Astronomy:HD 138867

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Short description: Star in the constellation of Apus
HD 138867
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Apus
Right ascension  15h 41m 54.68806s[1]
Declination −76° 04′ 55.0718″[1]
Apparent magnitude (V) 5.94±0.01[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type B9.5 V[4]
Astrometry
Radial velocity (Rv)1.1±1.7[5] km/s
Proper motion (μ) RA: −12.407[1] mas/yr
Dec.: −41.541[1] mas/yr
Parallax (π)7.8146 ± 0.0916[1] mas
Distance417 ± 5 ly
(128 ± 1 pc)
Absolute magnitude (MV)+0.4[6]
Details
Mass2.81[3] M☉
Radius2.59±0.09[7] R☉
Luminosity54.9[8] L☉
Surface gravity (log g)4.04±0.07[7] cgs
Temperature10,375±48[3] K
Metallicity [Fe/H]0.00[9] dex
Rotational velocity (v sin i)178[10] km/s
Age272[9] Myr
Other designations
CPD−75°1222, FK5 3235, GC 21025, HD 138867, HIP 76877, HR 5786, SAO 257310[11]
Database references
SIMBADdata

HD 138867, also known as HR 5786, is a bluish-white hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 5.94,[2] making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 417 light years away from Earth.[1] However, it is receding with a heliocentric radial velocity of 1.1 km/s.[5]

HD 138867 has a stellar classification of B9.5 V,[4] indicating that it is a B-type main-sequence star just shy of being an A-type star. It has 2.81 times the mass of the Sun[3] and is estimated to be 272 million years,[9] having completed 67.4% of its main sequence lifetime.[3] HD 138867 has an effective temperature of 10,375 K,[3] which combined with a radius of 2.59 R☉,[7] yields a luminosity over 50 times that of Sun.[8] A solar metallicity has been calculated for HD 138867.[9] It is currently spinning rapidly with a projected rotational velocity of 178 km/s.[10]

There has been disagreement in regards to HD 138867's muplicity. Chini et al. (2012) list it as a solitary star[12] while Eggleton and Tokovinn (2008) found it to be an astrometric binary.[13] The first one is more likely as the object has a constant radial velocity.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 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.
  2. ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. ISSN 0004-6361. Bibcode: 2012A&A...537A.120Z. 
  4. ↑ 4.0 4.1 Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series 99: 135. doi:10.1086/192182. ISSN 0067-0049. Bibcode: 1995ApJS...99..135A. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (November 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. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 Stassun, Keivan G. et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S. 
  8. ↑ 8.0 8.1 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (15 June 2017). "Fundamental parameters and infrared excesses of Tycho–Gaia stars". Monthly Notices of the Royal Astronomical Society 471 (1): 770–791. doi:10.1093/mnras/stx1433. ISSN 0035-8711. Bibcode: 2017MNRAS.471..770M. 
  9. ↑ 9.0 9.1 9.2 9.3 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters 38 (12): 771–782. doi:10.1134/S1063773712120031. ISSN 0320-0108. Bibcode: 2012AstL...38..771G. 
  10. ↑ 10.0 10.1 Levato, H.; Grosso, M. (June 2004). "New Projected Rotational Velocities of All Southern B-type Stars of the Bright Star Catalogue". Astronomical Society of the Pacific 215: 51. Bibcode: 2004IAUS..215...51L. 
  11. ↑ "HD 138867". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+138867. 
  12. ↑ Chini, R.; Hoffmeister, V. H.; Nasseri, A.; Stahl, O.; Zinnecker, H. (10 July 2012). "A spectroscopic survey on the multiplicity of high-mass stars". Monthly Notices of the Royal Astronomical Society 424 (3): 1925–1929. doi:10.1111/j.1365-2966.2012.21317.x. ISSN 0035-8711. Bibcode: 2012MNRAS.424.1925C. 
  13. ↑ 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. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
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