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==Theory==
==Theory==
The inspiral and merging of two [[Compact star|compact objects]] are a strong source of [[gravitational wave]]s (GW).<ref name=Metzger2010>{{cite journal |author=Metzger, B. D. |author2=Martínez-Pinedo, G. |author3=Darbha, S. |author4=Quataert, E. |author5=Arcones, A. |author6=Kasen, D. |author7=Thomas, R. |author8=Nugent, P. |author9=Panov, I. V. |author10=Zinner, N. T. |displayauthors=4 |title=Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei |journal=Monthly Notices of the Royal Astronomical Society |volume=406 |issue=4 |page=2650 |date=August 2010 |doi=10.1111/j.1365-2966.2010.16864.x |bibcode=2010MNRAS.406.2650M |arxiv=1001.5029 }}</ref> It is also thought to be the [[Gamma-ray burst progenitors|progenitor]] of short [[gamma-ray burst]]s<ref name=Metzger2010/> and the predominant s[[Light source|ource]] of stable r-process [[Chemical element|elements]] in the [[Universe]].<ref name=Tanvir2013/> The term ''kilonova'' was introduced by Metzger ''et al.'' in 2010<ref name=Metzger2010/> to characterize the energy emitted, which can reach 1000 times the energy emitted in a [[nova]]. The basic model for neutron star mergers was introduced by Li and Paczyński in 1998.<ref name="LiPaczynski1998">{{cite journal|last1=Li-Xin Li and Bohdan Paczyński|title=Transient Events from Neutron Star Mergers|journal=The Astrophysical Journal|date=1998|volume=507|page=L59-L62|url=http://iopscience.iop.org/article/10.1086/311680/fulltext/}}</ref>
The inspiral and merging of two [[Compact star|compact objects]] are a strong source of [[gravitational wave]]s (GW).<ref name=Metzger2010>{{cite journal |author=Metzger, B. D. |author2=Martínez-Pinedo, G. |author3=Darbha, S. |author4=Quataert, E. |author5=Arcones, A. |author6=Kasen, D. |author7=Thomas, R. |author8=Nugent, P. |author9=Panov, I. V. |author10=Zinner, N. T. |displayauthors=4 |title=Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei |journal=Monthly Notices of the Royal Astronomical Society |volume=406 |issue=4 |page=2650 |date=August 2010 |doi=10.1111/j.1365-2966.2010.16864.x |bibcode=2010MNRAS.406.2650M |arxiv=1001.5029 }}</ref> It is also thought to be the [[Gamma-ray burst progenitors|progenitor]] of short [[gamma-ray burst]]s<ref name=Metzger2010/> and the predominant s[[Light source|ource]] of stable r-process [[Chemical element|elements]] in the [[Universe]].<ref name=Tanvir2013/> The term ''kilonova'' was introduced by Metzger ''et al.'' in 2010<ref name=Metzger2010/> to characterize the energy emitted, which can reach 1000 times the energy emitted in a [[nova]]. The basic model for neutron star mergers was introduced by [[Li-Xin Li|Li]] and [[Bohdan Paczyński|Paczyński]] in 1998.<ref name="LiPaczynski1998">{{cite journal|last1=Li-Xin Li and Bohdan Paczyński|title=Transient Events from Neutron Star Mergers|journal=The Astrophysical Journal|date=1998|volume=507|page=L59-L62|url=http://iopscience.iop.org/article/10.1086/311680/fulltext/}}</ref>


==Observations==
==Observations==

Revision as of 06:38, 17 October 2017

A kilonova (macronova or r-process supernova) is a type of supernova that occurs when two neutron stars or a neutron star and a black hole merge in a binary system. Strong electromagnetic radiation is emitted due to the decay of heavy r-process ions that are produced and ejected fairly isotropically during the merger process—similar to a faint, short-lived supernova.[1]


Theory

The inspiral and merging of two compact objects are a strong source of gravitational waves (GW).[2] It is also thought to be the progenitor of short gamma-ray bursts[2] and the predominant source of stable r-process elements in the Universe.[1] The term kilonova was introduced by Metzger et al. in 2010[2] to characterize the energy emitted, which can reach 1000 times the energy emitted in a nova. The basic model for neutron star mergers was introduced by Li and Paczyński in 1998.[3]

Observations

The first clear detection of a kilonova was in 2013, in association with the short-duration gamma-ray burst GRB 130603B, where the faint infrared emission from the distant kilonova was detected using the Hubble Space Telescope.[1]

On October 16, 2017, the LIGO and Virgo collaborations announced the first simultaneous detections of gravitational waves (GW170817) and electromagnetic radiation (GRB 170817A, SSS17a) of any phenomena,[4] and demonstrating that the source was a kilonova caused by a binary neutron star merger.[5] This GRB was in a relatively nearby galaxy, NGC 4993.[6]

See also

References

  1. ^ a b c Tanvir, N. R.; Levan, A. J.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. L. (2013). "A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B". Nature. 500 (7464): 547–9. arXiv:1306.4971. Bibcode:2013Natur.500..547T. doi:10.1038/nature12505. PMID 23912055.
  2. ^ a b c Metzger, B. D.; Martínez-Pinedo, G.; Darbha, S.; Quataert, E.; Arcones, A.; Kasen, D.; Thomas, R.; Nugent, P.; Panov, I. V.; Zinner, N. T. (August 2010). "Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei". Monthly Notices of the Royal Astronomical Society. 406 (4): 2650. arXiv:1001.5029. Bibcode:2010MNRAS.406.2650M. doi:10.1111/j.1365-2966.2010.16864.x. {{cite journal}}: Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  3. ^ Li-Xin Li and Bohdan Paczyński (1998). "Transient Events from Neutron Star Mergers". The Astrophysical Journal. 507: L59-L62.
  4. ^ Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; et al. (LIGO Scientific Collaboration & Virgo Collaboration) (16 October 2017). "GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral". Physical Review Letters. 119 (16). doi:10.1103/PhysRevLett.119.161101.
  5. ^ Miller, M. Coleman (16 October 2017). "Gravitational waves: A golden binary". Nature. News and Views. doi:10.1038/nature24153.
  6. ^ Berger, Edo (16 October 2017). "Focus on the Electromagnetic Counterpart of the Neutron Star Binary Merger GW170817". Astrophysical Journal Letters. IOP Science. Retrieved 16 October 2017.
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