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Kilonovae.

Brian D Metzger1

  • 1Columbia Astrophysics Laboratory, Department of Physics, Columbia University, New York, NY USA.

Living Reviews in Relativity
|June 6, 2017
PubMed
Summary
This summary is machine-generated.

Kilonovae, or macronovae, are supernova-like transients following neutron star mergers. These events produce heavy elements and offer insights into the rapid neutron capture process (r-process).

Keywords:
Black holesGravitational wavesNeutron starsNucleosynthesisRadiative transfer

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Area of Science:

  • Astrophysics
  • Nuclear Physics
  • Gravitational Wave Astronomy

Background:

  • Double neutron star (NS-NS) and black hole-neutron star (BH-NS) mergers are key sources for gravitational wave (GW) detectors.
  • These mergers produce neutron-rich ejecta essential for rapid neutron capture (r-process) nucleosynthesis, creating heavy elements.
  • The radioactive decay of these nuclei powers kilonovae (macronovae), observable electromagnetic counterparts to GW signals.

Purpose of the Study:

  • To review the history and physics of kilonovae, establishing the current understanding of their emission properties.
  • To explore variations from the canonical kilonova model, including blue emission and precursor UV/blue signals.
  • To assess the detectability of kilonovae in conjunction with future GW detections of compact binary mergers.

Main Methods:

  • Review of existing literature on kilonova physics and observational history.
  • Utilizing a simple light curve model to illustrate fundamental kilonova physics.
  • Analysis of potential variations in kilonova emission based on ejecta composition and central engine activity.

Main Results:

  • The established paradigm describes week-long kilonova emission peaking in the near-infrared.
  • Potential variations include day-long optical emission from lanthanide-free ejecta and hour-long UV/blue precursor emission.
  • Enhanced emission can occur due to energy input from central engines like accreting black holes or magnetars.

Conclusions:

  • Kilonovae are crucial electromagnetic counterparts to GW events from compact binary mergers.
  • They serve as direct probes of the r-process nucleosynthesis site, vital for understanding heavy element origins.
  • Future GW detections will be complemented by kilonova observations, enhancing our understanding of these energetic events.