The electromagnetic signals of compact binary mergers

By T. Piran, E. Nakar, Stephan Rosswog. 2012

226 citations recorded by the source corpus.

Compact binary mergers are prime sources of gravitational waves (GWs), targeted by current and next generation detectors. The question 'what is the observable electromagnetic (EM) signature of a co ...

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/18aff519ea7a9c525e429c035298b3015a1f4b54

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. B. Metzger
2. E. Berger
3. Bing Zhang
4. E. Quataert
5. D. Kasen
6. R. Fern'andez
7. David Radice
8. Luke F. Roberts

In Nuclear and High Energy Physics

1. B. Metzger
2. Bing Zhang
3. E. Berger
4. E. O’Connor
5. D. Kasen
6. Stephan Rosswog
7. Christian D. Ott
8. R. Fern'andez

Citations in the corpus

• The long-term evolution of neutron star merger remnants { II. Radioactively powered transients (2013, methodology): “Subsequently much effort has been invested in refining macronova models and in further understanding their properties (Kulkarni 2005; Rosswog 2005; Metzger et al. 2010; Goriely et al. 2011; Roberts et al. 2011; Bauswein et al. 2013; Piran et al. 2013; Rosswog et al. 2013).”
• Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “…electromagnetic counterparts would provide crucial information to localize the astrophysical environments of gravitational wave signals (Metzger & Berger 2012; Nissanke et al. 2013; Piran et al. 2013; Singer et al. 2014; Chu et al. 2015; Ghosh et al. 2015; Bartos et al. 2016; Abbott et al. 2016a).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “…1998; Kulkarni, 2005; Metzger et al., 2010), and a long-lasting radio afterglow due to the interaction of the ejecta with the surrounding matter (Rezzolla et al., 2010; Nakar and Piran, 2011; Shibata et al., 2011; Metzger and Berger, 2012; Piran et al., 2013; Kyutoku et al., 2012, 2013).”
• DOUBLE COMPACT OBJECTS. II. COSMOLOGICAL MERGER RATES (2013, background): “Since this matter may be enriched in heavy elements through the r-process, the resulting radioactive decay may generate observable light, thereby providing a promising electromagnetic counterpart to the GW emission (Metzger & Berger 2012; Piran et al. 2013; Barnes & Kasen 2013).”
• NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “Such kilonovae are an important facet in the multi-messenger view of compact binary mergers (Rosswog 2015) and, since they emit quasi-isotropically, they may become crucial in assuring the first direct gravitational wave detections (Metzger & Berger 2012; Nissanke et al. 2013; Piran et al. 2013).”
• First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, unknown): “…and theoretical studies of r-process enrichment, Mrp = 0.05 M (Rosswog et al. 1999; Metzger et al. 2010; Roberts et al. 2011; Bauswein et al. 2013; Piran et al. 2013; Grossman et al. 2014; Just et al. 2015; Ramirez-Ruiz et al. 2015), γNSNS/γSNIa = 10−3, and γSNIa,MW ≈ 5 × 10−3yr−1 (Crocker et al.…”
• Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, background): “Previous studies showed that such signals can be produced by several different ejecta components, e.g., an SGRB jet, cocoon, and dynamical ejecta (van Eerten & MacFadyen 2011; Piran et al. 2013; Hotokezaka & Piran 2015).”
• Unequal mass binary neutron star mergers and multimessenger signals (2016, background): “(For Newtonian or approximate GR, studies have been presented in [53, 54].”
• A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, methodology): “Appendix Layered Kilonova Model Multi-velocity semi-analytic one-dimensional kilonova models have been considered in several previous works (e.g., Piran et al. 2013; Metzger 2017; Waxman et al. 2017).”
• Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, background): “Note that equation (12) may be overestimating the deceleration time, because it does not account for asphericities and nonuniform velocities in the outflows (Piran et al. 2013; Margalit & Piran 2015).”
• BRIGHT “MERGER-NOVA” FROM THE REMNANT OF A NEUTRON STAR BINARY MERGER: A SIGNATURE OF A NEWLY BORN, MASSIVE, MILLISECOND MAGNETAR (2013, background): “…nuclear synthesis, radiative transfer, etc (e.g., Kulkarni 2005; Rosswog 2005; Metzger et al. 2010; Goriely et al. 2011; Roberts et al. 2011; Barnes & Kasen 2013; Bauswein et al. 2013; Grossman et al. 2013; Piran et al. 2013; Rosswog et al. 2013; Takami et al. 2013; Tanaka & Hotokezaka 2013).”
• HIRAX: a probe of dark energy and radio transients (2016, background): “HIRAX will add radio transient monitoring to this suite of observations, which will open up the discovery space for transient phenomena and contribute to multi-messenger science, for example following up nearby explosive events found by LIGO.(30) In addition, Fast Radio Bursts (FRBs) are a source of”
• The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, background): “…electromagnetic transients powered by radioactivity, so-called ‘macronovae’ (Li & Paczyński 1998; Kulkarni 2005; Rosswog 2005; Metzger et al. 2010; Roberts et al. 2011; Goriely et al. 2011a; Metzger & Berger 2012; Kelley et al. 2012; Rosswog et al. 2013; Piran et al. 2013; Barnes & Kasen 2013).”
• Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, background): “…transient peaks on longer timescales – up to a ∼ week – and at a lower luminosity and frequency – in the near infrared rather than optical (Barnes & Kasen 2013; Tanaka & Hotokezaka 2013) – than in original models that assumed opacity similar to Fe (e.g. Metzger et al. 2010, Piran et al. 2013).”
• AN r-PROCESS KILONOVA ASSOCIATED WITH THE SHORT-HARD GRB 130603B (2013, methodology): “The inferred ejecta mass agrees with the results of merger simulations, which predictMej ∼ (0.5− 5)×10−2 M⊙ (depending on the mass ratio of the binary constituents; Goriely et al. 2011; Piran et al. 2013).”