Beta Sextantis
Location of β Sextantis (circled in red) | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Sextans |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | 5.07[2] |
| Characteristics | |
| Evolutionary stage | Main sequence[3] |
| Spectral type | B6 V[4] or B5 IV/V[5] |
| U−B color index | −0.51[2] |
| B−V color index | −0.14[2] |
| Variable type | α2 CVn[6] |
| Astrometry | |
| Radial velocity (Rv) | 11.6±2.8[7] km/s |
| Proper motion (μ) | RA: −39.290 mas/yr[1] Dec.: −23.582 mas/yr[1] |
| Parallax (π) | 8.8899±0.1477 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | −0.38[8] |
| Details | |
| Mass | 4.01±0.07[3] M☉ |
| Radius | 3.00[9] R☉ |
| Luminosity | 330[3] L☉ |
| Surface gravity (log g) | 4.21[10] cgs |
| Temperature | 13,870[3] K |
| Metallicity [Fe/H] | 0.19[10] dex |
| Rotational velocity (v sin i) | 85±4[10] km/s |
| Age | 216[11] Myr |
| Other designations | |
| Template:Odlist[12] | |
| Database references | |
| SIMBAD | data |
Beta Sextantis, Latinized from β Sextantis, is a variable star in the equatorial constellation of Sextans. With an apparent visual magnitude of 5.07,[2] it is faintly visible to the naked eye on a dark night. According to the Bortle scale, it can be viewed from brighter lit suburban skies. The distance to this star, based upon an annual parallax shift of 8.89 mas,[1] is around 367 light years.
This star served as a primary standard in the MK spectral classification system with a stellar classification of B6 V,[4] indicating that it is a B-type main sequence star. However, Houk and Swift (1999) list a classification of B5 IV/V, suggesting it may be transitioning into a subgiant star.[5] Stellar evolution models support this is a main sequence star.[3] It has served as a uvby photometric standard, but is also categorized as an Alpha2 Canum Venaticorum variable[6] with a suspected period of 15.4 days. This lengthy a period conflicts with a relatively high projected rotational velocity of 85 km/s, leaving the explanation for the variance unresolved.[10][4]
References
- ^ a b c d e Template:Cite DR3
- ^ a b c d Page Module:Citation/CS1/styles.css has no content.Crawford, D. L.; et al. (1971). "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere". The Astronomical Journal. 76: 1058. Bibcode:1971AJ.....76.1058C. doi:10.1086/111220.
- ^ a b c d e Page Module:Citation/CS1/styles.css has no content.Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics. 537: A120. arXiv:1201.2052. Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691.
- ^ a b c Page Module:Citation/CS1/styles.css has no content.Mathys, G.; et al. (March 1986). "Photometric variability of some early-type stars". Astronomy and Astrophysics Supplement Series. 63 (3): 403–416. Bibcode:1986A&AS...63..403M.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1999MSS...C05....0H.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Kholopov, P. N.; et al. (April 1989). "The 69th Name-List of Variable Stars". Information Bulletin on Variable Stars. 3323 (3323): 1. Bibcode:1989IBVS.3323....1K.
- ^ Page Module:Citation/CS1/styles.css has no content.de Bruijne, J. H. J.; Eilers, A.-C. (October 2012). "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project". Astronomy & Astrophysics. 546: 14. arXiv:1208.3048. Bibcode:2012A&A...546A..61D. doi:10.1051/0004-6361/201219219. S2CID 59451347. A61.
- ^ Template:Cite XHIP
- ^ Page Module:Citation/CS1/styles.css has no content.McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017-10-01). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society. 471: 770–791. arXiv:1706.02208. Bibcode:2017MNRAS.471..770M. doi:10.1093/mnras/stx1433. ISSN 0035-8711.
- ^ a b c d Page Module:Citation/CS1/styles.css has no content.Hempel, M.; Holweger, H. (September 2003). "Abundance analysis of late B stars. Evidence for diffusion and against weak stellar winds". Astronomy and Astrophysics. 408 (3): 1065–1076. Bibcode:2003A&A...408.1065H. doi:10.1051/0004-6361:20030889.
- ^ Page Module:Citation/CS1/styles.css has no content.Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771. arXiv:1606.08814. Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031.
- ^ Page Module:Citation/CS1/styles.css has no content."bet Sex". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-12-13.
{{cite web}}: Invalid|mode=Script error: No such module "Citation mode".(help) - ^ Page Module:Citation/CS1/styles.css has no content."MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 27 August 2024.
