accelerators. However, those particles are extremely rare and large natural detector volumes are needed to detect them. Here radio detection techniques provide interesting possibilities. Geosychrotron radiation in the Earth's atmosphere or radio Cherenkov (Askaryan) emission in solid media make it possible to observe radio waves from showers induced by UHECRs and neutrinos. In the NuMoon project we have used the Westerbork Synthesis Radio Telescope (WSRT) to monitor the lunar surface for an aggregate observing time of 46 hours at a frequency around 150 MHz. This has allowed us to improve current limits for the cosmic neutrino flux above 4$\times $10$^{22}$ eV by almost an order of magnitude, bringing it into an astrophysically interesting regime. In the future we will be using the new LOFAR interferometer to lower this neutrino limit further by at least one to two orders of magnitude. In addition we will place further constraints on UHECR beyond the Greisen-Zatsepin-Kuzmin (GZK) cut-off ($>$10$^{20}$ eV) and detect air showers from cosmic rays at lower energies around 10$^{18}$ eV. [Preview Abstract] |
Tuesday, February 16, 2010 2:42PM - 3:18PM |
Y1.00003: Neutrinos from Supernovae: Flavor Transformation, Detection and Nucleosynthesis Invited Speaker: Supernova neutrinos are of interest for a number of reasons. A future detection will provide a rare opportunity to obtain information about the supernova core, and perhaps also about the hydrodynamics of the explosion and/or the properties of the neutrinos themselves. In addition to traditional supernovae, MeV scale neutrinos also originate from sources such as black-hole accretion disk supernova, gamma ray bursts and compact object mergers. Astrophysically produced MeV scale neutrinos exhibit a rich variety of behavior. Neutrino flavor transformation in all these environments is affected by a changing stellar and neutrino density profile, and new flavor transformation behavior of neutrinos recently has been discovered. Neutrinos from these environments play a crucial role in element synthesis. I will review some recent developments in these areas. [Preview Abstract] |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700