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HD 290327

HD 290327
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Right ascension 05h 23m 21.5637s[1]
Declination –02° 16′ 39.433″[1]
Apparent magnitude (V) 8.99[2]
Characteristics
Spectral type G5IV[3] or G8V[4]
Apparent magnitude (B) 9.751[2]
Apparent magnitude (J) 7.683±0.026[2]
Apparent magnitude (H) 7.404±0.047[2]
Apparent magnitude (K) 7.271±0.027[2]
B−V color index 0.761±0.033[2]
Astrometry
Radial velocity (Rv)+29.52±0.17[1] km/s
Proper motion (μ) RA: 32.478(19) mas/yr[1]
Dec.: −97.255(13) mas/yr[1]
Parallax (π)17.9008 ± 0.0196 mas[1]
Distance182.2 ± 0.2 ly
(55.86 ± 0.06 pc)
Absolute magnitude (MV)5.24[2]
Details[5]
Mass0.86±0.01 M☉
Radius0.95±0.02 R☉
Luminosity0.747±0.004 L☉
Surface gravity (log g)4.41±0.01 cgs
Temperature5,525±20 K
Metallicity [Fe/H]−0.11 dex
Rotational velocity (v sin i)1.44±1.0[4] km/s
Age11.8±1.2 Gyr
Other designations
BD−02°128, HD 290327, HIP 25191, SAO 132049, PPM 175811[6]
Database references
SIMBADdata
Exoplanet Archivedata

HD 290327 is a single[7] star in the equatorial constellation of Orion. It has a yellow hue with an apparent visual magnitude of 8.99,[2] which is too faint to be viewed with the naked eye. Parallax measurements provide a distance estimate of 182 light years from the Sun. It is drifting away with a radial velocity of +29.5 km/s,[1] having come to within 124 light-years around a million years ago.[2]

Kazanasmas (1973) found a stellar classification of G5IV[3] for this object, matching a G-type star that is evolving along the subgiant branch. It was later given a class of G8V,[4] suggesting it is instead a G-type main-sequence star. This object is nearly twelve[5] billion years old and is spinning slowly with a projected rotational velocity of 1.4 km/s.[4] The star has 86% of the mass of the Sun and 95% of the Sun's radius. It is radiating 75% of the luminosity of the Sun from its photosphere at an effective temperature of 5,525 K. The metallicity is sub-solar,[5] meaning it has a lower abundance of elements other than hydrogen and helium compared to the Sun.

In 2009, a gas giant planet was found in orbit around the star. It is orbiting at a distance of around 3.4 AU with a period of 6.7 years.[4]

The HD 290327 planetary system[4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥ 2.54+0.17
−0.14 MJ 		3.43+0.20
−0.12 		2443+205
−117 		0.08+0.08
−0.03 		— —

See also

References

  1. ^ 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.
  2. ^ a b c d e f g h i 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. S2CID 119257644.
  3. ^ a b Kazanasmas, M. S. (1973). "Catalogue of magnitudes, color indices, spectral and luminosity classes of stars in Orion". Abastumanskaya Astrofiz. Obs., Byull. 44: 175. Bibcode:1973AbaOB..44..175K.
  4. ^ a b c d e f Naef, Dominique; Mayor, Michel; Lo Curto, Gaspare; Bouchy, François; Lovis, Christophe; Moutou, Claire; Benz, Willy; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Bonfils, Xavier; Delfosse, Xavier; Forveille, Thierry; Hébrard, Guillaume; Mordasini, Christoph; Perrier, Christian; Boisse, Isabelle; Sosnowska, Danuta (2010). "The HARPS Search for Southern Extrasolar Planets XXIII. 8 Planetary Companions to Low-activity Solar-type Stars". Astronomy and Astrophysics. 523: A15. arXiv:1008.4600. Bibcode:2010A&A...523A..15N. doi:10.1051/0004-6361/200913616. S2CID 118845989.
  5. ^ a b c 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.
  6. ^ "HD 290327". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-18.
  7. ^ Ginski, C.; et al. (2016). "A lucky imaging multiplicity study of exoplanet host stars – II". Monthly Notices of the Royal Astronomical Society. 457 (2): 2173–2191. arXiv:1601.01524. Bibcode:2016MNRAS.457.2173G. doi:10.1093/mnras/stw049.


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