Astronomy:HD 23753
  | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus[1] |
| Right ascension | 03h 48m 20.81678s[2] |
| Declination | +23° 25′ 16.4959″[2] |
| Apparent magnitude (V) | 5.44[1] |
| Characteristics | |
| Evolutionary stage | main sequence[3] |
| Spectral type | B9 Vn[4] |
| B−V color index | −0.067±0.008[1] |
| Astrometry | |
| Radial velocity (Rv) | +7.6±0.5[5] km/s |
| Proper motion (μ) | RA: +19.695[2] mas/yr Dec.: −47.113[2] mas/yr |
| Parallax (π) | 7.6909 ± 0.0985[2] mas |
| Distance | 424 ± 5 ly (130 ± 2 pc) |
| Absolute magnitude (MV) | 0.00[1] |
| Details | |
| Mass | 3.21±0.07[3] M☉ |
| Radius | 2.7[6] R☉ |
| Luminosity | 150.0+16.2 −14.8[3] L☉ |
| Surface gravity (log g) | 4.09[7] cgs |
| Temperature | 11,535+80 −79[3] K |
| Metallicity [Fe/H] | −0.57[7] dex |
| Rotation | 0.6994 d[8] |
| Rotational velocity (v sin i) | 335[3] km/s |
| Age | 125[9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 23753 is a single[11] star in the equatorial zodiac constellation of Taurus, and is a member of the Pleiades open cluster.[12] It is dimly visible to the naked eye with an apparent visual magnitude of 5.44.[1] The distance to this star, as determined from its annual parallax shift of 7.7 mas, is about 424 light years. It is moving further from the Earth with a heliocentric radial velocity of +8 km/s.[5] The star is positioned near the ecliptic and so is subject to lunar occultations.[13]
This is a B-type main-sequence star with a stellar classification of B9 Vn,[4] where the 'n' indicates "nebulous" lines due to rapid rotation. It is 125 million years old[9] with a projected rotational velocity of 335 km/s,[3] completing a full revolution about its axis every 16.79 hours.[8] HD 23753 has been catalogued as a suspected variable star with the designation NSV 1321,[14] although the amplitude is no more than 0.1 magnitude and it may even be suitable for a photometric standard.[15] Wraight et al. report that STEREO detected very shallow eclipses, with a period of 2.2663 days, during which the brightness falls by 1%.[16]
HD 23753 has 3.21 times the mass of the Sun[3] and 2.7 times the Sun's radius.[6] It is radiating 150 times the Sun's luminosity[3] from its photosphere at an effective temperature of 11,535 K.[3]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 2.4 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z.
- ↑ 4.0 4.1 Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal 77: 750–755, doi:10.1086/111348, Bibcode: 1972AJ.....77..750C.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 6.0 6.1 Huber, Daniel; Bryson, Stephen T.; Haas, Michael R.; Barclay, Thomas; Barentsen, Geert; Howell, Steve B.; Sharma, Sanjib; Stello, Dennis et al. (2016), "The K2 Ecliptic Plane Input Catalog (EPIC) and Stellar Classifications of 138,600 Targets in Campaigns 1-8", The Astrophysical Journal Supplement Series 224 (1): 2, doi:10.3847/0067-0049/224/1/2, Bibcode: 2016ApJS..224....2H.
- ↑ 7.0 7.1 Khalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G. et al. (2024), "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost", Astronomy and Astrophysics 691: A98, doi:10.1051/0004-6361/202451427, Bibcode: 2024A&A...691A..98K.
- ↑ 8.0 8.1 Rebull, L. M. et al. (November 2016), "Rotation in the Pleiades with K2. I. Data and First Results", The Astronomical Journal 152 (5): 19, doi:10.3847/0004-6256/152/5/113, 113, Bibcode: 2016AJ....152..113R.
- ↑ 9.0 9.1 Su, K. Y. L. et al. (December 2006), "Debris Disk Evolution around A Stars", The Astrophysical Journal 653 (1): 675–689, doi:10.1086/508649, Bibcode: 2006ApJ...653..675S.
- ↑ "HD 161840". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+161840.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ White, Richard E. et al. (February 2001), "Interstellar Matter Near the Pleiades. V. Observations of NA I toward 36 Stars", The Astrophysical Journal Supplement Series 132 (2): 253–280, doi:10.1086/318950, Bibcode: 2001ApJS..132..253W
- ↑ Eitter, J. J.; Beavers, W. I. (August 1977), "Lunar occultation summary. II", Astrophysical Journal Supplement Series 34: 493–504, doi:10.1086/190460, Bibcode: 1977ApJS...34..493E.
- ↑ Samus', N. N. et al. (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ Adelman, S. J. et al. (October 2000), "On the Variability of Late B III-V Stars", Information Bulletin on Variable Stars 4968: 1, Bibcode: 2000IBVS.4968....1A.
- ↑ Wraight, K. T.; White, Glenn J.; Bewsher, D.; Norton, A. J. (October 2011), "STEREO observations of stars and the search for exoplanets", Monthly Notices of the Royal Astronomical Society 416 (4): 2477–2493, doi:10.1111/j.1365-2966.2011.18599.x, Bibcode: 2011MNRAS.416.2477W.
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