HD 138289

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HD 138289
Apus constellation map.svg
Red circle.svg
location of HD 138289 on the map (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Apus
Right ascension 15h 39m 18.39712s [1]
Declination −77° 55′ 04.8196″ [1]
Apparent magnitude  (V)6.18±0.01 [2]
Characteristics
Evolutionary stage horizontal branch [3]
Spectral type K2.5 IIIb CN1.5 Ba+0.5 [4]
U−B color index +1.36 [5]
B−V color index +1.21 [5]
Astrometry
Radial velocity (Rv)+13.1 [6]  km/s
Proper motion (μ)RA: −79.376  mas/yr [1]
Dec.: −130.969  mas/yr [1]
Parallax (π)9.0832 ± 0.0204  mas [1]
Distance 359.1 ± 0.8  ly
(110.1 ± 0.2  pc)
Absolute magnitude  (MV)+1.21 [7]
Details
Mass 1.59 [8]   M☉
Radius 13±0.7 [9]   R☉
Luminosity 52.5+2.5
−2.4 [10]   L☉
Surface gravity (log g)2.71 [8]   cgs
Temperature 4,672±100 [11]   K
Metallicity [Fe/H]−0.04 [8]   dex
Rotational velocity (v sin i)5.2±4.3 [12]  km/s
Age 2.78+0.37
−0.52 [1]   Gyr
Other designations
32 G. Apodis [13] , CPD−77°1134, FK5  3228, GC  20948, HD  138289, HIP  76664, HR  5757, SAO  257303 [14]
Database references
SIMBAD data

HD 138289, also known as HR 5757, is a probable spectroscopic binary [12] located in the constellation Apus, the bird-of-paradise. It has an apparent magnitude of 6.18, [2] placing it near the limit for naked eye. Gaia DR3 parallax measurements place the object 359 light years away [1] and it is currently receding with a heliocentric radial velocity of 13.1  km/s . [6] At its current distance, HD 138289's brightness is diminished by 0.25 magnitudes due to extinction from interstellar dust. [15] It has an absolute magnitude of +1.21. [7]

The visible component has a stellar classification of K2.5 IIIb CN1.5 Ba+0.5, [4] indicating that it is a red giant with an anomalous overabundance of cyano radicals in its spectrum. The IIIb luminosity class indicates that it is a lower luminosity giant star. The Ba+0.5 suffix states that it is a mild barium star, whose barium abundance might have come from a hidden white dwarf companion. HD 138289 is estimated to be 2.8 billion years old, [1] enough time for it to cool and expand to 13 times the radius of the Sun. [9] It is now on the horizontal branch, [3] fusing helium at its core. At present it has 1.59 times the mass of the Sun and radiates 52.5 times the luminosity of the Sun [10] from its enlarged photosphere at an effective temperature of 4,672  K . [11] HD 138289 has a near solar metallicity and spins modestly with a poorly constrained projected rotational velocity of 5.2  km/s . [12]

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

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<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

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

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Pi<sup>2</sup> Doradus G-type giant in the constellation Dorado

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References

  1. 1 2 3 4 5 6 7 8 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 Laney, C. D.; Joner, M. D.; Pietrzyński, G. (11 November 2011). "A new Large Magellanic Cloud K-band distance from precision measurements of nearby red clump stars". Monthly Notices of the Royal Astronomical Society. 419 (2): 1637–1641. arXiv: 1109.4800 . Bibcode:2012MNRAS.419.1637L. doi: 10.1111/j.1365-2966.2011.19826.x . ISSN   0035-8711.
  4. 1 2 Keenan, Philip C.; McNeil, Raymond C. (October 1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. eISSN   1538-4365. ISSN   0067-0049.
  5. 1 2 Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  6. 1 2 Evans, David S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E
  7. 1 2 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.
  8. 1 2 3 Liu, Y. J.; Zhao, G.; Shi, J. R.; Pietrzyński, G.; Gieren, W. (7 November 2007). "The abundances of nearby red clump giants". Monthly Notices of the Royal Astronomical Society. 382 (2): 553–566. Bibcode:2007MNRAS.382..553L. doi: 10.1111/j.1365-2966.2007.11852.x . eISSN   1365-2966. ISSN   0035-8711.
  9. 1 2 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants". Astronomy & Astrophysics. 426 (1): 297–307. arXiv: astro-ph/0404180 . Bibcode:2004A&A...426..297K. doi: 10.1051/0004-6361:20035930 . eISSN   1432-0746. ISSN   0004-6361.
  10. 1 2 Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (January 2020). "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era". Astronomy & Astrophysics. 633: A34. arXiv: 1910.12732 . Bibcode:2020A&A...633A..34C. doi: 10.1051/0004-6361/201936360 . eISSN   1432-0746. ISSN   0004-6361.
  11. 1 2 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.
  12. 1 2 3 De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars V: Southern stars". Astronomy & Astrophysics. 561: A126. arXiv: 1312.3474 . Bibcode:2014A&A...561A.126D. doi: 10.1051/0004-6361/201220762 . eISSN   1432-0746. ISSN   0004-6361. S2CID   54046583.
  13. ↑ 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.
  14. ↑ "HD 138289". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 September 2015.
  15. ↑ 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.
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