Astronomy:LMC X-1
250px Hubble image of LMC X-1 (right side: star in the red circle) and NGC 2079 (nebula on the left) | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[3] mas/yr Dec.: 0.622 ± 0.023[3] mas/yr |
| Distance | 180,000 ly (55,000 pc) |
| Orbit[4] | |
| Primary | giant star |
| Companion | black 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 | |
| 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 an instrument carried by a Sandia Terrier-Sandhawk sounding rocket, launched from the Johnston Atoll on October 29, 1968.[5][6] 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.[7][8] The orbital period later turned out to be shorter at around 3.9 days.[9] 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
- M33 X-7 is a stellar mass black hole in the Triangulum Galaxy
- Cyg X-1 another x-ray binary with a stellar black hole and a massive star
- Gaia BH1 first dormant black hole
References
- ↑ 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. doi:10.1086/423910. ISSN 0004-6256. Bibcode: 2004AJ....128.1606Z. https://ui.adsabs.harvard.edu/abs/2004AJ....128.1606Z.
- ↑ 2.0 2.1 2.2 2.3 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. doi:10.1088/1538-3873/aa7407. ISSN 0004-6280. Bibcode: 2017PASP..129i4201H. https://ui.adsabs.harvard.edu/abs/2017PASP..129i4201H.
- ↑ 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.
- ↑ 4.0 4.1 4.2 4.3 4.4 Orosz, Jerome A.; Steeghs, Danny; McClintock, Jeffrey E.; Torres, Manuel A. P.; Bochkov, Ivan; Gou, Lijun; Narayan, Ramesh; Blaschak, Michael et al. (2009-05-04). "A NEW DYNAMICAL MODEL FOR THE BLACK HOLE BINARY LMC X-1*" (in en). The Astrophysical Journal 697 (1): 573–591. doi:10.1088/0004-637X/697/1/573. ISSN 0004-637X. Bibcode: 2009ApJ...697..573O. https://dx.doi.org/10.1088/0004-637X/697/1/573.
- ↑ 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. Bibcode: 1969ApJ...155L.143M. https://ui.adsabs.harvard.edu/abs/1969ApJ...155L.143M.
- ↑ "Johnston Island". https://ccspacemuseum.org/sites/johnston-island/.
- ↑ 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. Bibcode: 1983ApJ...275L..43H. https://ui.adsabs.harvard.edu/abs/1983ApJ...275L..43H.
- ↑ 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. Bibcode: 1987AJ.....94..340H. https://ui.adsabs.harvard.edu/abs/1987AJ.....94..340H.
- ↑ 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. https://www.astronomerstelegram.org/?read=940. Retrieved 2024-05-04.
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