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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The Large Magellanic Cloud (LMC) is a dwarf irregular galaxy, and satellite galaxy of the Milky Way. At a distance of around 50 kiloparsecs (163,000 light-years), the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (c. 16 kiloparsecs (52,000 light-years) away) and the possible dwarf irregular galaxy called the Canis Major Overdensity. Based on the D25 isophote at the B-band (445 nm wavelength of light), the Large Magellanic Cloud is about 9.86 kiloparsecs (32,200 light-years) across. It is roughly one-hundredth the mass of the Milky Way and is the fourth-largest galaxy in the Local Group, after the Andromeda Galaxy (M31), the Milky Way, and the Triangulum Galaxy (M33).

<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.

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NGC 300 (also known as Caldwell 70) is a spiral galaxy in the constellation Sculptor. It is one of the closest galaxies to the Local Group, and probably lies between the latter and the Sculptor Group. It is the brightest of the five main spirals in the direction of the Sculptor Group. It is inclined at an angle of 42° when viewed from Earth and shares many characteristics of the Triangulum Galaxy. It is 94,000 light-years in diameter, somewhat smaller than the Milky Way, and has an estimated mass of (2.9 ± 0.2) × 1010M☉.

<span class="mw-page-title-main">47 Tucanae</span> Globular cluster in the constellation Tucana

47 Tucanae or 47 Tuc is a globular cluster located in the constellation Tucana. It is about 4.45 ± 0.01 kpc (15,000 ± 33 ly) from Earth, and 120 light years in diameter. 47 Tuc can be seen with the naked eye, with an apparent magnitude of 4.1. It appears about 44 arcminutes across including its far outreaches. Due to its far southern location, 18° from the south celestial pole, it was not catalogued by European astronomers until the 1750s, when the cluster was first identified by Nicolas-Louis de Lacaille from South Africa.

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

NGC 1850 is a double cluster and a super star cluster in the Dorado constellation, located in the northwest part of the bar of the Large Magellanic Cloud, at a distance of 168 kly (51.5 kpc) from the Sun. It was discovered by Scottish astronomer James Dunlop in 1826.

<span class="mw-page-title-main">WR 136</span> Star in the constellation of Cygnus

WR 136 is a Wolf–Rayet star located in the constellation Cygnus. It is in the center of the Crescent Nebula. Its age is estimated to be around 4.7 million years and it is nearing the end of its life. Within a few hundred thousand years, it is expected to explode as a supernova.

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

NGC 1023 is a barred lenticular galaxy, a member of the NGC 1023 group of galaxies in the Local Supercluster. Distance measurements vary from 9.3 to 19.7 million parsecs (30 to 64 million light-years). The supermassive black hole at the core has a mass of (4.4±0.5)×107 M☉. The black hole was discovered by analyzing the dynamics of the galaxy.

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

R136a1 is one of the most massive and luminous stars known, at nearly 200 M☉ and nearly 4.7 million L☉, and is also one of the hottest, at around 46,000 K. It is a Wolf–Rayet star at the center of R136, the central concentration of stars of the large NGC 2070 open cluster in the Tarantula Nebula in the Large Magellanic Cloud. The cluster can be seen in the far southern celestial hemisphere with binoculars or a small telescope, at magnitude 7.25. R136a1 itself is 100 times fainter than the cluster and can only be resolved using speckle interferometry.

<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.

<span class="mw-page-title-main">R136a2</span> Star in the constellation Dorado

R136a2 is a Wolf-Rayet star residing near the center of the R136, the central concentration of stars of the large NGC 2070 open cluster in the Tarantula Nebula, a massive H II region in the Large Magellanic Cloud which is a nearby satellite galaxy of the Milky Way. It has one of the highest confirmed masses and luminosities of any known star, at about 151 M☉ and 3.5 million L☉ respectively.

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

<span class="mw-page-title-main">NGC 5204</span> Galaxy in the constellation Ursa Major

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.

BAT99-98 is a Wolf-Rayet star in the Large Magellanic Cloud. It is located near the R136 cluster in the 30 Doradus nebula. At 226 M☉ and 5,000,000 L☉ it is currently one of the most massive and luminous stars known.

<span class="mw-page-title-main">NGC 4203</span> Galaxy in the constellation Coma Berenices

NGC 4203 is the New General Catalogue identifier for a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 20, 1787 by English astronomer William Herschel, and is situated 5.5° to the northwest of the 4th magnitude star Gamma Comae Berenices and can be viewed with a small telescope. The morphological classification of NGC 4203 is SAB0−, indicating that it has a lenticular form with tightly wound spiral arms and a weak bar structure at the nucleus.

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

UY Volantis, also known as EXO 0748-676, is a low mass X-ray binary system located in the constellation Volans. With an apparent magnitude of 16.9, it requires a powerful telescope to see. With a radial velocity of 20 km/s, it is drifting away from the Solar System, and is currently located 26,000 light years away.

<span class="mw-page-title-main">Henize 70</span> H II region in the Large Magellanic Cloud

Henize 70 (N70) is a faint emission nebula and superbubble located in the Large Magellanic Cloud. It is located in the constellation of Dorado.

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: 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: 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. 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. 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. 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. 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. Bibcode:2006ATel..940....1L . Retrieved 2024-05-04.
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