A0620-00

Last updated

A0620-00
V616MonLightCurve.png
A visual band light curve for V616 Monocerotis, adapted from van Grunsven et al. (2017) [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Monoceros
Right ascension 06h 22m 44.542s [2]
Declination −00° 20′ 44.29″ [2]
Apparent magnitude  (V)11.2 [3]
Characteristics
Evolutionary stage Black hole + main sequence [4]
Spectral type K2 V [5]
Variable type X-ray nova, Ellipsoidal [6]
Astrometry
Radial velocity (Rv)−5±12 [7]  km/s
Proper motion (μ)RA: −0.439  mas/yr [2]
Dec.: −5.138  mas/yr [2]
Parallax (π)0.6969 ± 0.1168  mas [2]
Distance approx. 4,700  ly
(approx. 1,400  pc)
Orbit
Period (P)7.75234 ± 0.00010 [7] hr
Inclination (i)50.98 ± 0.87 [4] °
Periastron epoch (T)JD 2446082.7481 ± 0.0008 [7]
Semi-amplitude (K1)
(primary)		457 ± 8 [7] km/s
Details
Black hole
Mass 5.86±1.24 [8]   M☉
Star
Mass 0.34±0.03 [8]   M☉
Radius 1.057 [9]   R☉
Luminosity0.44 [9]   L☉
Surface gravity (log g)5.0 [5]   cgs
Temperature 5,000 [5]   K
Metallicity [Fe/H]0.0 [5]   dex
Rotational velocity (v sin i)83.8±1.9 [5]  km/s
Other designations
1A  0620-00, INTREF  297, Nova Mon 1917, Nova Mon 1975, Mon X-1, V616 Mon [3]
Database references
SIMBAD data

A0620-00 (abbreviated from 1A 0620-00) is a binary star system in the constellation of Monoceros, with an apparent magnitude of 11.2

Contents

A0620-00 consists of two objects. The first object is a K-type main-sequence star. [4] [5] The second object cannot be seen, but based on its calculated mass of about 6 M☉, [8] [4] it is too massive to be a neutron star and must therefore be a stellar-mass black hole. [7] The two objects orbit each other every 7.75 hours. [7] At a distance of roughly 3,300 light-years (1,000 parsecs ) away, the black hole of A0620-00 would be one of the nearest known black holes to the Solar System, closer than GRO J1655-40. [10]

This image of A0620-00 was created from Sloan Digital Sky Survey data in visible and infrared light (filters u,g,i,z) and spans roughly 8 arcminutes. V616mon sdss ugiz 1 besk.jpg
This image of A0620-00 was created from Sloan Digital Sky Survey data in visible and infrared light (filters u,g,i,z) and spans roughly 8 arcminutes.

A0620-00 has undergone two X-ray outbreaks. The first one was in 1917. [11] The second burst, in 1975, was detected by the Ariel 5 satellite. [12] During that time, A0620-00 was the brightest X-ray point source. [7] It is now classified as an X-ray nova. [7] Its black hole nature was determined in 1986. [7]

The black hole in A0620-00 pulls matter from the K-type star into an accretion disk. [4] The accretion disk emits significant amounts of visible light and X-rays. Because the K-type star has been pulled into an ellipsoidal shape, the amount of surface area visible, and thus the apparent brightness, changes from the Earth's perspective. A0620-00 also bears the variable star designation V616 Monocerotis. [6]

Stephen Hawking memorial broadcast

On 15 June 2018, a signal was transmitted from the European Space Agency big radio antenna at Cebreros Station (77 kilometers west of Madrid, Spain), in memory of Stephen Hawking, who died on 14 March 2018, and his work on the physics of black holes. The broadcast will travel the 3,457-light-year distance at the speed of light and will arrive in the year 5475; this will be the first-ever human interaction with a currently known black hole. [13] 1A 0620-00 was chosen for this broadcast as it was the closest known black hole to Earth at the time. [14] The message was one of peace and hope according to his family.

