HD 30177
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Dorado[1] |
| Right ascension | 04h 41m 54.374s[2] |
| Declination | −58° 01′ 14.73″[2] |
| Apparent magnitude (V) | 8.41[1] |
| Characteristics | |
| Evolutionary stage | main sequence[3] |
| Spectral type | G8V[4] |
| B−V color index | 0.773±0.015[1] |
| Astrometry | |
| Radial velocity (Rv) | 62.697±0.0013[5] km/s |
| Proper motion (μ) | RA: 66.303±0.023 mas/yr[2] Dec.: −11.795±0.024 mas/yr[2] |
| Parallax (π) | 18.0190 ± 0.0195 mas[2] |
| Distance | 181.0 ± 0.2 ly (55.50 ± 0.06 pc) |
| Absolute magnitude (MV) | 4.72±0.09[3] |
| Details[6] | |
| Mass | 1.053±0.023 M☉ |
| Radius | 1.019±0.034 R☉ |
| Luminosity | 1.04±0.01[7] L☉ |
| Surface gravity (log g) | 4.417±0.034 cgs |
| Temperature | 5,607±47 K |
| Metallicity [Fe/H] | 0.39±0.05 dex |
| Rotation | ~45 d |
| Rotational velocity (v sin i) | 2.96±0.50[8] km/s |
| Age | 4.8±1.5 Gyr[7] 2.525±1.954[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 30177 is a single star with a pair of orbiting exoplanets in the southern constellation Dorado. Based on parallax measurements, it is located at a distance of 181 light years from the Sun. It has an absolute magnitude of 4.72,[3] but at that distance the star is too faint to be viewed by the naked eye with an apparent visual magnitude of 8.41.[1] The star is drifting further away with a radial velocity of 62.7 km/s.[5]
The spectrum of HD 30177 matches a late G-type main-sequence star with a stellar classification of G8V.[4] It is a yellow dwarf with a mass and radius similar to the Sun that is fusing hydrogen in its core. The chromosphere shows a negligible level of magnetic activity.[3] The abundance of iron, an indicator of the star's metallicity, is more than double the Sun's. It is radiating a similar luminosity to the Sun from its photosphere at an effective temperature of 5,607 K.[6]
A 2024 multiplicity survey, using astrometry from the Gaia spacecraft, identified a proper motion companion to HD 30177. This co-moving companion is a red dwarf star, around 10% the mass of the Sun, is located at 780" from HD 30177 with a position angle of 188°. The angular distance translates to an observed separation of 43,300 astronomical units.[10]
Planetary system
The Anglo-Australian Planet Search team announced the discovery of HD 30177 b, which has a minimum mass 8 times that of Jupiter, on June 13, 2002. The scientific paper describing the discovery was published in The Astrophysical Journal in 2003.[11][3] A second massive gas giant planet was later discovered in an approximately 32 year orbit.[12] In 2022, the inclination and estimated mass of both planets were measured via astrometry.[13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 8.403+1.241 −0.489 MJ |
3.604+0.135 −0.147 |
6.884+0.014 −0.012 |
0.207+0.012 −0.017 |
85.393+14.354 −18.742° |
— |
| c | 6.150+1.308 −0.341 MJ |
10.258+0.535 −0.480 |
33.088+1.596 −1.207 |
0.039+0.005 −0.013 |
98.016+16.025 −24.235° |
— |
See also
References
- ^ a b c d 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.
- ^ a b c d 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.
- ^ a b c d e Tinney, C. G.; et al. (2003). "Four New Planets Orbiting Metal-enriched Stars". The Astrophysical Journal. 587 (1): 423–428. arXiv:astro-ph/0207128. Bibcode:2003ApJ...587..423T. doi:10.1086/368068.
- ^ a b Houk, Nancy; Cowley, Anne P. (1975). University of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars. Declinations −90° to −53°. Vol. 1. Department of Astronomy, University of Michigan. Bibcode:1975mcts.book.....H. ISBN 978-0-8357-0331-4.
- ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID 52952408.
- ^ a b c Barbato, D.; et al. (August 2018). "Exploring the realm of scaled solar system analogues with HARPS". Astronomy & Astrophysics. 615: 21. arXiv:1804.08329. Bibcode:2018A&A...615A.175B. doi:10.1051/0004-6361/201832791. S2CID 119099721. A175.
- ^ a b 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.
- ^ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
- ^ "HD 30177". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-22.
- ^ González-Payo, J.; Caballero, J. A.; Gorgas, J.; Cortés-Contreras, M.; Gálvez-Ortiz, M.-C.; Cifuentes, C. (2024-07-29). "Multiplicity of stars with planets in the solar neighbourhood". arXiv:2407.20138 [astro-ph.SR].
- ^ Tinney, Chris (2007-09-07). "AAPS Discovered Planets". Anglo-Australian Planet Search. University of New South Wales. Retrieved 2018-04-17.
- ^ Wittenmyer, Robert A.; et al. (2017). "The Anglo-Australian Planet Search. XXV. A Candidate Massive Saturn Analog Orbiting HD 30177". The Astronomical Journal. 153 (4). 167. arXiv:1612.02072. Bibcode:2017AJ....153..167W. doi:10.3847/1538-3881/aa5f17.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
External links
- "Notes for star HD 30177". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007. Retrieved 2008-08-29.
