Bulletin of the American Physical Society
APS April Meeting 2013
Volume 58, Number 4
Saturday–Tuesday, April 13–16, 2013; Denver, Colorado
Session L5: Invited Session: Gravitational Wave Astrophysics |
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Sponsoring Units: GGR DAP Chair: Daniel Holz, University of Chicago Room: Governor's Square 14 |
Sunday, April 14, 2013 3:30PM - 4:06PM |
L5.00001: Gravitational Waves: Probes of Stellar Collapse Invited Speaker: Chris Fryer Supernovae arising from the core-collapse of a massive star produce outbursts in a broad range of photon wavelengths and this emission dominates most studies of supernovae. But neutrinos and gravitational waves provide a much more direct means to study the explosive engine deep in the collapsed core. Here we review the limitations of photon observations in studying the supernova engine, focusing on what we can learn from neutrinos and gravitational waves. Gravitational waves also provide an additional probe of the supernova engine, a study of the compact remnant mass, and we will also discuss this indirect probe of the supernova engine. [Preview Abstract] |
Sunday, April 14, 2013 4:06PM - 4:42PM |
L5.00002: Learning about dense matter from gravitational waves Invited Speaker: Jocelyn Read Binary neutron stars are some of the most promising sources for gravitational-wave detections with Advanced LIGO. For any gravitational-wave source containing matter, the matter contributes to the spacetime dynamics, leaving an imprint on radiation from the system. I will discuss how we can understand and model this imprint, so that we can use it to constrain our understanding of the properties of dense matter, with a focus on the inspiral and merger of binary neutron stars. [Preview Abstract] |
Sunday, April 14, 2013 4:42PM - 5:18PM |
L5.00003: Gravitational waves from binaries and dense stellar clusters Invited Speaker: Will Farr It is an exciting time for gravitational wave astrophysics! The LIGO and Virgo gravitational wave detectors are currently undergoing an upgrade that will improve their sensitivity by a factor of about 10. At this ``advanced'' sensitivity, it is likely that they will detect at least one gravitational wave signal from a coalescing compact binary per year; it is possible that detection rates may be several hundred times that. Many of these sources are possibly formed in dense stellar environments---though the exact rates of field and cluster formation are uncertain. I will discuss the state-of-the-art in extracting information about the binary system's properties from these signals and what this information can tell us about the formation environment of the coalescing objects. I will review our current knowledge---and uncertainty---about the formation mechanisms of these objects, highlighting the ways that gravitational wave observations can inform our understanding. Finally, I will discuss some recent modeling results that run contrary to decades old assumptions about the formation of binary black hole gravitational wave sources in globular clusters and the implications for gravitational wave astronomy. [Preview Abstract] |
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