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V404 Cygni

V404 Cygni is a microquasar and a triple star system in the constellation of Cygnus . It contains a black hole with a mass of about 9 M ☉ and an early K giant star companion w...

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V404 Cygni is a microquasar and a triple star system in the constellation of Cygnus. It contains a black hole with a mass of about 9 M☉ and an early Kgiant star companion with a mass slightly smaller than the Sun, and an evolved tertiary component. The inner star and the black hole orbit each other every 6.47129 days at fairly close range, while the outer tertiary takes 70000 years to orbit the inner binary system.[10] Due to their proximity and the intense gravity of the black hole, the secondary star loses mass to an accretion disk around the black hole and ultimately to the black hole itself.[11]

The "V" in the name indicates that it is a variable star, which repeatedly gets brighter and fainter over time. It is also considered a nova, because at least three times in the 20th century it produced a bright outburst of energy. Finally, it is a soft X-ray transient because it periodically emits short bursts of X-rays.

The black hole companion has been proposed as a Q star candidate.[12]

Observation history

Rare X-ray outburst from a stellar-mass black hole in the binary system V404 Cygni. Video on YouTube

The system was first noted as Nova Cygni 1938 and given the variable star designation V404 Cygni. It was considered to be an ordinary "moderately fast" nova although large fluctuations were noted during the decline. It was discovered after maximum light, and the photographic magnitude range was measured at 12.5–20.5.[13]

On May 22, 1989 the Japanese Ginga Team discovered a new X-ray source that was catalogued as GS 2023+338.[14] This source was quickly linked to V404 Cygni, which was discovered to be in outburst again as Nova Cygni 1989.[15][16]

Follow-up studies showed a previously unnoticed outburst in 1956. There was also a possible brightening in 1979.[17]

En 2009, el agujero negro en el sistema V404 Cygni se convirtió en el primer agujero negro en tener una medición de paralaje precisa para su distancia al Sistema Solar . Medida mediante interferometría de línea de base muy larga utilizando el High Sensitivity Array , la distancia es2,39 ± 0,14 kiloparsecs  , [ 18 ] o7800 ± 460 años luz .

En abril de 2019, los astrónomos anunciaron que los chorros de partículas que salían del agujero negro oscilaban de un lado a otro en el orden de los minutos, algo nunca antes visto en los chorros de partículas que emanan de un agujero negro. Los astrónomos creen que la oscilación es causada por el efecto Lense-Thirring debido a la curvatura del espacio-tiempo por el enorme campo gravitatorio en las proximidades del agujero negro. [ 19 ]

En abril de 2024, los astrónomos anunciaron que se descubrió que V404 Cygni forma parte de un sistema estelar triple jerárquico, con la compañera terciaria ubicada a al menos 3500 UA del sistema binario interno. [ 9 ] Este descubrimiento demostró que V404 Cygni se formó con un impulso inicial mínimo del agujero negro, del orden de menos de 5 km/s. También se encontró que el componente terciario había evolucionado, lo que indica que el sistema triple se ha mantenido delimitado durante la formación del agujero negro y que la edad del sistema está restringida a entre 3 y 5 mil millones de años.

Estallido de 2015

Curva de luz en banda visual para V404 Cygni. El gráfico principal muestra las grandes variaciones durante el estallido de 2015, y el recuadro muestra las variaciones en escalas de tiempo cortas. Adaptado de Rodríguez et al. (2015) [ 20 ] y Martí et al. (2016) [ 21 ].

El 15 de junio de 2015, el satélite Swift de la NASA detectó los primeros indicios de actividad renovada. Se inició una campaña de observación mundial y el 17 de junio el observatorio de rayos gamma INTEGRAL de la ESA comenzó a monitorizar el estallido. INTEGRAL detectaba "destellos brillantes y repetidos de luz con una duración inferior a una hora, algo poco frecuente en otros sistemas de agujeros negros", y durante estos destellos, V404 Cygni era el objeto más brillante en el cielo de rayos X , hasta cincuenta veces más brillante que la Nebulosa del Cangrejo . Este estallido fue el primero desde 1989.

