Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30884
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Siegel, Daniel M. | en_US |
dc.contributor.author | CIOLFI, RICCARDO | en_US |
dc.date.accessioned | 2021-04-23T13:41:06Z | - |
dc.date.available | 2021-04-23T13:41:06Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30884 | - |
dc.description.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. | en_US |
dc.language.iso | eng | en_US |
dc.title | Electromagnetic Emission from Long-lived Binary Neutron Star Merger Remnants. II. Lightcurves and Spectra | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-637X/819/1/15 | en_US |
dc.identifier.scopus | 2-s2.0-84960864130 | en_US |
dc.identifier.isi | WOS:000372303400015 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/819/1/15 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 819 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 15 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 2 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | DEU | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJ...819...15S | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_11 Relativistic astrophysics | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0003-3140-8933 | - |
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