LMC X-1

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LMC X-1
NGC 2079 and LMC X-1 HST.jpg
Hubble image of LMC X-1 (right side: star in the red circle) and NGC 2079 (nebula on the left)
Observation data
Epoch J2000       Equinox J2000
Constellation Dorado
Right ascension 05h 39m 38.8284s
Declination −69° 44′ 35.5315″
Apparent magnitude  (V)14.612 ± 0.171 [1]
Characteristics
Evolutionary stage X-ray binary
Spectral type O8 IIIf or O8 f?p [2]
Astrometry
Radial velocity (Rv)309.12 ± 0.333 [2]  km/s
Proper motion (μ)RA: 1.889 ± 0.020  mas/yr [3]
Dec.: 0.622 ± 0.023  mas/yr [3]
Distance 180,000  ly
(55,000  pc) [2]
Orbit [4]
Primarygiant star
Companionblack hole
Period (P)3.90917 ± 0.00005 days
Semi-major axis (a)36.49 ± 1.51 R☉
Eccentricity (e)<0.0256 ± 0.0066
Inclination (i)36.38 ± 2.02°
Semi-amplitude (K2)
(secondary)		71.61 ± 1.10 km/s
Details [4]
star
Mass 31.79 ± 3.48   M☉
Radius 17.0 ± 0.8  R☉
Surface gravity (log g)3.485 ± 0.018  cgs
Temperature 33,000 to 35,000 [2]   K
Rotational velocity (v sin i)129.9 ± 2.2 km/s
Age 5  Myr
black hole
Mass 10.91 ± 1.41  M☉
Other designations
2MASS  J05393883-6944356, 2E  1522, 1RXS  J053938.8-694515
Database references
SIMBAD data

LMC X-1 is the first X-ray source detected in the Large Magellanic Cloud. [4] It was discovered in 1969, using data from a sounding rocket, launched from the Johnston Atoll on October 29, 1968. [5] LMC X-1 is a persistently luminous X-ray binary. [4]

In the 80s Hutchings et al. performed spectroscopic follow-up observations of the optical counterpart and found an orbital period of about 4 days and a secondary mass of about 6 M☉, making the secondary a stellar mass black hole. [6] [7] The orbital period later turned out to be shorter at around 3.9 days. [8] The optical counterpart is also called "star 32". The black hole has a mass of around 11 M☉ and the star has a mass of around 32 M☉ and a radius of 17 R☉. With this radius the star nearly fills its Roche lobe and it is predicted that it will encounter its Roche lobe in a few hundred thousand years. Once it reaches its Roche lobe, it will begin rapid and possibly unstable mass transfer to its companion. [4]

The X-ray source is surrounded by a nebula, which is the only nebula energized by an X-ray binary. It is suspected that the nebula is a bow shock nebula. The nebula is also detected in radio wavelengths with ATCA imaging. A possible origin of LMC X-1 is the star cluster [NKN2005] N159-O1. Other possible origins are NGC 2077, NGC 2080, NGC 2085 and NGC 2086. In the scenario of N159-O1 being the origin, the progenitor to the black hole would have a mass of about 60 M☉, meaning it was the most massive member of this star cluster. [2]

See also

Related Research Articles

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<span class="mw-page-title-main">NGC 2346</span> Planetary nebula in the constellation Monoceros

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<span class="mw-page-title-main">Tarantula Nebula</span> H II region in the constellation Dorado

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<span class="mw-page-title-main">Stellar black hole</span> Black hole formed by a collapsed star

A stellar black hole is a black hole formed by the gravitational collapse of a star. They have masses ranging from about 5 to several tens of solar masses. They are the remnants of supernova explosions, which may be observed as a type of gamma ray burst. These black holes are also referred to as collapsars.

<span class="mw-page-title-main">NGC 300</span> Galaxy in the constellation Sculptor

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<span class="mw-page-title-main">S Doradus</span> Star in the Large Magellanic Cloud

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<span class="mw-page-title-main">NGC 1850</span> Super star cluster in the constellation Dorado

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<span class="mw-page-title-main">Ultraluminous X-ray source</span>

An ultraluminous X-ray source (ULX) is an astronomical source of X-rays that is less luminous than an active galactic nucleus but is more consistently luminous than any known stellar process (over 1039 erg/s, or 1032 watts), assuming that it radiates isotropically (the same in all directions). Typically there is about one ULX per galaxy in galaxies which host them, but some galaxies contain many. The Milky Way has not been shown to contain a ULX, although SS 433 may be a possible source. The main interest in ULXs stems from their luminosity exceeding the Eddington luminosity of neutron stars and even stellar black holes. It is not known what powers ULXs; models include beamed emission of stellar mass objects, accreting intermediate-mass black holes, and super-Eddington emission.

