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HD 30177 is an 8th magnitude star located approximately 182 light-years (56 parsecs) away in the constellation Dorado. The star is a yellow dwarf, a type of yellow star that fuses hydrogen in its core. Since if this star is a late G-type, it is cooler and less massive than the Sun, but larger in radius. It is 1.8 times older than the Sun. This star system contains two known extrasolar planets.

HD 30177
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Dorado
Right ascension 04h 41m 54.37378s[1]
Declination −58° 01′ 14.7277″[1]
Apparent magnitude (V) 8.41
Characteristics
Spectral type G8V
Astrometry
Radial velocity (Rv)62.63±0.12[1] km/s
Proper motion (μ) RA: 66.303±0.023 mas/yr[1]
Dec.: −11.795±0.024 mas/yr[1]
Parallax (π)18.0190 ± 0.0195 mas[1]
Distance181.0 ± 0.2 ly
(55.50 ± 0.06 pc)
Absolute magnitude (MV)4.72
Details[2]
Mass1.053±0.023 M☉
Radius1.54±0.03 R☉[3]
1.019±0.034[2] R☉
Luminosity1.04 ± 0.01[3] L☉
Surface gravity (log g)4.417±0.034 cgs
Temperature5,607±47 K
Metallicity [Fe/H]0.39±0.05 dex
Rotation~45 d
Age4.8±1.5 Gyr[3]
2.525±1.954[2] Gyr
Other designations
CD−58°984, HIP 21850, SAO 233633, 2MASS J04415438-5801146[4]
Database references
SIMBADdata

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.[5][6] A second massive gas giant planet was later discovered in an approximately 32 year orbit.[7] In 2022, the inclination and true mass of both planets were measured via astrometry.[8]

The HD 30177 planetary system[8]
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


  1. Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  2. 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.
  3. 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.
  4. "HD 30177". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-22.
  5. Tinney, Chris (2007-09-07). "AAPS Discovered Planets". Anglo-Australian Planet Search. University of New South Wales. Retrieved 2018-04-17.
  6. 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.
  7. 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.
  8. 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). arXiv:2208.12720. Bibcode:2022arXiv220812720F. doi:10.3847/1538-4365/ac7e57.


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[de] HD 30177

HD 30177 ist ein etwa 172 Lichtjahre entfernter Hauptreihenstern der Spektralklasse G8 im Sternbild Doradus. Er besitzt eine scheinbare Helligkeit von 8,4 mag.
- [en] HD 30177


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