Categories
BO Carinae
Topic: Astronomy
From HandWiki - Reading time: 6 min
280px BO Carinae is the brightest red star, towards upper left, in this image of the Carina Nebula. Credit: ESO | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 46m 00.53s |
| Declination | 59° 29′ 19.5″ |
| Apparent magnitude (V) | 7.18 - 8.50[1] |
| Characteristics | |
| Spectral type | M4 Ib[1] |
| Variable type | Lc[1] |
| Astrometry | |
| Proper motion (μ) | RA: −7.334±0.027[2] mas/yr Dec.: −1.420±0.028[2] mas/yr |
| Parallax (π) | 0.6020 ± 0.0259[2] mas |
| Distance | 5,400 ± 200 ly (1,660 ± 70 pc) |
| Details | |
| Radius | 790[3] R☉ |
| Luminosity | 78,000[3] L☉ |
| Temperature | 3,525[3] K |
| Other designations | |
BO Car, IDS 10419−5858, IRAS 10438−5913, 2MASS J10455065−5929193, AAVSO 1042−58, SAO 238447, CD−58 3547, HD 93420 | |
| Database references | |
| SIMBAD | data |
BO Carinae, also known as HD 93420, is an irregular variable star in the constellation Carina.
BO Car has a maximum apparent magnitude of +7.18. Its distance and membership is uncertain, but its possible membership to the star cluster Trumpler 15 allows a distance estimate of approximately 2,500 parsecs (8,150 light-years).[4][5] The Gaia Data Release 2 parallax of 0.73±0.08 mas suggests a closer distance, but the value is considered unreliable due to excess astrometric noise.[6]
BO Car is a red supergiant of spectral type M4Ib with an effective temperature of 3,525 K, a radius of 790 solar radii. Its bolometric luminosity is 78,000 L☉.[3] Mass-loss is on the order of 0.3×10−9 solar masses per year.[5]
In 1919, William Matthew Worssell of the Union Observatory announced that the star, then known as CPD-58 2683, is a variable star.[8] It was given its variable star designation, BO Carinae, in 1921.[9] Billed as an irregular variable like TZ Cassiopeiae or V528 Carinae; its apparent brightness fluctuates between magnitude +7.18 and +8.50 without clear periodicity.[1][10] Some observers have found BO Car not to be variable,[11] but more extensive studies find small amplitude variations with a possible period of 145 days.[12]
Multiple star catalogues list an 11th-magnitude star as a companion to BO Car. The separation was 14.2″ in 2015, and slowly increasing.[13] The companion is a distant blue giant.[14]
See also
References
- ↑ 1.0 1.1 1.2 1.3 Samus, N. N. 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.
- ↑ 2.0 2.1 2.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Cite error: Invalid
<ref>tag; no text was provided for refs namedrg - ↑ Tapia, Mauricio; Roth, Miguel; Vázquez, Rubén A.; Feinstein, Alejandro (2003). "Imaging study of NGC 3372, the Carina nebula - I. UBVRIJHK photometry of Tr 14, Tr 15, Tr 16 and Car I". Monthly Notices of the Royal Astronomical Society 339 (1): 44–62. doi:10.1046/j.1365-8711.2003.06186.x. Bibcode: 2003MNRAS.339...44T.
- ↑ 5.0 5.1 Josselin, E.; Blommaert, J. A. D. L.; Groenewegen, M. A. T.; Omont, A.; Li, F. L. (2000). "Observational investigation of mass loss of M supergiants". Astronomy and Astrophysics 357: 225–232. Bibcode: 2000A&A...357..225J.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ "ASAS All Star Catalogue". The All Sky Automated Survey. http://www.astrouw.edu.pl/asas/?page=aasc.
- ↑ Worssell, M. W. (1919). "Variable Stars". Circular of the Union Observatory Johannesburg 46: 17. https://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?journal=CiUO.&year=%3f%3f%3f%3f&volume=..46&letter=.&db_key=AST&page_ind=19&plate_select=NO&data_type=GIF&type=SCREEN_GIF&classic=YES. Retrieved 7 January 2025.
- ↑ Hartwig; Müller (January 1921). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten 212 (19): 353-374. doi:10.1002/asna.19202121902. https://articles.adsabs.harvard.edu/pdf/1921AN....212..353.. Retrieved 7 January 2025.
- ↑ Chatys, Filip W.; Bedding, Timothy R.; Murphy, Simon J.; Kiss, László L.; Dobie, Dougal; Grindlay, Jonathan E. (2019). "The period-luminosity relation of red supergiants with Gaia DR2". Monthly Notices of the Royal Astronomical Society 487 (4): 4832. doi:10.1093/mnras/stz1584. Bibcode: 2019MNRAS.487.4832C.
- ↑ Percy, John R.; Sato, Hiromitsu (2009-02-01). "Long Secondary Periods in Pulsating Red Supergiant Stars". Journal of the Royal Astronomical Society of Canada 103 (1): 11. ISSN 0035-872X. Bibcode: 2009JRASC.103...11P.
- ↑ Percy, J. R. (2020). "Period Analysis of All-Sky Automated Survey for Supernovae (ASAS-SN) Data on a Sample of "Irregular" Pulsating Red Giants". Journal of the American Association of Variable Star Observers (Jaavso) 48 (1): 50. Bibcode: 2020JAVSO..48...50P.
- ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
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