HD 175219
Location of HD 175219 (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Corona Australis
Right ascension 18h 56m 16.95125s[1]
Declination −42° 42′ 38.4231″[1]
Apparent magnitude (V) 5.35±0.01[2]
Characteristics
Spectral type K0 III[3] or G6 III-IV[4]
B−V color index +1.00[5]
Astrometry
Radial velocity (Rv)−21.1±0.8[6] km/s
Proper motion (μ) RA: −27.046 mas/yr
Dec.: −29.284 mas/yr
Parallax (π)10.3847 ± 0.109 mas[1]
Distance314 ± 3 ly
(96 ± 1 pc)
Absolute magnitude (MV)+0.57[7]
Details
Mass1.93±0.21[8] M☉
Radius12.3±0.2[8] R☉
Luminosity76.3±2.0[8] L☉
Surface gravity (log g)2.55±0.07[8] cgs
Temperature4,877±26[8] K
Metallicity [Fe/H]−0.28±0.02[8] dex
Rotational velocity (v sin i)<1[9] km/s
Age346[1] Myr
Other designations
30 G. Coronae Australis[10], CD−42°13761, CPD−42°8539, GC 25956, HD 175219, HIP 92953, HR 7122, SAO 229383[11]
Database references
SIMBADdata

HD 175219, also known as HR 7122, is a solitary,[12] orange hued star located in the southern constellation Corona Australis. It has an apparent magnitude of 5.35,[2] 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[1] but is drifting closer with a heliocentric radial velocity of −21.1 km/s.[6] At its current distance, HD 175219's brightness is diminished by 0.26 magnitudes due to interstellar dust.[13] It has an absolute magnitude of +0.57.[7]

This is a red giant with a stellar classification of K0 III.[3] An earlier source gives it a class of G6 III-IV,[4] indicating that it is an evolved G-type star with a luminosity class intermediate between a giant star and a subgiant. At present it has nearly twice the mass of the Sun but it has expanded to 12.3 times the Sun's radius.[8] HD 175219 radiates 76.3 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,877 K.[8] The star is metal deficient, having less than half the abundance of heavy elements compared to the Sun.[8] Common for giant stars, it spins slowly, having a projected rotational velocity too low to be measured accurately.[9]

References

  1. 1 2 3 4 5 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 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars Volume II: Declinations −52° to −41°. Bibcode:1978mcts.book.....H.
  4. 1 2 Evans, D. S.; Menzies, A.; Stoy, R. H. (1 December 1959). "Fundamental Data for Southern Stars (Second List)". Monthly Notices of the Royal Astronomical Society. 119 (6): 638–647. Bibcode:1959MNRAS.119..638E. doi:10.1093/mnras/119.6.638. eISSN 1365-2966. ISSN 0035-8711.
  5. ↑ 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 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.
  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 4 5 6 7 8 9 Ottoni, G.; Udry, S.; Ségransan, D.; Buldgen, G.; Lovis, C.; Eggenberger, P.; Pezzotti, C.; Adibekyan, V.; Marmier, M.; Mayor, M.; Santos, N. C.; Sousa, S. G.; Lagarde, N.; Charbonnel, C. (January 2022). "CORALIE radial-velocity search for companions around evolved stars (CASCADES): I. Sample definition and first results: Three new planets orbiting giant stars". Astronomy & Astrophysics. 657: A87. arXiv:2201.01528. Bibcode:2022A&A...657A..87O. doi:10.1051/0004-6361/202040078. eISSN 1432-0746. ISSN 0004-6361.
  9. 1 2 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". Astronomy & Astrophysics. 561: A126. arXiv:1312.3474. Bibcode:2014A&A...561A.126D. doi:10.1051/0004-6361/201220762. eISSN 1432-0746. ISSN 0004-6361.
  10. ↑ 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.
  11. ↑ "HD 175219". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved December 24, 2022.
  12. ↑ 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.
  13. ↑ 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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