Summary
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]
| 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 mas[1] |
| Distance | 226 ± 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 | |
| Mass | 1.69[7] M☉ |
| Radius | 2.97+0.17 −0.07[1] R☉ |
| Luminosity | 29.4±0.4[1] L☉ |
| Surface gravity (log g) | 4.11[7] cgs |
| Temperature | 7,976±271[7] K |
| Metallicity [Fe/H] | 0.26±0.12[8] dex |
| Rotational velocity (v sin i) | 9.6[6] km/s |
| Age | 465[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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 edit
- ^ 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.
- ^ 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.
- ^ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "32 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-16.
- ^ 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.
- ^ 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.