HD 138867

Last updated
HD 138867
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
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  mas/yr [1]
Dec.: −41.541  mas/yr [1]
Parallax (π)7.8146 ± 0.0916  mas [1]
Distance 417 ± 5  ly
(128 ± 1  pc)
Absolute magnitude  (MV)+0.4 [6]
Details
Mass 2.81 [3]   M☉
Radius 2.59±0.09 [7]   R☉
Luminosity 54.9 [8]   L☉
Surface gravity (log g)4.04±0.07 [7]   cgs
Temperature 10,375±48 [3]   K
Metallicity [Fe/H]0.00 [9]   dex
Rotational velocity (v sin i)178 [10]  km/s
Age 272 [9]   Myr
Other designations
34 G. Apodis [11] , CPD−75°1222, FK5  3235, GC  21025, HD  138867, HIP  76877, HR  5786, SAO  257310 [12]
Database references
SIMBAD data

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 [13] while Eggleton and Tokovinn (2008) found it to be an astrometric binary. [14] The first one is more likely as the object has a constant radial velocity.

Related Research Articles

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<span class="mw-page-title-main">Q Scorpii</span> High proper motion binary star system in the constellation of Scorpius

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<span class="mw-page-title-main">HD 26764</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">HD 25291</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">HD 76236</span> Star in the constellation Chamaeleon

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HD 194612 is a solitary orange hued star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.9, making it visible to the naked eye under ideal conditions. Parallax measurements place it at a distance of 760 light years and it has a low heliocentric radial velocity of 0.3 km/s.

HD 75171, also known as HR 3495, is a solitary, white hued star located in the southern constellation of Volans. It has an apparent magnitude of 6.02, making it faintly visible to the naked eye under ideal conditions. The object is relatively close at a distance of 191 light years but is receding with a heliocentric radial velocity of 10.7 km/s. Eggen (1995) lists it as a probable member of the Hyades Supercluster.

<span class="mw-page-title-main">WZ Columbae</span> Star in the constellation of Columba

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HD 43899, also designated as HR 2263, is a solitary, orange hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.53, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 284 light years distant. It appears to be rapidly receding with a heliocentric radial velocity of 66.5 km/s. Eggen (1993) lists HD 43899 as an old disk star and its kinematics match with that of the ζ Herculis moving group.

<span class="mw-page-title-main">HD 198716</span> Star in the constellation of Microscopium

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<span class="mw-page-title-main">HD 197630</span> Star in the constellation of Microscopium

HD 197630, also known as HR 7933 or rarely 23 G. Microscopii, is a probable astrometric binary located in the southern constellation Microscopium. The visible component is a bluish-white hued star that is faintly visible to the naked eye with an apparent magnitude of 5.47. Based on parallax measurements from the Gaia satellite, the system is estimated to be 328 light years away. However, it is drifting closer with a heliocentric radial velocity of −30 km/s. At its current distance, HD 197630's brightness is diminished by 0.11 magnitudes due to interstellar dust. A 2012 multiplicity survey failed to confirm the velocity variations.

<span class="mw-page-title-main">HD 168592</span> Star in the constellation of Corona Australis

HD 168592, also designated as HR 6862 or rarely 7 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.07. Gaia DR3 parallax measurements place it at a distance of 490 light years and is currently receding with a heliocentric radial velocity of 18 km/s. At its current distance, HD 168592's brightness is diminished by 0.38 magnitudes due to interstellar dust. It has an absolute magnitude of −0.76.

<span class="mw-page-title-main">HD 175219</span> K-type giant; Corona Australis

HD 175219, also known as HR 7122, is a solitary, orange hued star located in the southern constellation Corona Australis. It has an apparent magnitude of 5.35, allowing it to be faintly visible to the naked eye. The object is located relatively close at a distance of 314 light years based on Gaia DR3 parallax measurements but is drifting closer with a heliocentric radial velocity of −21.1 km/s. At its current distance, HD 175219's brightness is diminished by 0.26 magnitudes due to interstellar dust. It has an absolute magnitude of +0.57.

<span class="mw-page-title-main">HD 31134</span> Star in the constellation of Camelopardalis

HD 31134, also designated as HR 1561, is a solitary star located in the northern circumpolar constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued star with an apparent magnitude of 5.74. Gaia DR3 parallax measurements place it 473 light years away. It appears to be approaching the Solar System with a heliocentric radial velocity of −15.1 km/s. At its current distance, HD 31134's brightness is diminished by 0.35 magnitudes due to interstellar dust. It has an absolute magnitude of +0.19.

<span class="mw-page-title-main">HD 170521</span> Distant K-type giant; Corona Australis

HD 170521, also known as HR 6937 or rarely 12 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued point of light with an apparent magnitude of 5.69. The object is located relatively far at a distance of approximately 1,500 light years based on Gaia DR3 parallax measurements, and it is receding with a heliocentric radial velocity of 7.2 km/s. At its current distance, HD 170521's brightness is heavily diminished by 0.46 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of −1.90.

<span class="mw-page-title-main">HD 28780</span> A-type star in the constellation Camelopardalis

HD 28780, also known as HR 1440, is a solitary white-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.91, making it faintly viisble to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 488 light-years, and it is currently drifting closer with a heliocentric radial velocity of −22.6 km/s. At its current distance, HD 28780's brightness is diminished by 0.33 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.26.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. 1 2 3 4 5 6 Zorec, J.; Royer, F. (January 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 . ISSN   0004-6361. S2CID   55586789.
  4. 1 2 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. Bibcode:1995ApJS...99..135A. doi: 10.1086/192182 . ISSN   0067-0049.
  5. 1 2 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. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN   1562-6873. ISSN   1063-7737. S2CID   119231169.
  6. ↑ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  7. 1 2 3 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.
  8. 1 2 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. arXiv: 1706.02208 . Bibcode:2017MNRAS.471..770M. doi: 10.1093/mnras/stx1433 . eISSN   1365-2966. ISSN   0035-8711.
  9. 1 2 3 4 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. ISSN   0320-0108. S2CID   118345778.
  10. 1 2 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. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  12. ↑ "HD 138867". SIMBAD . Centre de données astronomiques de Strasbourg.
  13. ↑ 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. arXiv: 1205.5238 . Bibcode:2012MNRAS.424.1925C. doi: 10.1111/j.1365-2966.2012.21317.x . ISSN   0035-8711.
  14. ↑ 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.
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