HD 30432
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Caelum
Right ascension 04h 45m 55.45152s[1]
Declination −39° 21′ 23.8094″[1]
Apparent magnitude (V) 6.04±0.01[2]
Characteristics
Evolutionary stage red giant branch[3]
Spectral type K1 III[4]
B−V color index +1.07[5]
Astrometry
Radial velocity (Rv)−6±4.3[6] km/s
Proper motion (μ) RA: −59.362 mas/yr[1]
Dec.: −20.031 mas/yr[1]
Parallax (π)10.5049 ± 0.0202 mas[1]
Distance310.5 ± 0.6 ly
(95.2 ± 0.2 pc)
Absolute magnitude (MV)+1.10[7]
Details
Mass2.80±0.04[1] M☉
Radius9.55+0.68
−0.64[8] R☉
Luminosity38.9±1.8[9] L☉
Surface gravity (log g)2.76[1] cgs
Temperature4,758±122[10] K
Metallicity [Fe/H]−0.08[11] dex
Rotational velocity (v sin i)<1.3[12] km/s
Age455+45
−46[1] Myr
Other designations
15 G. Caeli[13], CD−39°1624, CPD−39°514, FK5 2355, GC 5821, HD 30432, HIP 22144, HR 1526, SAO 195278[14]
Database references
SIMBADdata

HD 30432, also known as HR 1526, is a solitary, orange hued star located in the southern constellation of Caelum, the chisel. It has an apparent magnitude of 6.04,[2] making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 310 light years distant.[1] It appears to be approaching the Solar System, having a fairly constrained radial velocity of −6 km/s.[6] Eggen (1993) lists it as a member of the old disk population.[11]

HD 30432 has a stellar classification of K1 III, indicating that it is an evolved giant star. It is currently on the red giant branch,[3] fusing a hydrogen shell around an inert helium core. It has 2.8 times the mass of the Sun and is estimated to be 455 million years old.[1] At that age, the star has expanded to 9.5 times the radius of the Sun[8] and now has a cool effective temperature of 4,758 K.[10] Despite the low temperature, HD 30432 shines with a luminosity 39 times that of the Sun from its photosphere.[9] It has a metallicity 16% below solar levels,[11] making it slightly metal deficient. Like most giants, HR 1526 spins slowly, with its projected rotational velocity being lower than 1.3 km/s.[12]

References

  1. 1 2 3 4 5 6 7 8 9 10 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 Cardiel, Nicolás; Zamorano, Jaime; Carrasco, Josep Manel; Masana, Eduard; Bará, Salvador; González, Rafael; Izquierdo, Jaime; Pascual, Sergio; Sánchez de Miguel, Alejandro (23 July 2021). "RGB photometric calibration of 15 million Gaia stars". Monthly Notices of the Royal Astronomical Society. 507 (1): 318–329. arXiv:2107.08734. Bibcode:2021MNRAS.507..318C. doi:10.1093/mnras/stab2124. eISSN 1365-2966. ISSN 0035-8711.
  4. ↑ Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars III: Declinations −40° to −26°. Bibcode:1982mcts.book.....H.
  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. ↑ 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 Allende Prieto, C.; Lambert, D. L. (December 1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: masses, radii and effective temperatures". Astronomy and Astrophysics. 352: 555–562. arXiv:astro-ph/9911002. Bibcode:1999A&A...352..555A. ISSN 0004-6361.
  9. 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.
  10. 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.
  11. 1 2 3 Eggen, O. J. (July 1993). "Evolved GK stars near the sun. I - The old disk population". The Astronomical Journal. 106: 80. Bibcode:1993AJ....106...80E. doi:10.1086/116622.
  12. 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.
  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. ↑ "HR 1526". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 6, 2022.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.