Astronomy:HD 30669
| Observation data Epoch J2000.0 Equinox (celestial coordinates) | |
|---|---|
| Constellation | Caelum[1] |
| Right ascension | 04h 48m 28.48538s[2] |
| Declination | −28° 25′ 09.4617″[2] |
| Apparent magnitude (V) | 9.11±0.01[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | G8/K0 V[4] |
| B−V color index | +0.82[3] |
| Astrometry | |
| Radial velocity (Rv) | 65.7±0.4[5] km/s |
| Proper motion (μ) | RA: +237.591[2] mas/yr Dec.: +50.927[2] mas/yr |
| Parallax (π) | 17.2896 ± 0.0127[2] mas |
| Distance | 188.6 ± 0.1 ly (57.84 ± 0.04 pc) |
| Absolute magnitude (MV) | +5.35[1] |
| Details | |
| Mass | 0.92±0.03[6] M☉ |
| Radius | 0.91±0.04[7] R☉ |
| Luminosity | 0.71[8] L☉ |
| Surface gravity (log g) | 4.43±0.06[9] cgs |
| Temperature | 5,353±100[9] K |
| Metallicity [Fe/H] | +0.13[10] dex |
| Rotational velocity (v sin i) | <1.7[7] km/s |
| Age | 7.25±4.64[11] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 30669 is a yellowish-orange hued star located in the southern constellation Caelum, the chisel. It has an apparent magnitude of 9.11,[3] making it readily visible in small telescopes but not to the naked eye. The object is relatively close at a distance of 189 light-years, based on parallax measurements from Gaia DR3.[2] Its distance from the Solar System is rapidly increasing, having a heliocentric radial velocity of 66 km/s.[5]
Characteristics
HD 30669 has a stellar classification of G8/K0 V[4] — a main sequence star with the characteristics of a star with a class of G8 or K0. It has alternatively been given a class of G9 V. It has 92% the mass of the Sun[6] and 91% its radius.[7] The object radiates 71% the luminosity of the Sun[8] from its photosphere at an effective temperature of 5,353 K[9] from its photosphere. Like most planetary hosts, HD 30669 is metal enriched, having a metallicity 35% above solar levels.[10] The star is extremely chromopsherically inactive and is estimated to be 7 1⁄4 billion years old.[11]
Planetary system
In 2015, C. Motou and colleagues discovered a long period exoplanet orbiting the star during a HARPS survey. It has nearly half the mass of Jupiter and it takes over 4 1⁄2 years to revolve HD 30669 in a slightly eccentric orbit.[7]
A candidate second planet was identified in a 2026 study using HARPS-N. This would be a super-Neptune on an eccentric orbit closer to the star, with a period of 150 days. Despite the eccentric orbits of both planets, dynamical simulations show that the two-planet system is stable.[13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| .01[13] (unconfirmed) | ≥28.7±3.5 M⊕ | 0.5 | 149.9±0.2 | 0.496+0.088 −0.097 |
— | — |
| b[7] | ≥0.47±0.06 MJ | 2.69±0.08 | 1684±61 | 0.33±0.06[13] | — | — |
References
- ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H.
- ↑ 4.0 4.1 Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars III: Declinations −40° to −26°. Bibcode: 1982mcts.book.....H.
- ↑ 5.0 5.1 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G.
- ↑ 6.0 6.1 Gomes da Silva, J.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Campante, T. L.; Figueira, P.; Bossini, D.; Delgado-Mena, E. et al. (February 2021). "Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample". Astronomy & Astrophysics 646: A77. doi:10.1051/0004-6361/202039765. ISSN 0004-6361. Bibcode: 2021A&A...646A..77G.
- ↑ 7.0 7.1 7.2 7.3 7.4 Moutou, C.; Lo Curto, G.; Mayor, M.; Bouchy, F.; Benz, W.; Lovis, C.; Naef, D.; Pepe, F. et al. (26 March 2015). "The HARPS search for southern extra-solar planets". Astronomy & Astrophysics 576: A48. doi:10.1051/0004-6361/201424965. ISSN 0004-6361. Bibcode: 2015A&A...576A..48M.
- ↑ 8.0 8.1 Loyd, R. O. Parke; Shkolnik, Evgenya L.; Schneider, Adam C.; Richey-Yowell, Tyler; Barman, Travis S.; Peacock, Sarah; Pagano, Isabella (2020). "Current Population Statistics do Not Favor Photoevaporation over Core-powered Mass Loss as the Dominant Cause of the Exoplanet Radius Gap". The Astrophysical Journal 890 (1): 23. doi:10.3847/1538-4357/ab6605. Bibcode: 2020ApJ...890...23L.
- ↑ 9.0 9.1 9.2 Aguilera-Gómez, Claudia; Ramírez, Iván; Chanamé, Julio (June 2018). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy & Astrophysics 614: A55. doi:10.1051/0004-6361/201732209. ISSN 0004-6361. Bibcode: 2018A&A...614A..55A.
- ↑ 10.0 10.1 Mortier, A.; Santos, N. C.; Sousa, S.; Israelian, G.; Mayor, M.; Udry, S. (March 2013). "On the functional form of the metallicity-giant planet correlation". Astronomy & Astrophysics 551: A112. doi:10.1051/0004-6361/201220707. ISSN 0004-6361. Bibcode: 2013A&A...551A.112M.
- ↑ 11.0 11.1 Pace, G. (22 February 2013). "Chromospheric activity as age indicator". Astronomy & Astrophysics 551: L8. doi:10.1051/0004-6361/201220364. ISSN 0004-6361. Bibcode: 2013A&A...551L...8P.
- ↑ "HD 30669". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+30669.
- ↑ 13.0 13.1 13.2 Ruggieri, A. et al. (July 2026). "The GAPS Programme with HARPS-N at TNG LXXVII. Occurrence rates of small close-in planets in the presence of cold Jupiters". Astronomy & Astrophysics.
 |  |
