Astronomy:HD 57197

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Short description: Star in the constellation Puppis
HD 57197
Puppis constellation map.svg
Red circle.svg
Location of HD 57197 (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Puppis
Right ascension  07h 18m 04.24932s[1]
Declination −43° 59′ 12.4288″[1]
Apparent magnitude (V) 5.84±0.01[2]
Characteristics
Spectral type B8 II/III[3]
U−B color index −0.47[4]
B−V color index −0.14[4]
Astrometry
Radial velocity (Rv)13±10[5] km/s
Proper motion (μ) RA: −9.483[1] mas/yr
Dec.: −5.396[1] mas/yr
Parallax (π)5.1842 ± 0.0442[1] mas
Distance629 ± 5 ly
(193 ± 2 pc)
Absolute magnitude (MV)−0.43[6]
Details
Mass3.08[7] M☉
Radius3.9±0.2[8] R☉
Luminosity234[9] L☉
Surface gravity (log g)3.77[7] cgs
Temperature12,596[9] K
Metallicity [Fe/H]−0.18[7] dex
Age220[10] Myr
Other designations
M Puppis, CD−43°3093, CPD−43°1430, GC 9732, HD 57197, HIP 35347, HR 2789, SAO 218618[11]
Database references
SIMBADdata

HD 57197, also known as M Puppis or HR 2789, is a suspected astrometric binary[12] located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 5.84,[2] making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, the system is estimated to be 629 light years away from the Solar System.[1] The value is poorly constrained, but it appears to be receding with a heliocentric radial velocity of 13 km/s.[5] At its current distance, HD 57197's brightness is diminished by 0.3 magnitudes due to interstellar dust.[13] It has an absolute magnitude of -0.43.[6]

The visible component has a stellar classification of B8 II/III, indicating that it is an evolved B-type star with the blended luminosity class of a bright giant and a giant star. HD 57197 is estimated to be 220 million years old,[10] enough time for it to expand to 3.9 times the Sun's radius.[8] It has 3.08 times the mass of the Sun[7] and radiates 234 times the luminosity of the Sun from its photosphere at an effective temperature of 12,596 K,[9] giving it a bluish-white hue. Based on its extinction in the Gaia passband, it has an iron abundance 66% that of the Sun.[7] This makes HD 57197 metal deficent.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 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. ↑ 4.0 4.1 Cousins, A. W. J.; Lagerweij, H. C. (1970). "Comparison Stars for Long Period Variables and RY Sagittarii". Monthly Notes of the Astronomical Society of South Africa 29: 7. ISSN 0024-8266. Bibcode: 1970MNSSA..29....7C. 
  5. ↑ 5.0 5.1 Kharchenko, N.V.; Scholz, R.-D.; Piskunov, A.E.; Röser, S.; Schilbach, E. (November 2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten 328 (9): 889–896. doi:10.1002/asna.200710776. ISSN 0004-6337. Bibcode: 2007AN....328..889K. 
  6. ↑ 6.0 6.1 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Anders, F. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  8. ↑ 8.0 8.1 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. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  9. ↑ 9.0 9.1 9.2 McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (21 November 2012). "Fundamental parameters and infrared excesses of Hipparcos stars: Parameters and IR excesses from Hipparcos". Monthly Notices of the Royal Astronomical Society 427 (1): 343–357. doi:10.1111/j.1365-2966.2012.21873.x. ISSN 0035-8711. Bibcode: 2012MNRAS.427..343M. 
  10. ↑ 10.0 10.1 Gontcharov, G. A. (November 2012). "Spatial distribution and kinematics of OB stars". Astronomy Letters 38 (11): 694–706. doi:10.1134/S1063773712110035. ISSN 1063-7737. Bibcode: 2012AstL...38..694G. 
  11. ↑ "HD 57197". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+57197. 
  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. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  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. doi:10.1093/mnras/stx2219. ISSN 0035-8711. Bibcode: 2017MNRAS.472.3805G. 
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