Related Research Articles

<span class="mw-page-title-main">Cygnus X-1</span> Galactic X-ray source in the constellation Cygnus that is very likely a black hole

Cygnus X-1 (abbreviated Cyg X-1) is a galactic X-ray source in the constellation Cygnus and was the first such source widely accepted to be a black hole. It was discovered in 1965 during a rocket flight and is one of the strongest X-ray sources detectable from Earth, producing a peak X-ray flux density of 2.3×10−23 W/(m2⋅Hz) (2.3×103 jansky). It remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 21.2 times the mass of the Sun and has been shown to be too small to be any known kind of normal star or other likely object besides a black hole. If so, the radius of its event horizon has 300 km "as upper bound to the linear dimension of the source region" of occasional X-ray bursts lasting only for about 1 ms.

<span class="mw-page-title-main">26 Andromedae</span> Star in the constellation Andromeda

26 Andromedae, abbreviated 26 And, is a binary star system in the constellation Andromeda. 26 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 6.10, which is near the lower limit of visibility to the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.35 mas, which yields a distance of about 600 light years. At that distance, the visual magnitude of the stars is diminished from an extinction of 0.04 due to interstellar dust. The system is moving further from the Earth with a heliocentric radial velocity of +3.3 km/s.

<span class="mw-page-title-main">NGC 514</span> Spiral galaxy in the constellation Pisces

NGC 514 is a low-luminosity, intermediate spiral galaxy in the equatorial constellation of Pisces, located at a distance of approximately 83 million light-years from the Milky Way. It was discovered on 16 October 1784 by astronomer William Herschel. The general form of the galaxy is specified by its morphological classification of SAB(rs)c, which indicates it has a weak bar system at the core (SAB), an incomplete ring formation around the bar (rs), and somewhat loosely-wound spiral arms (c). This galaxy has an H II nucleus with an extended region that displays weak emission lines in the optical range, but not in the near infrared. The suspected supermassive black hole at the core has an estimated mass of 3.2×106 M☉.

<span class="mw-page-title-main">NGC 4639</span> Galaxy in the constellation Virgo

NGC 4639 is a barred spiral galaxy located in the equatorial constellation of Virgo. It was discovered by German-born astronomer William Herschel on April 12, 1784. John L. E. Dreyer described it as "pretty bright, small, extended, mottled but not resolved, 12th magnitude star 1 arcmin to southeast". This is a relatively nearby galaxy, lying approximately 72 million light-years away from the Milky Way. It is a companion to NGC 4654, and the two appear to have interacted roughly 500 million years ago. NGC 4639 is a member of the Virgo Cluster.

<span class="mw-page-title-main">IC 2391</span> Open star cluster in the constellation Vela

IC 2391 is an open cluster in the constellation Vela consisting of hot, young, blueish stars, some of which binaries and one of which is a quadruple. Persian astronomer A. a.-R. al-Sufi first described it as "a nebulous star" in c. 964. It was re-found by Abbe Lacaille and cataloged as Lac II 5.

<span class="mw-page-title-main">4U 1700-37</span>

4U 1700-37 is one of the stronger binary X-ray sources in the sky, and is classified as a high-mass X-ray binary. It was discovered by the Uhuru satellite. The "4U" designation refers to the fourth Uhuru catalog.

<span class="mw-page-title-main">V4641 Sagittarii</span> Binary star in the constellation Sagittarius

V4641 Sagittarii is a variable X-ray binary star system in the constellation Sagittarius. It is the source of one of the fastest superluminal jets in the Milky Way galaxy.

<span class="mw-page-title-main">V404 Cygni</span> Star and black hole binary star system in the constellation Cygnus

V404 Cygni is a microquasar and a binary 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 with a mass slightly smaller than the Sun. The star and the black hole orbit each other every 6.47129 days at fairly close range. Due to their proximity and the intense gravity of the black hole, the companion star loses mass to an accretion disk around the black hole and ultimately to the black hole itself.

