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The Physics of Extreme-Gravity Stars

5–30 Jun 2017
Nordita, Stockholm
Europe/Stockholm timezone

Session

GW (cont) and EM counterparts of compact object mergers

21 Jun 2017, 14:00
122:026 (Nordita, Stockholm)

122:026

Nordita, Stockholm

Presentation materials

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  1. 399. Pulsar binaries with next generation radio telescopes
    Ben Stappers
    21/06/2017, 14:00
    Pulsars in binary systems provide us with excellent opportunities to understand their formation and evolution. Over the last few years there has been a staggering increase in the number of these systems as discovered in radio searches, either blind and particularly guided by Fermi. On the near horizon there are a number of facilities that provide us with even greater sensitivity to...
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  2. 400. Electromagnetic Counterparts of Neutron Star Mergers
    Brian Metzger
    21/06/2017, 14:30
    Hopes are high that Advanced LIGO/Virgo will detect coalescing binary neutron stars in the next few years. Maximizing the scientific return from this discovery will require identifying a coincident electromagnetic counterpart. One possible counterpart is a thermal optical/IR transient, powered by the radioactive decay of neutron-rich elements synthesized in the merger ejecta (a...
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  3. 401. Exploring the Boundary Between Neutron Stars and Black Holes
    Tony Piro
    21/06/2017, 15:00
    Even though we know that stellar mass black holes exist both from those found in our Galaxy and gravitational wave observations, the actual events that give rise to them is poorly understood. Furthermore, the transition between these black holes and neutron stars have important implications for the elusive high density equation of state. I will discuss two avenues for investigating the...
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  4. 402. EM signals following binary black hole mergers
    Andrew King
    21/06/2017, 16:00
  5. 403. Resonant Shattering Flares as EM Counterparts
    David Tsang
    21/06/2017, 16:30
    Resonant Shattering Flares (RSFs) are expected to occur during the inspiral phase for some NS-NS and NS-BH mergers. They result from the resonant tidal excitation of the NS crust-core interface mode fracturing the crust and sparking a relativistic pair-photon fireball, emitted seconds before the merger. RSFs are prompt, bright, and isotropic, allowing detection and triggering...
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  6. 404. The Cocoon Emission - a bright electromagnetic counterpart to neutron star mergers
    Tsvi Piran
    21/06/2017, 16:45
    It is widely accepted that short GRBs are associated from neutron star mergers. As these mergers involve a significant mass ejection, the GRB jet must penetrate this mass before producing the observed radiation. As the jet propagates within the ejecta is create a hot cocoon containing a significant amount of energy. Eventually the cocoon breakout from the ejecta and produces a...
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