HD 4391

Last updated
HD 4391
Phoenix constellation map.svg
Red circle.svg
Location of HD 4391 (circled in red)
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix [1]
Right ascension 00h 45m 45.5929s [2]
Declination −47° 33′ 07.143″ [2]
Apparent magnitude  (V)5.80 [3]
Characteristics
A
Evolutionary stage main sequence [2]
Spectral type G3V [4]
B−V color index +0.64 [3]
Astrometry
A
Radial velocity (Rv)−11.4 [5] km/s
Proper motion (μ)RA: +183.635 [2] mas/yr
Dec.: +79.015 [2] mas/yr
Parallax (π)66.4509±0.0446  mas [2]
Distance 49.08 ± 0.03  ly
(15.05 ± 0.01  pc)
Absolute magnitude  (MV)+4.90 [1]
Details
A
Mass 1.08 [6]   M☉
Radius 0.92 [6]   R☉
Luminosity 0.92 [6]   L☉
Surface gravity (log g)4.55 [6]   cgs
Temperature 5,916 [6]   K
Metallicity [Fe/H]−0.06 [7]   dex
Rotation 12 days [8]
Rotational velocity (v sin i)3.5 [4]  km/s
Age 800 [7]   Myr
Other designations
CD−48 176, HD 4391, GJ 1021, HIP 3583, HR  209, SAO 215232 [9]
Database references
SIMBAD data

HD 4391 is a quadruple star system [10] in the constellation Phoenix that is located at a distance of 49.1 light years from the Sun. The primary has a stellar classification of G3V, which is a G-type main sequence star. The physical properties of this star are similar to the Sun, making it a solar analog. However, it is believed to have 6% greater mass than the Sun [6] and is only 800 million years old. [7] The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process. [8]

No planet has been detected in orbit around this star, [11] nor does it emit a statistically significant excess of infrared radiation that might indicate a debris disk. [12] However, it has three companions that share a common proper motion through space with HD 4391, effectively making it a quadruple star system. HD 4391 B, a pair of red dwarfs of combined spectrum M4, lies at an angular separation of 17″ from the primary, with the two components designated Ba and Bb. HD 4391 C is a type M5 star at a separation of 49″. [13] [10] The close red dwarf pair are also sometimes designated HD 4391 B and HD 4391 C, with the outer component being named HD 4391 D. [14] [15]

References

  1. 1 2 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. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  4. 1 2 Torres, 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. S2CID   16080025.
  5. ↑ 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.
  6. 1 2 3 4 5 6 Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 .
  7. 1 2 3 Casali, G.; et al. (2020). "The Gaia-ESO survey: The non-universality of the age-chemical-clocks-metallicity relations in the Galactic disc". Astronomy and Astrophysics. 639: A127. arXiv: 2006.05763 . Bibcode:2020A&A...639A.127C. doi:10.1051/0004-6361/202038055.
  8. 1 2 Santos, 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. S2CID   17279966.
  9. ↑ "HD 4391 -- Pre-main sequence Star". SIMBAD. Centre de Données astronomiques de Strasbourg . Retrieved 2010-07-13.
  10. 1 2 Fuhrmann, Klaus; Chini, Rolf (2018-06-01). "Nearby Gaia DR2 Companions". Research Notes of the AAS. 2 (2): 56. Bibcode:2018RNAAS...2...56F. doi: 10.3847/2515-5172/aacc72 . ISSN   2515-5172.
  11. ↑ Santos, 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. S2CID   119347084.
  12. ↑ 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. S2CID   14207148.
  13. ↑ Raghavan, 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. S2CID   368553.
  14. ↑ "HD 4391C". SIMBAD . Centre de données astronomiques de Strasbourg.
  15. ↑ "HD 4391D". SIMBAD . Centre de données astronomiques de Strasbourg.
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