Other outbursts occurred in 1938 and 1956, and the outbursts were probably caused by material piling up in a disk around the black hole until a tipping point was reached.[22] The outburst was unusual in that physical processes in the inner accretion disk were detectable in optical photometry from small telescopes; previously, these variations were thought to be only detectable with space-based X-ray telescopes.[11] A detailed analysis of the INTEGRAL data revealed the existence of so-called pair plasma near the black hole. This plasma consists of electrons and their antimatter counterparts, positrons.[23]

A follow-up study of the 2015 data found a coronal magnetic field strength of 461±12 gauss, "substantially lower than previous estimates for such systems".[24]

See also

References

  1. 12345Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875.Gaia DR3 record for this source at VizieR.
  2. ↑Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  3. ↑Khargharia, Juthika; Froning, Cynthia S.; Robinson, Edward L. (2010). "Near-infrared Spectroscopy of Low-mass X-ray Binaries: Accretion Disk Contamination and Compact Object Mass Determination in V404 Cyg and Cen X-4". The Astrophysical Journal. 716 (2): 1105. arXiv:1004.5358. Bibcode:2010ApJ...716.1105K. doi:10.1088/0004-637X/716/2/1105. S2CID 119116307.
  4. 12Liu, Q. Z.; Van Paradijs, J.; Van Den Heuvel, E. P. J. (2007). "A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)". Astronomy and Astrophysics. 469 (2): 807. arXiv:0707.0544. Bibcode:2007A&A...469..807L. doi:10.1051/0004-6361:20077303. S2CID 14673570.
  5. ↑Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. 12Bernardini, F.; Russell, D. M.; Shaw, A. W.; Lewis, F.; Charles, P. A.; Koljonen, K. I. I.; Lasota, J. P.; Casares, J. (2016). "Events leading up to the 2015 June Outburst of V404 Cyg". The Astrophysical Journal Letters. 818 (1): L5. arXiv:1601.04550. Bibcode:2016ApJ...818L...5B. doi:10.3847/2041-8205/818/1/L5. S2CID 119251825.
  7. 1234Shahbaz, T.; Ringwald, F. A.; Bunn, J. C.; Naylor, T.; Charles, P. A.; Casares, J. (1994). "The mass of the black hole in V404 Cygni". Monthly Notices of the Royal Astronomical Society. 271: L10–L14. Bibcode:1994MNRAS.271L..10S. doi:10.1093/mnras/271.1.L10.
  8. 1234González Hernández, Jonay I.; Casares, Jorge; Rebolo, Rafael; Israelian, Garik; Filippenko, Alexei V.; Chornock, Ryan (2011). "Chemical Abundances of the Secondary Star in the Black Hole X-Ray Binary V404 Cygni". The Astrophysical Journal. 738 (1): 95. arXiv:1106.4278. Bibcode:2011ApJ...738...95G. doi:10.1088/0004-637X/738/1/95. S2CID 118443418.
  9. 123456Burdge, Kevin B.; El-Badry, Kareem; Kara, Erin; Canizares, Claude; Chakrabarty, Deepto; Frebel, Anna; Millholland, Sarah C.; Rappaport, Saul; Simcoe, Rob; Vanderburg, Andrew (2024). "The black hole low mass X-ray binary V404 Cygni is part of a wide hierarchical triple, and formed without a kick". arXiv:2404.03719 [astro-ph.HE].
  10. ↑Burdge, Kevin B.; El-Badry, Kareem; Kara, Erin; Canizares, Claude; Chakrabarty, Deepto; Frebel, Anna; Millholland, Sarah C.; Rappaport, Saul; Simcoe, Rob; Vanderburg, Andrew (2024-10-23). "The black hole low-mass X-ray binary V404 Cygni is part of a wide triple". Nature. 635 (8038): 316–320. arXiv:2404.03719. Bibcode:2024Natur.635..316B. doi:10.1038/s41586-024-08120-6. ISSN 1476-4687. PMID 39443805.
