Astronomy:HD 4391

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Short description: Triple star system in the constellation of Phoenix
HD 4391
Location of HD 4391 (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
Distance49.08 ± 0.03 ly
(15.05 ± 0.01 pc)
Absolute magnitude (MV)+4.90[1]
Details
A
Mass1.08[6] M☉
Radius0.92[6] R☉
Luminosity0.92[6] L☉
Surface gravity (log g)4.55[6] cgs
Temperature5,916[6] K
Metallicity [Fe/H]−0.06[7] dex
Rotation12 days[8]
Rotational velocity (v sin i)3.5[4] km/s
Age800[7] Myr
Other designations
CD−48 176, HD 4391, GJ 1021, HIP 3583, HR 209, SAO 215232[9]
Database references
SIMBADdata

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. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 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. ↑ 4.0 4.1 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. doi:10.1051/0004-6361:20065602. Bibcode: 2006A&A...460..695T. 
  5. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". in Alan Henry Batten. University of Toronto: Academic Press, London. p. 57. Bibcode: 1967IAUS...30...57E. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Stassun, Keivan G. et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S. 
  7. ↑ 7.0 7.1 7.2 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. doi:10.1051/0004-6361/202038055. Bibcode: 2020A&A...639A.127C. 
  8. ↑ 8.0 8.1 Santos, N. C. et al. (October 2004). "Beryllium anomalies in solar-type field stars". Astronomy and Astrophysics 425 (3): 1013–1027. doi:10.1051/0004-6361:20040510. Bibcode: 2004A&A...425.1013S. 
  9. ↑ "HD 4391 -- Pre-main sequence Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+4391. 
  10. ↑ 10.0 10.1 Fuhrmann, Klaus; Chini, Rolf (2018-06-01). "Nearby Gaia DR2 Companions". Research Notes of the AAS 2 (2): 56. doi:10.3847/2515-5172/aacc72. ISSN 2515-5172. Bibcode: 2018RNAAS...2...56F. 
  11. ↑ Santos, N. C. et al. (July 2001). "The metal-rich nature of stars with planets". Astronomy and Astrophysics 373 (3): 1019–1031. doi:10.1051/0004-6361:20010648. Bibcode: 2001A&A...373.1019S. 
  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. doi:10.1086/508449. Bibcode: 2006ApJ...652.1674B. 
  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. doi:10.1088/0067-0049/190/1/1. Bibcode: 2010ApJS..190....1R. 
  14. ↑ "HD 4391C". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+4391C. 
  15. ↑ "HD 4391D". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+4391D. 



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