<span class="mw-page-title-main">HD 24479</span> Star in the constellation Camelopardalis

HD 24479, also designated as HR 1204, is a solitary, bluish-white hued star located in the northern circumpolar constellation Camelopardalis. The star is visible to the naked eye with an apparent visual magnitude of 5.04. Based on Gaia DR3 parallax measurements, it is located 385 light years from the Sun. However, it is receding with a somewhat constrained heliocentric radial velocity of 4.6 km/s. At its current distance, HD 24479's brightness is diminished by 0.29 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 168607</span> Star in the constellation Sagittarius

HD 168607 is a blue hypergiant and luminous blue variable (LBV) star located in the constellation of Sagittarius, easy to see with amateur telescopes. It forms a pair with HD 168625, also a blue hypergiant and possible luminous blue variable, that can be seen at the south-east of M17, the Omega Nebula.

23 Orionis is a double star located around 1,200 light-years away from the Sun in the equatorial constellation of Orion. It is visible to the naked eye as a dim, blue-white-hued point of light with a combined apparent visual magnitude of 4.99. The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, and they are members of the Orion OB1 association, subgroup 1a.

<span class="mw-page-title-main">NGC 266</span> Galaxy in the constellation Pisces

NGC 266 is a massive barred spiral galaxy in the constellation Pisces. NGC 266 is located at a distance of 197 megalight-years from the Milky Way. It was discovered on September 12, 1784, by William Herschel. The form of this barred galaxy is described by its morphological classification of SB(rs)ab, which indicates a quasi-ring-like structure (rs) and moderate-to-tightly wound spiral arms (ab). It is the dominant member of a small group with six low-mass galaxies.

BP Crucis is an X-ray binary system containing a blue hypergiant and a pulsar.

4U 1543-475 is a recurrent X-ray transient located in the southern constellation Lupus, the wolf. IL Lupi is its variable star designation. It has an apparent magnitude that fluctuates between 14.6 and 16.7, making it readily visible in large telescopes but not to the naked eye. The object is located relatively far at a distance of approximately 17,000 light years based on Gaia DR3 parallax measurements.

<span class="mw-page-title-main">BP Tauri</span> Star in the constellation Taurus

BP Tauri is a young T Tauri star in the constellation of Taurus about 416 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">V723 Monocerotis</span> Variable star

V723 Monocerotis is a variable star in the constellation Monoceros. It was proposed in 2021 to be a binary system including a lower mass gap black hole candidate nicknamed "The Unicorn". Located 1,500 light years from Earth, it would be the closest black hole to our planet, and among the smallest ever found.

<span class="mw-page-title-main">10 Trianguli</span> Star in the constellation Triangulum

10 Trianguli, or simply 10 Tri is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.29. Gaia DR3 parallax measurements imply a distance of 363 light-years and it is slowly receding with a heliocentric radial velocity of 0.4 km/s. At its current distance, 10 Tri's brightness is diminished by an interstellar extinction of 0.11 magnitudes and it has an absolute magnitude of −0.02.

<span class="mw-page-title-main">Gaia BH1</span> Binary system containing the closest black hole to Earth

Gaia BH1 is a binary system consisting of a G-type main-sequence star and a likely stellar-mass black hole, located about 1,560 light-years (478 pc) away from the Solar System in the constellation of Ophiuchus. As of 2022, it is the nearest known system that astronomers are reasonably confident contains a black hole, followed by Gaia BH2 and A0620-00.

<span class="mw-page-title-main">HD 10390</span> B-type main-sequence star; Triangulum

HD 10390 is a solitary star located in the northern constellation Triangulum. It is faintly visible to the naked eye as a bluish-white hued point of light with an apparent magnitude of 5.64. The object is located relatively close at a distance of 292 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −1.9 km/s. At its current distance, HD 10390's brightness is diminished by an interstellar extinction of only five-hundredths of a magnitude and it has an absolute magnitude of +1.00.

