HD 99015

Last updated
HD 99015
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Chamaeleon [1]
Right ascension 11h 21m 56.89166s [2]
Declination −77° 36′ 30.1275″ [2]
Apparent magnitude  (V)6.42±0.01 [3]
Characteristics
Evolutionary stage main sequence [2]
Spectral type A5 V [4]
U−B color index +0.11 [5]
B−V color index +0.20 [5]
Astrometry
Radial velocity (Rv)−5.9±2.5 [6] km/s
Proper motion (μ)RA: −79.623 mas/yr [2]
Dec.: −8.231 mas/yr [2]
Parallax (π)13.3992±0.0202  mas [2]
Distance 243.4 ± 0.4  ly
(74.6 ± 0.1  pc)
Absolute magnitude  (MV)+2.08 [1]
Details
Mass 1.87±0.06 [7]   M☉
Radius 1.83±0.09 [8]   R☉
Luminosity 12.0+0.3
−0.2 [2]   L☉
Surface gravity (log g)4.2±0.1 [9]   cgs
Temperature 7,859±124 [9]   K
Metallicity [Fe/H]+0.15 [10]   dex
Age 854 [11]   Myr
Other designations
31 G. Chamaeleontis [12] , CD−76°495, CPD−76°662, GC 15628, HD 99015, HIP 55497, HR 4397, SAO 256832 [13]
Database references
SIMBAD data

HD 99015, also known as HR 4397 or rarely 31 G. Chamaeleontis, is a solitary white-hued star located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude of 6.42, [3] placing it near the limit for naked eye visibility even in ideal conditions. The object is located relatively close at a distance of 243 light years [2] and is drifting closer with a somewhat constrained heliocentric radial velocity of −5.9  km/s . [6] At its current distance, HD 99015's brightness is diminished by 0.31 magnitudes due to interstellar dust. [14] It has an absolute magnitude of +2.08. [1]

This is an ordinary A-type main-sequence star with a stellar classification of A5 V. [4] However, Nancy Houk and A. P. Cowley gave a class of A5 III/IV, [15] indicating that it is instead an evolved A-type star with the luminosity class of a subgiant and giant star. It has 1.87 times the mass of the Sun [7] and 1.83 times the solar radius. [8] It radiates 12 times the luminosity of the Sun [2] from its photosphere at an effective temperature of 7,859  K . [9] HD 99015 is somewhat metal enriched ([Fe/H] = +0.15 [10] ) and is estimated to be 854 million years old. [11]

References

  1. 1 2 3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters . 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 7 8 9 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.
  3. 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.
  4. 1 2 Oblak, E.; Chareton, M. (September 1981). "On the Estimation of Photometric Spectral Types". Astronomy and Astrophysics Supplement Series. 45: 459. Bibcode:1981A&AS...45..459O. ISSN   0365-0138.
  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 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 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.
  8. 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.
  9. 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. hdl: 1721.1/124721 . S2CID   166227927.
  10. 1 2 Netopil, Martin (4 May 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society. 469 (3): 3042–3055. arXiv: 1705.00883 . Bibcode:2017MNRAS.469.3042N. doi: 10.1093/mnras/stx1077 . eISSN   1365-2966. ISSN   0035-8711.
  11. 1 2 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 . eISSN   1562-6873. ISSN   1063-7737.
  12. ↑ 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.
  13. ↑ "HD 99015". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved January 30, 2023.
  14. ↑ 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.
  15. ↑ Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations −90° to −53°. Bibcode:1975mcts.book.....H.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.