HD 4391
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Phoenix |
| Right ascension | 00h45m45.5930s[1] |
| Declination | –47° 33′ 07.1438″[1] |
| Apparent magnitude(V) | 5.80[2] |
| Characteristics | |
| Spectral type | G3V[3] |
| B−Vcolor index | +0.64[2] |
| Astrometry | |
| Radial velocity(Rv) | –11.4[4]km/s |
| Proper motion(μ) | RA:183.99[1]mas/yr Dec.:78.81[1]mas/yr |
| Parallax(π) | 65.97 ± 0.39mas[1] |
| Distance | 49.4 ± 0.3ly (15.16 ± 0.09pc) |
| Details | |
| Mass | 1.22 ± 0.04[5]M☉ |
| Surface gravity(logg) | 4.85[5]cgs |
| Temperature | 5,955[5]K |
| Metallicity[Fe/H] | 0.01[5]dex |
| Rotation | 12 days[6] |
| Rotational velocity(vsini) | 3.5[3]km/s |
| Age | 1.2[6]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 4391is atriple star system[8]in theconstellationPhoenixthat is located at a distance of 48.7light yearsfrom theSun.The primary has astellar classificationof G3V, which is aG-type main sequence star.The physical properties of this star are similar to the Sun, making it asolar analog.However, it is believed to have 22% greater mass than the Sun and is only 1.2 billion years old.[5]The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process.[6]
No planet has been detected in orbit around this star,[5]nor does it emit a statistically significantexcess of infrared radiationthat might indicate adebris disk.[9]However, it has two companions that share acommon proper motionthrough space with HD 4391, effectively making it a triple star system. The first, ared dwarfof type M4, lies at anangular separationof 17″ from the primary. The second is a type M5 star at a separation of 49″.[8]
References
[edit]- ^abcdevan Leeuwen, F. (November 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.S2CID18759600.
- ^abJohnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars".Communications of the Lunar and Planetary Laboratory.4:99.Bibcode:1966CoLPL...4...99J.
- ^abTorres, C. A. O.; et al. (December 2006). "Search for associations containing young stars (SACY). I. Sample and searching method".Astronomy and Astrophysics.460(3): 695–708.arXiv:astro-ph/0609258.Bibcode:2006A&A...460..695T.doi:10.1051/0004-6361:20065602.S2CID16080025.
- ^Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Alan Henry Batten; John Frederick Heard (eds.).Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30.University of Toronto: Academic Press, London. p. 57.Bibcode:1967IAUS...30...57E.
- ^abcdefSantos, N. C.; et al. (July 2001). "The metal-rich nature of stars with planets".Astronomy and Astrophysics.373(3): 1019–1031.arXiv:astro-ph/0105216.Bibcode:2001A&A...373.1019S.doi:10.1051/0004-6361:20010648.S2CID119347084.
- ^abcSantos, N. C.; et al. (October 2004). "Beryllium anomalies in solar-type field stars".Astronomy and Astrophysics.425(3): 1013–1027.arXiv:astro-ph/0408109.Bibcode:2004A&A...425.1013S.doi:10.1051/0004-6361:20040510.S2CID17279966.
- ^"HD 4391 -- Pre-main sequence Star".SIMBAD.Centre de Données astronomiques de Strasbourg.Retrieved2010-07-13.
- ^abRaghavan, Deepak; et al. (September 2010). "A Survey of Stellar Families: Multiplicity of Solar-type Stars".The Astrophysical Journal Supplement.190(1): 1–42.arXiv:1007.0414.Bibcode:2010ApJS..190....1R.doi:10.1088/0067-0049/190/1/1.S2CID368553.
- ^Beichman, C. A.; et al. (December 2006). "New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets".The Astrophysical Journal.652(2): 1674–1693.arXiv:astro-ph/0611682.Bibcode:2006ApJ...652.1674B.doi:10.1086/508449.S2CID14207148.
