Summary
Chi Geminorum (χ Gem) is a binary star system in the constellation Gemini, near the eastern border with Cancer. It can be viewed with the naked eye on a dark night, having an apparent visual magnitude of 4.98.[2] Based upon an annual parallax shift of 12.73 mas,[1] it is located roughly 260 light years from the Sun.
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Gemini |
| Right ascension | 08h 03m 31.08225s[1] |
| Declination | +27° 47′ 39.6243″[1] |
| Apparent magnitude (V) | 4.98[2] |
| Characteristics | |
| Spectral type | K2 III[3] |
| U−B color index | +1.09[2] |
| B−V color index | +1.14[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.83±0.17[4] km/s |
| Proper motion (μ) | RA: −25.52[1] mas/yr Dec.: -31.89[1] mas/yr |
| Parallax (π) | 12.73 ± 0.90 mas[1] |
| Distance | 260 ± 20 ly (79 ± 6 pc) |
| Absolute magnitude (MV) | 0.461[5] |
| Orbit[6] | |
| Period (P) | 2,437.8d |
| Eccentricity (e) | 0.06 |
| Periastron epoch (T) | 2442894.5 ± 10.0 JD |
| Argument of periastron (ω) (secondary) | 264° |
| Semi-amplitude (K1) (primary) | 5.2 km/s |
| Details[4] | |
| Mass | 1.83[3] M☉ |
| Radius | 14 R☉ |
| Luminosity | 79 L☉ |
| Surface gravity (log g) | 2.5 cgs |
| Temperature | 4,560±5 K |
| Metallicity [Fe/H] | 0.03 dex |
| Rotational velocity (v sin i) | 3.8 km/s |
| Age | 1.92[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The two components of this system form a spectroscopic binary with an orbital period of 2,437.8 days and an eccentricity of 0.06.[6] The primary component is a K-type giant star with a stellar classification of K2 III.[3] This is a candidate mild Barium star with the slight overabundance most likely acquired through accretion from what is now a white dwarf companion.[8] The primary has an estimated 1.83[3] times the mass of the Sun and has expanded to 14 times the Sun's radius.[4] The effective temperature of the outer atmosphere is 4,560 K, from whence it radiates 79 times the solar luminosity.[4] It has a leisurely projected rotational velocity of 3.8[4] km/s and is around two billion years old.[3]
References edit
- ^ a b c d e f 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- ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b c d e f Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 23, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114, 88.
- ^ a b c d e Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209.
- ^ Soubiran, C.; et al. (March 2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID 16602121.
- ^ a b Pourbaix, D.; et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy & Astrophysics, 424 (2): 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
- ^ "* chi Gem". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-12-09.
{{cite web}}: CS1 maint: postscript (link) - ^ Yang, Guo-Chao; et al. (January 2016), "Chemical abundance analysis of 19 barium stars", Research in Astronomy and Astrophysics, 16 (1): 019, arXiv:1602.08704, Bibcode:2016RAA....16...19Y, doi:10.1088/1674-4527/16/1/019, S2CID 14474857, 19.