32 Aquarii

32 Aquarii
Observation data
Epoch J2000.0      Equinox ICRS
Constellation Aquarius[1]
Right ascension 22h 04m 47.42197s[2]
Declination −00° 54′ 22.8469″[2]
Apparent magnitude (V) 5.29[1]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A5 IV[4] or Am (A5/A9V/F2)[5]
B−V color index 0.231±0.004[1]
Astrometry
Radial velocity (Rv)18.9±4.2[1] km/s
Proper motion (μ) RA: −19.69[6] mas/yr
Dec.: −42.15[6] mas/yr
Parallax (π)14.4329±0.1784 mas[2]
Distance226 ± 3 ly
(69.3 ± 0.9 pc)
Absolute magnitude (MV)1.12[1]
Orbit[7]
Period (P)7.83238±0.00002 d
Eccentricity (e)0
Periastron epoch (T)53,420.2304±0.0001 HJD
Argument of periastron (ω)
(secondary)		0°
Semi-amplitude (K1)
(primary)		7.2150±0.4 km/s
Details
Mass1.69[8] M☉
Radius2.97+0.17
−0.07[2] R☉
Luminosity29.4±0.4[2] L☉
Surface gravity (log g)4.11[8] cgs
Temperature7,976±271[8] K
Metallicity [Fe/H]0.26±0.12[9] dex
Rotational velocity (v sin i)9.6[7] km/s
Age465[8] Myr
Other designations
32 Aqr, BD−01°4242, HD 209625, HIP 108991, HR 8410, SAO 145853[10]
Database references
SIMBADdata

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.[1] This system is moving away from the Earth with a heliocentric radial velocity of +19 km/s,[1] and is a possible member of the corona of the Ursa Major flow.[11]

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),[7] 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[7] with the calcium K line of an A3 star, the hydrogen lines of an F1 star, and the metal lines of an F2 star.[5] It is a sharp-lined, slowly rotating star[12] with a projected rotational velocity of 9.6 km/s[7] and is about 465 million years old.[8] The star has 1.69[8] times the mass of the Sun and three[2] times the Sun's radius. It is radiating 29[2] times the luminosity of the Sun from its photosphere at an effective temperature of 7,976 K.[8]

References

  1. 1 2 3 4 5 6 7 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 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.
  3. ↑ 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.
  4. ↑ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  5. 1 2 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.
  6. 1 2 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.
  7. 1 2 3 4 5 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.
  8. 1 2 3 4 5 6 7 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.
  9. ↑ 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.
  10. ↑ "32 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-16.
  11. ↑ 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.
  12. ↑ 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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