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32 Aquarii is a binary star system in the zodiac constellation of Aquarius. 32 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.29.[2] This system is moving away from the Earth with a heliocentric radial velocity of +19 km/s,[2] and is a possible member of the corona of the Ursa Major flow.[10]

This is a single-lined spectroscopic binary with an (assumed) circular orbit having a period of only 7.8 days. It has an a sin i value of 0.777 Gm (0.00519 AU),[6] where a is the semimajor axis and i is the orbital inclination. Since the sine function can be no larger than one, this provides a lower bound on the true semimajor axis of their orbit.

The primary component is a metallic-line (Am) star[6] with the calcium K line of an A3 star, the hydrogen lines of an F1 star, and the metal lines of an F2 star.[4] It is a sharp-lined, slowly rotating star[11] with a projected rotational velocity of 9.6 km/s[6] and is about 465 million years old.[7] The star has 1.69[7] times the mass of the Sun and three[1] times the Sun's radius. It is radiating 29[1] times the luminosity of the Sun from its photosphere at an effective temperature of 7,976 K.[7]

References

  1. ^ a b c d e f g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e f 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, S2CID 119257644.
  3. ^ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  4. ^ a b Abt, Helmut A. (January 2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–118, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117, S2CID 122811461.
  5. ^ a b van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  6. ^ a b c d e Carrier, F.; et al. (August 2007), "A search for solar-like oscillations in the Am star HD 209625", Astronomy and Astrophysics, 470 (3): 1009–1012, arXiv:0706.0803, Bibcode:2007A&A...470.1009C, doi:10.1051/0004-6361:20067022, S2CID 15812804.
  7. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  8. ^ Hui-Bon-Hoa, A. (June 2000), "Metal abundances of field A and Am stars", Astronomy and Astrophysics Supplement, 144 (2): 203–209, Bibcode:2000A&AS..144..203H, doi:10.1051/aas:2000207.
  9. ^ "32 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-16.
  10. ^ Chupina, N. V.; et al. (June 2006), "Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars", Astronomy and Astrophysics, 451 (3): 909–916, Bibcode:2006A&A...451..909C, doi:10.1051/0004-6361:20054009.
  11. ^ Kocer, D.; et al. (July 1987), "Optical region elemental abundance analyses of B and A stars. VII - The metallic-lined star 32 Aquarii", Astronomy and Astrophysics Supplement Series, 70 (1): 49–56, Bibcode:1987A&AS...70...49K.
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