References

  1. ↑ van Grunsven, Theo F. J.; Jonker, Peter G.; Verbunt, Frank W. M.; Robinson, Edward L. (December 2017). "The mass of the black hole in 1A 0620–00, revisiting the ellipsoidal light curve modelling". Monthly Notices of the Royal Astronomical Society. 472 (2): 1907–1914. arXiv: 1708.08209 . Bibcode:2017MNRAS.472.1907V. doi:10.1093/mnras/stx2071 . Retrieved 29 January 2022.
  2. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. 1 2 "1A 0620-00". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 26 August 2017.
  4. 1 2 3 4 5 Cantrell, Andrew G.; Bailyn, Charles D.; Orosz, Jerome A.; McClintock, Jeffrey E.; Remillard, Ronald A.; Froning, Cynthia S.; Neilsen, Joseph; Gelino, Dawn M.; Gou, Lijun (2010). "The Inclination of the Soft X-Ray Transient A0620-00 and the Mass of its Black Hole". The Astrophysical Journal. 710 (2): 1127–1141. arXiv: 1001.0261 . Bibcode:2010ApJ...710.1127C. doi:10.1088/0004-637X/710/2/1127. S2CID   33906909.
  5. 1 2 3 4 5 6 Zheng, Wan-Min; Wu, Qiaoya; Wu, Jianfeng; Wang, Song; Sun, Mouyuan; Guo, Jing; Liu, Junhui; Yi, Tuan; Zhang, Zhi-Xiang; Gu, Wei-Min; Wang, Junfeng; Gou, Lijun; Liu, Jifeng; Callanan, Paul J.; Ho, Luis C.; Longa-Peña, Penélope; Orosz, Jerome A.; Reynolds, Mark T. (2022), "The Disk Veiling Effect of the Black Hole Low-mass X-Ray Binary A0620-00", The Astrophysical Journal, 925 (1): 83, arXiv: 2112.07842 , Bibcode:2022ApJ...925...83Z, doi: 10.3847/1538-4357/ac4332 , S2CID   245144462
  6. 1 2 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.
  7. 1 2 3 4 5 6 7 8 9 McClintock, J. E.; Remillard, R. A. (1986). "The black hole binary A0620-00". Astrophysical Journal. 308: 110–122. Bibcode:1986ApJ...308..110M. doi: 10.1086/164482 .
  8. 1 2 3 Van Grunsven, Theo F. J.; Jonker, Peter G.; Verbunt, Frank W. M.; Robinson, Edward L. (2017), "The mass of the black hole in 1A 0620-00, revisiting the ellipsoidal light curve modelling", Monthly Notices of the Royal Astronomical Society, 472 (2): 1907, arXiv: 1708.08209 , Bibcode:2017MNRAS.472.1907V, doi:10.1093/mnras/stx2071
  9. 1 2 Stassun, Keivan G.; et al. (1 October 2019), "The Revised TESS Input Catalog and Candidate Target List", The Astronomical Journal, 158 (4): 138, arXiv: 1905.10694 , Bibcode:2019AJ....158..138S, doi: 10.3847/1538-3881/ab3467 , hdl: 1721.1/124721 , ISSN   0004-6256, S2CID   166227927.
  10. ↑ Foellmi, Cédric (2009). "What is the closest black hole to the Sun?". New Astronomy. 14 (8): 674–691. arXiv: 0812.4232 . Bibcode:2009NewA...14..674F. doi:10.1016/j.newast.2009.04.003. S2CID   12843219.
  11. ↑ Eachus, L. J.; Wright, E. L.; Liller, W. (1976). "Optical observations of the recurrent nova associated with A0620-00 - 1917-1975". Astrophysical Journal. 203: L17–L19. Bibcode:1976ApJ...203L..17E. doi: 10.1086/182009 .
  12. ↑ Elvis, M.; Page, C. G.; Pounds, K. A.; Ricketts, M. J.; Turner, M. J. L. (1975). "Discovery of powerful transient X-ray source A0620-00 with Ariel V Sky Survey Experiment". Nature. 257 (5528): 656–657. Bibcode:1975Natur.257..656E. doi:10.1038/257656a0. S2CID   4160399.
  13. ↑ Ghosh, Pallab (15 June 2018). "Prof Hawking: A fitting way to go". BBC . Retrieved 20 July 2019.
  14. ↑ Kelly, Guy; Davies, Gareth (15 June 2018). "Stephen Hawking laid to rest between graves of Sir Isaac Newton and Charles Darwin". The Telegraph. ISSN   0307-1235 . Retrieved 16 June 2018.
Records
Preceded by Least distant black hole
1986—2022		Succeeded by
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.