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|Title:||Electromagnetic Emission from Long-lived Binary Neutron Star Merger Remnants. II. Lightcurves and Spectra||Authors:||Siegel, Daniel M.
|Issue Date:||2016||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||819||Issue:||1||First Page:||15||Abstract:||Recent observations indicate that in a large fraction of binary neutron star (BNS) mergers a long-lived neutron star (NS) may be formed rather than a black hole. Unambiguous electromagnetic (EM) signatures of such a scenario would strongly impact our knowledge on how short gamma-ray bursts (SGRBs) and their afterglow radiation are generated. Furthermore, such EM signals would have profound implications for multimessenger astronomy with joint EM and gravitational-wave (GW) observations of BNS mergers, which will soon become reality thanks to the ground-based advanced LIGO/Virgo GW detector network. Here we explore such EM signatures based on the model presented in a companion paper, which provides a self-consistent evolution of the post-merger system and its EM emission up to ∼10<SUP>7</SUP> s. Light curves and spectra are computed for a wide range of post-merger physical properties. We present X-ray afterglow light curves corresponding to the “standard” and the “time-reversal” scenario for SGRBs (prompt emission associated with the merger or with the collapse of the long-lived NS). The light curve morphologies include single and two-plateau features with timescales and luminosities that are in good agreement with Swift observations. Furthermore, we compute the X-ray signal that should precede the SGRB in the time-reversal scenario, the detection of which would represent smoking-gun evidence for this scenario. Finally, we find a bright, highly isotropic EM transient peaking in the X-ray band at ∼10<SUP>2</SUP>-10<SUP>4</SUP> s after the BNS merger with luminosities of L<SUB>X</SUB> ∼ 10<SUP>46</SUP>-10<SUP>48</SUP> erg s<SUP>-1</SUP>. This signal represents a very promising EM counterpart to the GW emission from BNS mergers.||URI:||http://hdl.handle.net/20.500.12386/30884||URL:||https://iopscience.iop.org/article/10.3847/0004-637X/819/1/15||ISSN:||0004-637X||DOI:||10.3847/0004-637X/819/1/15||Bibcode ADS:||2016ApJ...819...15S||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jun 19, 2021
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