HD 10390

Last updated
HD 10390
Triangulum constellation map.svg
Red circle.svg
Location of HD 10390 on the map (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Triangulum
Right ascension 01h 42m 03.48964s [1]
Declination +35° 14′ 44.5389″ [1]
Apparent magnitude  (V)5.64 [2]
Characteristics
Evolutionary stage main sequence star [3]
Spectral type B9 IV-V [4] or B9 V [5]
U−B color index −0.20 [2]
B−V color index −0.07 [2]
Astrometry
Radial velocity (Rv)−1.9±2.0 [6]  km/s
Proper motion (μ)RA: +48.763  mas/yr [1]
Dec.: −25.418  mas/yr [1]
Parallax (π)11.1882 ± 0.164  mas [1]
Distance 292 ± 4  ly
(89 ± 1  pc)
Absolute magnitude  (MV)+1.00 [7]
Details
Mass 2.62 [8]   M☉
Radius 2.14±0.11 [9]   R☉
Luminosity 51.5+2.4
−2.3 [3]   L☉
Surface gravity (log g)4.23+0.08
−0.04 [10]   cgs
Temperature 11,076±139 [11]   K
Metallicity [Fe/H]−0.20 [12]   dex
Rotational velocity (v sin i)45 [13]  km/s
Age 50+81
−31 [14]   Myr
Other designations
6 H. Trianguli, [15] AG+34°163, BD+34°297, FK5  1047, GC  2064, HD  10390, HIP  7943, HR  490, SAO  54912, TIC  61524043 [16]
Database references
SIMBAD data

HD 10390 (HR 490; 51 H. Trinaguli) is a solitary star [17] located in the northern constellation Triangulum. It is faintly visible to the naked eye as a bluish-white hued point of light with an apparent magnitude of 5.64. [2] The object is located relatively close at a distance of 292 light-years based on Gaia DR3 parallax measurements [1] and it is drifting closer with a heliocentric radial velocity of −1.9  km/s . [6] At its current distance, HD 10390's brightness is diminished by an interstellar extinction of only five-hundredths of a magnitude [18] and it has an absolute magnitude of +1.00. [7]

HD 10390 has a stellar classification of B9 IV-V, [4] indicating that it is a slightly evolved B-type star with a luminosity class intermediate between a subgiant and a main sequence star. Osawa (1959) gave a class of B9 V, [5] instead indicating that it is an ordinary B-type main-sequence star that is generating energy via hydrogen fusion at its core. It has 2.62 times the mass of the Sun [8] and 2.14 times the radius of the Sun. [9] It radiates 51.5 times the luminosity of the Sun [3] from its photosphere at an effective temperature of 11,076  K . [11] HD 10390 is metal defecient with an iron abundance of [Fe/H] = −0.2 or 63.1% of the Sun's [12] and it spins modestly with a projected rotational velocity of 45  km/s , [13] well below its breakup velocity of 355 km/s. [19] Despite the first classification, HD 10390 has only completed 16.8% of its main sequence lifetime [3] at the age of approximately 50 million years. [14]

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<span class="mw-page-title-main">3 Piscis Austrini</span> Star in the constellation Microscopium

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<span class="mw-page-title-main">HD 106248</span> Star in the constellation Chamaeleon

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References

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  8. 1 2 David, Trevor J.; Hillenbrand, Lynne A. (12 May 2015). "The Ages of Early-type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi: 10.1088/0004-637X/804/2/146 . eISSN   1538-4357. S2CID   33401607.
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  10. ↑ Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . eISSN   1538-3881. hdl: 1721.1/124721 . S2CID   166227927.
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  12. 1 2 Anders, F.; et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi: 10.1051/0004-6361/201935765 . eISSN   1432-0746. ISSN   0004-6361. S2CID   131780028.
  13. 1 2 Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002). "Rotational Velocities of B Stars". The Astrophysical Journal. 573 (1): 359–365. Bibcode:2002ApJ...573..359A. doi: 10.1086/340590 . ISSN   0004-637X.
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  16. ↑ "HD 10390". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved December 15, 2023.
  17. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . eISSN   1365-2966. ISSN   0035-8711. S2CID   14878976.
  18. ↑ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society. 472 (4): 3805–3820. arXiv: 1709.01160 . Bibcode:2017MNRAS.472.3805G. doi: 10.1093/mnras/stx2219 . eISSN   1365-2966. ISSN   0035-8711. S2CID   118879856.
  19. ↑ Huang, Wenjin; Gies, D. R.; McSwain, M. V. (22 September 2010). "A Stellar Rotation Census of B Stars: From ZAMS to TAMS". The Astrophysical Journal. 722 (1): 605–619. arXiv: 1008.1761 . Bibcode:2010ApJ...722..605H. doi: 10.1088/0004-637X/722/1/605 . eISSN   1538-4357. ISSN   0004-637X.
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