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HD 13931

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HD 13931
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda[1]
Right ascension 02h 16m 47.37872s[2]
Declination +43° 46′ 22.7862″[2]
Apparent magnitude (V) 7.60[3]
Characteristics
Spectral type G0V[4]
Apparent magnitude (B) 8.237[3]
Apparent magnitude (R) 7.2[5]
Apparent magnitude (I) 6.9[5]
Apparent magnitude (J) 6.452[6]
Apparent magnitude (H) 6.234[6]
Apparent magnitude (K) 6.139[6]
B−V color index 0.640[3]
R−I color index 0.3[5]
Astrometry
Radial velocity (Rv)30.65±0.13[2] km/s
Proper motion (μ) RA: 98.570±0.028 mas/yr[2]
Dec.: −183.408±0.030 mas/yr[2]
Parallax (π)21.1877±0.0251 mas[2]
Distance153.9 ± 0.2 ly
(47.20 ± 0.06 pc)
Absolute magnitude (MV)4.32±0.10[7]
Details[8]
Mass1.04±0.01 M☉
Radius1.18±0.02 R☉
Luminosity1.49±0.01 L☉
Surface gravity (log g)4.3±0.03 cgs
Temperature5868±24 K
Metallicity+0.03±0.04[7]
Rotation~26 days[7]
Age6.8±0.6 Gyr
Other designations
BD+43°459, HD 13931, HIP 10626, SAO 37918, PPM 44946, LTT 10766, NLTT 7491[9]
Database references
SIMBADdata
Exoplanet Archivedata

HD 13931 is a Sun-like star in the northern constellation of Andromeda. It can be viewed with binoculars or a small telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 7.60.[3] This object is located at a distance of 154 light years from the Sun, as determined from its parallax, and is drifting further away with a radial velocity of +31 km/s.[2]

This is an ordinary G-type main-sequence star with a stellar classification of G0V,[4] which indicates it, like the Sun, is generating energy through core hydrogen fusion. It is slightly larger, hotter, brighter, and more massive than the Sun. The metal content is about 8% greater than the Sun, and it has a quiet (magnetically inactive) chromosphere.[7] The star is an estimated 6.8 billion years old and it is spinning with a rotation period of about 26 days[7]

In 2009, a very long-period giant planet, more massive than Jupiter, was found in orbit around the star by measuring changes in the star's radial velocity.[7] This planet takes 12.16 years to orbit the star[10] at the typical distance of 5.32 AU (796 Gm). The planet's eccentricity (0.02) is about the same as Earth's.[11] In 2023, the inclination and true mass of HD 13931 b were measured via astrometry.[10]

According to a 2018 research, HD 13931 is the most promising Solar System analogue known, since it has a star similar to the Sun and a planet with mass and semimajor axis similar to Jupiter. Those characteristics yield a probability almost 75% for the existence of a dynamically stable habitable zone, where an Earth-like planet may exist and sustain life.[12]

The HD 13931 planetary system[11]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 2.8+0.8
−0.6 MJ 		5.32±0.09 4,442+49
−46[10] 		0.02±0.02 100+50
−60° 		—

See also

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References

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  1. ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
  2. ^ a b c d e f 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. ^ a b c d Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  4. ^ a b Grenier, S.; Baylac, M.-O.; Rolland, L.; Burnage, R.; Arenou, F.; Briot, D.; Delmas, F.; Duflot, M.; Genty, V.; Gómez, A. E.; Halbwachs, J.-L.; Marouard, M.; Oblak, E.; Sellier, A. (1999). "Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS". Astronomy and Astrophysics Supplement. 137 (3): 451. Bibcode:1999A&AS..137..451G. doi:10.1051/aas:1999489.
  5. ^ a b c Database entry, VizieR Online Data Catalog: The USNO-B1.0 Catalog (Monet+ 2003), D. G. Monet et al., CDS ID I/284 Accessed on line 2018-11-06.
  6. ^ a b c Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  7. ^ a b c d e f Howard, Andrew W.; et al. (2010). "The California Planet Survey. I. Four New Giant Exoplanets". The Astrophysical Journal. 721 (2): 1467–1481. arXiv:1003.3488. Bibcode:2010ApJ...721.1467H. doi:10.1088/0004-637X/721/2/1467. S2CID 14147776.
  8. ^ Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
  9. ^ "HD 13931". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-14.
  10. ^ a b c Philipot, F.; Lagrange, A.-M.; et al. (January 2023). "Updated characterization of long-period single companion by combining radial velocity, relative astrometry, and absolute astrometry". Astronomy & Astrophysics. 670: A65. arXiv:2301.01263. Bibcode:2023A&A...670A..65P. doi:10.1051/0004-6361/202245396. S2CID 255393653.
  11. ^ a b Van Zandt, Judah; Gilbert, Gregory J.; Petigura, Erik A.; Giacalone, Steven; Howard, Andrew W.; Handley, Luke B. (2026-04-02). "A Smooth Transition from Giant Planets to Brown Dwarfs from the Radial Occurrence Distribution". The Astronomical Journal. 171 (5): 267. arXiv:2511.18758. Bibcode:2026AJ....171..267V. doi:10.3847/1538-3881/ae5102. ISSN 0004-6256.
  12. ^ Agnew, Matthew T.; Maddison, Sarah T.; Horner, Jonathan (2018). "Properties of the single Jovian planet population and the pursuit of Solar system analogues". Monthly Notices of the Royal Astronomical Society. 477 (3): 3646. arXiv:1804.06547. Bibcode:2018MNRAS.477.3646A. doi:10.1093/mnras/sty868. S2CID 119232995.