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<span class="mw-page-title-main">NGC 1023</span> Galaxy in the constellation Perseus

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<span class="mw-page-title-main">R136a1</span> Wolf–Rayet star with one of the highest mass and luminosity of any known star

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<span class="mw-page-title-main">AB7</span> Binary star in the Small Magellanic Cloud in the constellation Tucana

AB7, also known as SMC WR7, is a binary star in the Small Magellanic Cloud. A Wolf–Rayet star and a supergiant companion of spectral type O orbit in a period of 19.56 days. The system is surrounded by a ring-shaped nebula known as a bubble nebula.

HD 38282 is a massive spectroscopic binary star in the Tarantula Nebula, consisting of two hydrogen-rich Wolf-Rayet stars.

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NCG 5204 is a Magellanic spiral galaxy located about 14.5 million light-years away from Earth in the constellation of Ursa Major and is a member of the M101 Group of galaxies. It has a galaxy morphological classification of SA(s)m and is highly irregular, with only the barest indication of any spiral arm structure. The galaxy's most prominent feature is an extremely powerful X-ray source designated NGC 5204 X-1. This has resulted in the galaxy being the target of several studies due to the strength of the source and its relative proximity to Earth.

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<span class="mw-page-title-main">NGC 6388</span> Globular cluster in the constellation Scorpius

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<span class="mw-page-title-main">UY Volantis</span> Low mass X-ray binary in the constellation Volans

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<span class="mw-page-title-main">VFTS 243</span>

VFTS 243 is an O7V type main sequence star that orbits a stellar mass black hole. 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 around 160,000 light years from Earth. The binary has an orbital period of 10.4 days.

References

  1. ↑ Zaritsky, Dennis; Harris, Jason; Thompson, Ian B.; Grebel, Eva K. (2004-10-01). "The Magellanic Clouds Photometric Survey: The Large Magellanic Cloud Stellar Catalog and Extinction Map". The Astronomical Journal. 128 (4): 1606–1614. arXiv: astro-ph/0407006 . Bibcode:2004AJ....128.1606Z. doi:10.1086/423910. ISSN   0004-6256.
  2. 1 2 3 4 5 Hyde, E. A.; Russell, D. M.; Ritter, A.; Filipović, M. D.; Kaper, L.; Grieve, K.; O'Brien, A. N. (2017-09-01). "LMC X-1: A New Spectral Analysis of the O-star in the Binary and Surrounding Nebula". Publications of the Astronomical Society of the Pacific. 129 (979): 094201. arXiv: 1706.01203 . Bibcode:2017PASP..129i4201H. doi:10.1088/1538-3873/aa7407. ISSN   0004-6280.
  3. 1 2 Vallenari, 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.
  4. 1 2 3 4 5 Orosz, Jerome A.; Steeghs, Danny; McClintock, Jeffrey E.; Torres, Manuel A. P.; Bochkov, Ivan; Gou, Lijun; Narayan, Ramesh; Blaschak, Michael; Levine, Alan M.; Remillard, Ronald A.; Bailyn, Charles D.; Dwyer, Morgan M.; Buxton, Michelle (2009-05-04). "A NEW DYNAMICAL MODEL FOR THE BLACK HOLE BINARY LMC X-1*". The Astrophysical Journal. 697 (1): 573–591. arXiv: 0810.3447 . Bibcode:2009ApJ...697..573O. doi:10.1088/0004-637X/697/1/573. ISSN   0004-637X.
  5. ↑ Mark, Hans; Price, R.; Rodrigues, R.; Seward, F. D.; Swift, C. D. (1969-03-01). "Detection of X-Rays from the Large Magellanic Cloud". The Astrophysical Journal. 155: L143. Bibcode:1969ApJ...155L.143M. doi:10.1086/180322. ISSN   0004-637X.
  6. ↑ Hutchings, J. B.; Crampton, D.; Cowley, A. P. (1983-12-01). "A spectrographic orbit for LMC X-1 : another massive X-ray source ?". The Astrophysical Journal. 275: L43–L47. Bibcode:1983ApJ...275L..43H. doi:10.1086/184168. ISSN   0004-637X.
  7. ↑ Hutchings, J. B.; Crampton, D.; Cowley, A. P.; Bianchi, L.; Thompson, I. B. (1987-08-01). "Optical and UV Spectroscopy of the Black Hole Binary Candidate LMC X-1". The Astronomical Journal. 94: 340. Bibcode:1987AJ.....94..340H. doi:10.1086/114475. ISSN   0004-6256.
  8. ↑ Levine, Alan M.; Corbet, Robin (9 Nov 2006). "ATel #940: Detection of Additional Periodicities in RXTE ASM Light Curves". The Astronomer's Telegram. 940: 1. Bibcode:2006ATel..940....1L . Retrieved 2024-05-04.
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