Astronomy:VFTS 243

From HandWiki
Short description: Spectroscopic binary in the constellation Dorado
VFTS 243
280px
VFTS 243 in Hubble Space Telescope colours
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Dorado
Right ascension  05h 38m 08.407s[1]
Declination −69° 09′ 18.98″[1]
Apparent magnitude (V) 15.26[2]
Characteristics
Evolutionary stage main sequence + black hole
Spectral type O7V(n)((f))[3]
Variable type variable[4]
Astrometry
Proper motion (μ) RA: +1.722[1] mas/yr
Dec.: +0.603[1] mas/yr
Parallax (π)−0.0468 ± 0.0244[1] mas
Orbit[4]
Period (P)10.4031 days
Eccentricity (e)0.017
Inclination (i)≥ 40°
Semi-amplitude (K1)
(primary)		81.4 km/s
Details[4]
star
Mass25 ± 2.3 M☉
Radius10.3 ± 0.3 R☉
Luminosity158000+14000
−15000 L☉
Surface gravity (log g)3.7 ± 0.1 cgs
Temperature36,000 ± 1000 K
Rotational velocity (v sin i)181 ± 16 km/s
Age7.4 Myr
black hole
Mass10.1 ± 2.0 M☉
Other designations
2MASS J05380840-6909190[5]
Database references
SIMBADdata

VFTS 243 (2MASS J05380840-6909190) is an O7V type main sequence star that orbits a stellar mass black hole.[6] The black hole is around nine times the mass of the Sun, with the blue star being 25 times the mass of the Sun making the star 200,000 times larger than the black hole. VFTS 243 is located in the Large Magellanic Cloud inside NGC 2070 (the Tarantula Nebula) around 160,000 light years from Earth.[7][5] The binary has an orbital period of 10.4 days.[4]

Physical properties

VTFS 253 is composed of a rapidly rotating O-type main sequence star and a black hole orbiting each other in a tight, circular orbit every 10.4 days. The system is the only known OB star-black hole binary outside the Milky Way that is 'quiet' in X-ray, with quiet referring to a lack of emissions. [4]

The primary star is roughly 25 solar mass and 10 solar radii. It has filled to roughly a third of its roche lobe is slightly ellipsoidal. It is rapidly rotating with a projected rotational velocity of 181 km/s, implying it had been spun up by accreting matter from the progenitor of the black hole. [4]

The black hole is roughly 10 solar mass and is quiet in X-ray, implying it is not accreting matter from an accretion disk. [4]

Evolution

Models suggests the system initially formed as a tight massive binary with an orbital period close to 4 days with two stars roughly 30 and 20 solar masses respectively. As the initially more massive star evolved and expanded, it transferred its outer envelope to the secondary star, rejuvenating it in the process. The primary eventually evolved into a Wolf-Rayet star before collapsing into a black hole. Based on the low eccentricity of the orbits, less than 0.5 solar mass was lost during the collapse of the progenitor into the black hole. [4]

Based on evolutionary models, as the now O-type star evolves, it would begin transferring mass back to the less massive black hole, shrinking their orbit in the process. The system is likely to end as a pair of black holes orbiting each other every few days, and would eventually merge to form a single black hole after several tens or hundreds of billions of years. [4]

Artist's impression of VFTS 243[8]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ Evans, C. J.; Taylor, W. D.; Hénault-Brunet, V.; Sana, H.; De Koter, A. et al. (June 2011). "The VLT-FLAMES Tarantula Survey. I. Introduction and observational overview". Astronomy & Astrophysics 530: A108. doi:10.1051/0004-6361/201116782. Bibcode: 2011A&A...530A.108E. 
  3. ↑ Walborn, N. R.; Sana, H.; Simón-Díaz, S.; Maíz Apellániz, J.; Taylor, W. D.; Evans, C. J.; Markova, N.; Lennon, D. J. et al. (2014). "The VLT-FLAMES Tarantula Survey. XIV. The O-type stellar content of 30 Doradus". Astronomy and Astrophysics 564: A40. doi:10.1051/0004-6361/201323082. Bibcode: 2014A&A...564A..40W. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 Shenar, Tomer; Sana, Hugues; Mahy, Laurent; El-Badry, Kareem; Marchant, Pablo; Langer, Norbert; Hawcroft, Calum; Fabry, Matthias et al. (2022-07-18). "An X-ray-quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud" (in en). Nature Astronomy 6 (9): 1085–1092. doi:10.1038/s41550-022-01730-y. ISSN 2397-3366. Bibcode: 2022NatAs...6.1085S. 
  5. ↑ 5.0 5.1 "VFTS 243". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=VFTS+243. 
  6. ↑ Stevance, H. F.; Ghodla, S.; Richards, S.; Eldridge, J. J.; Briel, M. M.; Tang, P. (2023). "VFTS 243 as predicted by the BPASS fiducial models". Monthly Notices of the Royal Astronomical Society 520 (3): 4740–4746. doi:10.1093/mnras/stad362. 
  7. ↑ Katie Hunt (18 July 2022). "'Black hole police' discover dormant black hole outside our galaxy for first time". https://www.cnn.com/2022/07/18/world/dormant-black-hole-discovered-scn/index.html. 
  8. ↑ "'Black hole police' discover a dormant black hole outside our galaxy". European Southern Observatory. 18 July 2022. https://www.eso.org/public/news/eso2210/. 

Template:Large Magellanic Cloud



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:VFTS_243&oldid=4625403"