42 Aquarii
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Aquarius |
| Right ascension | 22h 16m 48.04643s[1] |
| Declination | −12° 49′ 53.1673″[1] |
| Apparent magnitude (V) | 5.34[2] |
| Characteristics | |
| Evolutionary stage | giant |
| Spectral type | K1 III[3] |
| B−V color index | 1.132±0.001[2] |
| Astrometry | |
| Radial velocity (Rv) | +13.0±4.2[2] km/s |
| Proper motion (μ) | RA: +1.89[4] mas/yr Dec.: +5.03[4] mas/yr |
| Parallax (π) | 7.3032 ± 0.1451 mas[1] |
| Distance | 447 ± 9 ly (137 ± 3 pc) |
| Absolute magnitude (MV) | −0.93[2] |
| Details | |
| Mass | 3.14±0.27[5] M☉ |
| Radius | 11.24+0.23 −0.32[1] R☉ |
| Luminosity | 69.950±3.907[1] L☉ |
| Surface gravity (log g) | 2.90[6] cgs |
| Temperature | 4,980+71 −51[1] K |
| Metallicity [Fe/H] | +0.00±0.04[2] dex |
| Rotational velocity (v sin i) | 3.43[6] km/s |
| Age | 470±150[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
42 Aquarii is a single[8] star located 447 light years away from the Sun in the zodiac constellation of Aquarius. 42 Aquarii is its Flamsteed designation. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.34.[2] This object is moving further from the Sun with a heliocentric radial velocity of around +13 km/s.[2]
This object is an evolved giant star with a stellar classification of K1 III,[3] most likely (82% chance) on the horizontal branch.[5] It is around 470[5] million years old with a projected rotational velocity of 3.4 km/s.[6] The star has over three[5] times the mass of the Sun and has expanded to 11[1] times the Sun's radius. It is radiating 70[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,980 K.[1]
References
[edit]- ^ a b c d e f g h i 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 g 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.
- ^ a b Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
- ^ 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 Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy & Astrophysics, 574: A116, arXiv:1412.4634, Bibcode:2015A&A...574A.116R, doi:10.1051/0004-6361/201322360, hdl:10722/215277, S2CID 59334290.
- ^ a b c Hekker, S.; Meléndez, J. (2007), "Precise radial velocities of giant stars. III. Spectroscopic stellar parameters", Astronomy and Astrophysics, 475 (3): 1003, arXiv:0709.1145, Bibcode:2007A&A...475.1003H, doi:10.1051/0004-6361:20078233, S2CID 10436552.
- ^ "42 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-16.
- ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
