HD 290327
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 184 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]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h 23m 21.56388s[1] |
| Declination | –02° 16′ 39.4338″[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±0.21[1] km/s |
| Proper motion (μ) | RA: +32.312[1] mas/yr Dec.: −97.224[1] mas/yr |
| Parallax (π) | 17.6913 ± 0.0461[1] mas |
| Distance | 184.4 ± 0.5 ly (56.5 ± 0.1 pc) |
| Absolute magnitude (MV) | 5.24[2] |
| Details[5] | |
| Mass | 0.86±0.01 M☉ |
| Radius | 0.95±0.02 R☉ |
| Luminosity | 0.747±0.004 L☉ |
| Surface gravity (log g) | 4.41±0.01 cgs |
| Temperature | 5,525±20 K |
| Metallicity [Fe/H] | −0.11 dex |
| Rotational velocity (v sin i) | 1.44±1.0[4] km/s |
| Age | 11.8±1.2 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
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]
| 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
- List of extrasolar planets
References
- Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- 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.
- 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.
- Naef, D.; et al. (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.
- 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.
- "HD 290327". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-18.
- 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.