  11. 12Kimura, Mariko; et al. (7 January 2016). "Repetitive patterns in rapid optical variations in the nearby black-hole binary V404 Cygni". Nature. 529 (7584): 54–70. arXiv:1607.06195. Bibcode:2016Natur.529...54K. doi:10.1038/nature16452. PMID 26738590. S2CID 4463697.
  12. ↑Brecher, K. (1993-05-01). "Gray Holes". American Astronomical Society Meeting Abstracts #182. 182: 55.07. Bibcode:1993AAS...182.5507B.
  13. ↑Duerbeck, Hilmar W (1987). "A reference catalogue and atlas of galactic novae". Space Science Reviews. 45 (1–2): 1. Bibcode:1987SSRv...45....1D. doi:10.1007/BF00187826. S2CID 115854775.
  14. ↑Kitamoto, Shunji; Tsunemi, Hiroshi; Miyamoto, Sigenori; Yamashita, Koujun; Mizobuchi, Seiko; Nakagawa, Michio; Dotani, Tadayasu; Makino, Fumiaki (1989). "GS2023 + 338 - A new class of X-ray transient source?". Nature. 342 (6249): 518. Bibcode:1989Natur.342..518K. doi:10.1038/342518a0. S2CID 4308343.
  15. ↑Hurst, G. M (1989). "Nova Cygni 1938 Reappears - V404-CYGNI". Journal of the British Astronomical Society. 99: 161. Bibcode:1989JBAA...99..161H.
  16. ↑R. M. Wagner; S. Starrfield; A. Cassatella; R. Gonzalez-Riestra; T. J. Kreidl; S. B. Howell; R. M. Hjellming; X.-H. Han; G. Sonneborn (24 July 2005). "The 1989 outburst of V404 cygni: A very unusual x-ray nova". In A. Cassatella; R. Viotti (eds.). Physics of Classical Novae. Lecture Notes in Physics. Vol. 369. pp. 429–430. Bibcode:1990LNP...369..429W. doi:10.1007/3-540-53500-4_162. ISBN 978-3-540-53500-3. OSTI 7148923. S2CID 118834556.
  17. ↑Richter, Gerold A (1989). "V404 Cyg - a Further Outburst in 1956". Information Bulletin on Variable Stars. 3362: 1. Bibcode:1989IBVS.3362....1R.
  18. ↑Miller-Jones, J. C. A.; Jonker, P. G.; Dhawan, V.; Brisken, W.; Rupen, M. P.; Nelemans, G.; Gallo, E. (2009). "The First Accurate Parallax Distance to a Black Hole". The Astrophysical Journal. 706 (2): L230–L234. arXiv:0910.5253. Bibcode:2009ApJ...706L.230M. doi:10.1088/0004-637X/706/2/L230.
  19. ↑"This Black Hole's Jets Wobble Like Crazy Because It's Warping Space-Time". Space.com. 29 April 2019.
  20. ↑Rodriguez, J.; Cadolle Bel, M.; Alfonso-Garzón, J.; Siegert, T.; Zhang, X. L.; Grinberg, V.; Savchenko, V.; Tomsick, J. A.; Chenevez, J.; Clavel, M.; Diehl, R.; Domingo, A.; Gouiffès, C.; Greiner, J.; Krause, M. G. H.; Laurent, P.; Loh, A.; Markoff, S.; Mas-Hesse, J. M.; Miller-Jones, J. C. A.; Russell, D. M.; Wilms, J. (September 2015). "Correlated optical, X-ray, and γ-ray flaring activity seen with INTEGRAL during the 2015 outburst of V404 Cygni". Astronomy & Astrophysics. 581: L9. arXiv:1507.06659. Bibcode:2015A&A...581L...9R. doi:10.1051/0004-6361/201527043. S2CID 118579680.
  21. ↑Martí, Josep; Luque-Escamilla, Pedro L.; García-Hernández, María T. (February 2016). "Multi-colour optical photometry of V404 Cygni in outburst (Research Note)". Astronomy & Astrophysics. 586. arXiv:1601.01941. Bibcode:2016A&A...586A..58M. doi:10.1051/0004-6361/201527239. S2CID 119286126.
  22. ↑"Monster Black Hole Wakes Up After 26 Years". ESA. 25 June 2015. Archived from the original on 26 June 2015. Retrieved 26 June 2015.
  23. ↑"Gamma rays reveal pair plasma from a flaring black hole binary system". Max Planck Institute for Astrophysics. 29 February 2016.
  24. ↑Yigit Dallilar; et al. (8 Dec 2017). "A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni". Science. 358 (6368): 1299–1302. Bibcode:2017Sci...358.1299D. doi:10.1126/science.aan0249. PMID 29217570.