Astronomy:GW190425
GW190425 was a gravitational wave detected[1] on 25 April 2019 at LIGO-Livingston. Some low signal-to-noise data from the Virgo interferometer could not be used for detection but was used for parameter estimation.[2] In contrast to GW170817, LIGO-Hanford was offline and did not observe GW190425, and because the Virgo detection was low-confidence, the event is not well-localized in the sky — the 90% confidence zone spans 8284 deg2 (roughly 20% of the sky), while GW170817 was localized to 28 deg2 (about 0.07% of the sky) before its optical counterpart was identified.[2]
GW190425 was a compact binary coalescence with a signal to noise ratio 12.9.[2] No electromagnetic event has been conclusively associated with GW190425; one candidate is FRB 20190425A in the galaxy UGC 10667.[3]
The signal could be result of a collision of two neutron stars, a neutron star and a low-mass black hole, or two low-mass black holes[4] with a total mass of 3.4+0.3
−0.1 M☉ and a chirp mass of 1.44+0.02
−0.02 M☉, much heavier than any binary neutron-star system known from radioastronomy observations.[2] The unusual mass has led to several different hypothesis for the origin of the signal. Some examples include:[5] a neutron star might paired with 4-5 M☉ Helium star might undergo common envelope evolution then supernova to produce an unusual binary neutron star,[6] higher mass binary neutron stars may be preferentially created with either high or low magnetic fields explaining the lack of radioastronomy signals,[7] and the possibility that the mass observation is at the extreme of a distribution characteristic of binary neutron stars.[8]
References
- ↑ Barbieri, C.; Salafia, O. S.; Colpi, M.; Ghirlanda, G.; Perego, A. (2021-10-01). "Exploring the nature of ambiguous merging systems: GW190425 in low latency" (in en). Astronomy & Astrophysics 654: A12. doi:10.1051/0004-6361/202037778. ISSN 0004-6361. Bibcode: 2021A&A...654A..12B. https://www.aanda.org/articles/aa/abs/2021/10/aa37778-20/aa37778-20.html.
- ↑ 2.0 2.1 2.2 2.3 Abbott, B. P. et al. (2020). "GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M⊙". The Astrophysical Journal Letters 892 (1): L3. doi:10.3847/2041-8213/ab75f5. Bibcode: 2020ApJ...892L...3A.
- ↑ Magaña Hernandez, Ignacio; d'Emilio, Virginia; Morisaki, Soichiro; Bhardwaj, Mohit; Palmese, Antonella (2024). "On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A". The Astrophysical Journal Letters 971 (1): L5. doi:10.3847/2041-8213/ad5b4c. Bibcode: 2024ApJ...971L...5M.
- ↑ "GW190425: the merger of a compact binary with total mass of | ICCUB". https://icc.ub.edu/news/gw190425-merger-a-compact-binary-total-mass.
- ↑ Abbott, R.; Abbott, T. D.; Abraham, S.; Acernese, F.; Ackley, K.; Adams, A.; Adams, C.; Adhikari, R. X. et al. (July 1, 2021). "Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences". The Astrophysical Journal Letters 915 (1): L5. doi:10.3847/2041-8213/ac082e. ISSN 2041-8205. Bibcode: 2021ApJ...915L...5A.
- ↑ Romero-Shaw, Isobel M; Farrow, Nicholas; Stevenson, Simon; Thrane, Eric; Zhu, Xing-Jiang (July 21, 2020). "On the origin of GW190425" (in en). Monthly Notices of the Royal Astronomical Society: Letters 496 (1): L64–L69. doi:10.1093/mnrasl/slaa084. ISSN 1745-3925. https://academic.oup.com/mnrasl/article/496/1/L64/5835715.
- ↑ Safarzadeh, Mohammadtaher; Ramirez-Ruiz, Enrico; Berger, Edo (September 1, 2020). "Does GW190425 Require an Alternative Formation Pathway than a Fast-merging Channel?". The Astrophysical Journal 900 (1): 13. doi:10.3847/1538-4357/aba596. ISSN 0004-637X. Bibcode: 2020ApJ...900...13S.
- ↑ Mandel, Ilya; Müller, Bernhard; Riley, Jeff; de Mink, Selma E; Vigna-Gómez, Alejandro; Chattopadhyay, Debatri (November 18, 2020). "Binary population synthesis with probabilistic remnant mass and kick prescriptions" (in en). Monthly Notices of the Royal Astronomical Society 500 (1): 1380–1384. doi:10.1093/mnras/staa3390. ISSN 0035-8711. https://academic.oup.com/mnras/article/500/1/1380/5948109.
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