Astronomy:10 Lacertae
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lacerta |
| Right ascension | 22h 39m 15.67804s[1] |
| Declination | +39° 03′ 00.9724″[1] |
| Apparent magnitude (V) | 4.880[2] |
| Characteristics | |
| Spectral type | O9VCite error: Closing </ref> missing for <ref> tag
|
| Astrometry | |
| Radial velocity (Rv) | −10.10[3] km/s |
| Proper motion (μ) | RA: −1.274[1] mas/yr Dec.: −5.605[1] mas/yr |
| Parallax (π) | 2.192 ± 0.131[1] mas |
| Distance | 1,800±100 ly (552±32 pc) |
| Absolute magnitude (MV) | −4.17±0.12[4] |
| Details[4] | |
| Mass | 21.6±0.5 M☉ |
| Radius | 7.4±0.5 R☉ |
| Luminosity | 69,200+8,440 −7,520 L☉ |
| Surface gravity (log g) | 4.04±0.05 cgs |
| Temperature | 34,550±300 K |
| Rotational velocity (v sin i) | 14±1 km/s |
| Age | 3.55+0.72 −0.60 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
10 Lacertae (10 Lac) is a star in the constellation Lacerta. With an apparent magnitude of 4.9, it is located around 550 parsecs (1,800 ly) distant in the small Lacerta OB1 association. It is a hot blue main-sequence star of spectral type O9V, a massive star that is currently fusing its core hydrogen. It is a suspected Beta Cephei variable star.
It was one of the first O-type stars (along with S Monocerotis) to be defined as an anchor point for the MKK spectral classification; since the early twentieth century it has served as such a point. Specifically, the star is representative of O9V stars, meaning relatively cool O-type stars on the main-sequence.[5]
It is the star with the smallest angular diameter measured by the CHARA array, at 0.11±0.02 milliarcseconds.[6]
10 Lacertae has an 8th magnitude companion about one arc-minute away.[7]
References
- ↑ 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.
- ↑ Oja, T. (September 1993). "UBV photometry of stars whose positions are accurately known. VII". Astronomy and Astrophysics Supplement Series 100 (3): 591–592. ISSN 0365-0138. Bibcode: 1993A&AS..100..591O.
- ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
- ↑ 4.0 4.1 Aschenbrenner, P.; Przybilla, N.; Butler, K. (2023-03-01). "Quantitative spectroscopy of late O-type main-sequence stars with a hybrid non-LTE method". Astronomy and Astrophysics 671: A36. doi:10.1051/0004-6361/202244906. ISSN 0004-6361. Bibcode: 2023A&A...671A..36A.
- ↑ Garrison, R. F. (1994). "A Hierarchy of Standards for the MK Process". Astronomical Society of the Pacific 60: 3. Bibcode: 1994ASPC...60....3G.
- ↑ Gordon, Kathryn D.; Gies, Douglas R.; Schaefer, Gail H.; Huber, Daniel; Ireland, Michael; Hillier, D. John (December 2018). "Angular Sizes and Effective Temperatures of O-type Stars from Optical Interferometry with the CHARA Array" (in en). The Astrophysical Journal 869 (1): 37. doi:10.3847/1538-4357/aaec04. ISSN 0004-637X. Bibcode: 2018ApJ...869...37G.
- ↑ Dommanget, J.; Nys, O. (1994). "Catalogue of the Components of Double and Multiple stars (CCDM). First edition.". Communications de l'Observatoire Royal de Belgique 115. Bibcode: 1994CoORB.115.....D.
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