32 Aquarii

From Wikipedia, the free encyclopedia
32 Aquarii
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aquarius
Right ascension 22h 04m 47.42197s[1]
Declination −00° 54′ 22.8469″[1]
Apparent magnitude (V) 5.29[2]
Characteristics
Spectral type A5 IV[3] or Am (A5/A9V/F2)[4]
B−V color index 0.231±0.004[2]
Astrometry
Radial velocity (Rv)18.9±4.2[2] km/s
Proper motion (μ) RA: −19.69[5] mas/yr
Dec.: −42.15[5] mas/yr
Parallax (π)14.4329 ± 0.1784[1] mas
Distance226 ± 3 ly
(69.3 ± 0.9 pc)
Absolute magnitude (MV)1.12[2]
Orbit[6]
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[7] M☉
Radius2.97+0.17
−0.07[1] R☉
Luminosity29.4±0.4[1] L☉
Surface gravity (log g)4.11[7] cgs
Temperature7,976±271[7] K
Metallicity [Fe/H]0.26±0.12[8] dex
Rotational velocity (v sin i)9.6[6] km/s
Age465[7] Myr
Other designations
32 Aqr, BD−01°4242, HD 209625, HIP 108991, HR 8410, SAO 145853[9]
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.[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 an 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.
  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.
Retrieved from ""