29 Arietis is a triple star[5] system in the northern constellation of Aries. 29 Arietis is the Flamsteed designation. Its annual parallax shift of 34.86±0.13 mas[1] indicates a distance of about 94 light-years (29 parsecs) from Earth. The system is barely visible to the naked eye with an apparent visual magnitude of 6.0; it is 0.02 degree north of the ecliptic.[2] It is moving further from Earth with a heliocentric radial velocity of 9 km/s.[2]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Aries |
| Right ascension | 02h 32m 54.14202s[1] |
| Declination | +15° 02′ 04.3103″[1] |
| Apparent magnitude (V) | 6.00[2] |
| Characteristics | |
| Spectral type | F7 V + G5 V[3] + ? |
| B−V color index | 0.572±0.006[2] |
| Astrometry | |
| Radial velocity (Rv) | 9.1±2.5[2] km/s |
| Proper motion (μ) | RA: −20.557[1] mas/yr Dec.: +50.206[1] mas/yr |
| Parallax (π) | 34.8568 ± 0.1313 mas[1] |
| Distance | 93.6 ± 0.4 ly (28.7 ± 0.1 pc) |
| Absolute magnitude (MV) | 4.2/5.0[4] |
| Orbit[4] | |
| Period (P) | 19.4161±0.0005 d |
| Eccentricity (e) | 0.4096±0.0033 |
| Longitude of the node (Ω) | 179.09±0.44° |
| Periastron epoch (T) | 2,454,101.914±0.018 JD |
| Semi-amplitude (K1) (primary) | 23.36±0.09 km/s |
| Details | |
| 29 Ari A | |
| Mass | 1.14[5] M☉ |
| Radius | 1.59+0.07 −0.05 R☉ |
| Luminosity | 3.27[2] L☉ |
| Surface gravity (log g) | 4.12[6] cgs |
| Temperature | 6,063±114[4] K |
| Metallicity [Fe/H] | 0.09[6] dex |
| Age | 3.0±1.8[4] Gyr |
| 29 Ari B | |
| Mass | 0.88[5] M☉ |
| Temperature | 5,270±170[4] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
The core of the system is formed by a close spectroscopic binary with an angular separation of 3.892 mas,[5] a semimajor axis of 0.15692±0.00086 AU, an orbital period of 19.4 days, and an eccentricity of 0.4.[4] The larger member of this pair has 114% of the mass of the Sun, while its companion has 88% of the Sun's mass. Orbiting the pair at an angular separation of 1.422 arcseconds over a period of 164 years, the tertiary component has 52% of the Sun's mass.[5]
References edit
- ^ a b c d e f 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.
- ^ Lu, W. (April 1986), "The spectroscopic orbit of the double-lined binary 29 ARIETIS", Astronomical Society of the Pacific, Publications, 98: 468–470, Bibcode:1986PASP...98..468L, doi:10.1086/131780.
- ^ a b c d e f Katoh, Noriyuki; et al. (February 2013), "Determination of Orbital Elements of Spectroscopic Binaries Using High-dispersion Spectroscopy", The Astronomical Journal, 145 (2): 12, Bibcode:2013AJ....145...41K, doi:10.1088/0004-6256/145/2/41, 41.
- ^ a b c d e Tokovinin, A.; et al. (May 2006), "Tertiary companions to close spectroscopic binaries", Astronomy and Astrophysics, 450 (2): 681–693, arXiv:astro-ph/0601518, Bibcode:2006A&A...450..681T, doi:10.1051/0004-6361:20054427, S2CID 8899546.
- ^ a b Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID 56118016.
- ^ "29 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-06-02.