Bulletin of the American Physical Society
80th Annual Meeting of the APS Southeastern Section
Volume 58, Number 17
Wednesday–Saturday, November 20–23, 2013; Bowling Green, Kentucky
Session ED: Invited Session on Astrophysics |
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Chair: Tina Lund, North Carolina State University Room: 3/4 |
Friday, November 22, 2013 8:30AM - 9:06AM |
ED.00001: Neutrino Transport in Core-collapse Supernova Simulations Invited Speaker: Christian Cardall Neutrino transport is a key physical ingredient of core-collapse supernova simulations. Almost all of the gravitational binding energy released by the collapsing core of a dying massive star emerges in the form of intense neutrino fluxes. A small fraction of this energy is absorbed in the semi-transparent region outside the newly-born neutron star, and is believed to be responsible for powering the supernova explosion that follows core collapse. The ORNL group and its collaborators have used or are developing three different simulation codes, each with a different approach to neutrino transport: a full Boltzmann solve in 1D position space (spherical symmetry) + 2D momentum space; ray-by-ray flux-limited diffusion in 2D (axisymmetry) or 3D position space + 1D momentum space; and a two-moment variable Eddington factor method in 3D position space + 1D momentum space. [Preview Abstract] |
Friday, November 22, 2013 9:06AM - 9:42AM |
ED.00002: Stimulated Neutrino Transformation With Multiple Sinusoidal Potentials Invited Speaker: Kelly Patton Neutrinos have been known to oscillate between their flavors as they propagate for almost two decades, but a detailed understanding of their oscillation behavior in complex astrophysical environments, such as core collapse supernovae, is a subject of ongoing investigation. We study one aspect of such an environment - what happens when the matter density that the neutrinos travel through is not smooth, or is even turbulent? We consider the effect of density fluctuations on neutrino flavor transformation and find some startling results. By decomposing the matter density into a Fourier series, we find that two different ranges of frequencies contribute to the evolution. The first are those terms with frequencies corresponding to the energy splitting between the neutrino states or an integer fraction of that splitting, a phenomenon known as parametric resonance. Additionally, we show analytically that the long wavelength modes also significantly affect the results. We find that we can successfully predict the amplitudes and wavelengths of the resulting oscillations between the neutrino states for matter density profiles which consist of up to fifty Fourier modes.\\[4pt] In collaboration with James Kneller and Gail McLaughlin, North Carolina State University. [Preview Abstract] |
Friday, November 22, 2013 9:42AM - 10:18AM |
ED.00003: Neutrinos and black hole accretion disk nucleosynthesis Invited Speaker: Rebecca Surman The collapse of a massive, rotating star or the collision of two compact objects can produce a stellar mass black hole surrounded by a rapidly accreting disk of debris. This accretion disk is a source of intense neutrino emission, which can influence the dynamics of the event and shape the element synthesis that occurs in the disk outflows. Here we discuss the latter, noting in particular the influence of neutrino oscillations and neutrino general relativistic effects on the outflow nucleosynthesis. [Preview Abstract] |
Friday, November 22, 2013 10:18AM - 10:54AM |
ED.00004: Supernova Neutrino Detection with IceCube - Overview and Outlook Invited Speaker: Benedikt Riedel The IceCube Neutrino Observatory is a 1 km$^{3}$ scale neutrino telescope completed in the Austral summer of 2010/2011. The detector forms a lattice of 5,160 photomultiplier tubes (PMTs) installed in the South Polar ice cap at depths from 1450 to 2450 m. IceCube is designed to detect astrophysical neutrinos upward of 100 GeV. The special environment of the Antarctic ice and low-noise PMTs make the detection of a large MeV neutrino number flux possible as a collective rise in all photomultiplier rates on top of the dark noise. Assuming a supernova at the galactic center, the detectors sensitivity compares to a background-free megaton-scale supernova search experiment. At present, supernova data acquisition provides a 2 ms time resolution, allowing to track subtle features in the temporal development of a supernova neutrino burst. Recent work has been focussed on deepening the understanding and subsequently removing several dark noise contributions, especially from atmospheric muons, improving the detector response to supernova neutrinos, and setting a limit on the number of dark supernovae in the galaxy. [Preview Abstract] |
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