HD 169830
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 27m 49.48500s[1] |
| Declination | –29° 49′ 00.7008″[1] |
| Apparent magnitude (V) | +5.90[2] |
| Characteristics | |
| Spectral type | F7V[3] |
| B−V color index | 0.517±0.004[2] |
| Variable type | “None” |
| Astrometry | |
| Radial velocity (Rv) | −17.271±0.0004[4] km/s |
| Proper motion (μ) | RA: −0.341[1] mas/yr Dec.: 16.103[1] mas/yr |
| Parallax (π) | 27.1461 ± 0.1469 mas[1] |
| Distance | 120.1 ± 0.7 ly (36.8 ± 0.2 pc) |
| Absolute magnitude (MV) | +3.08[2] |
| Details[5] | |
| Mass | 1.4 M☉ |
| Radius | 1.84 R☉ |
| Luminosity | 4.63[6] L☉ |
| Surface gravity (log g) | 4.06 cgs |
| Temperature | 6,300±50[6] K |
| Metallicity [Fe/H] | 0.15 dex |
| Rotation | 8.3 d[7] |
| Rotational velocity (v sin i) | 3.83 km/s |
| Age | 4.95[8] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
HD 169830 is a star in the southern constellation of Sagittarius. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.90.[2] The star is located at a distance of 120 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −17.3 km/s,[4] and is predicted to come as close as 20.7 ly (6.4 pc) in 2.08 million years.[10] HD 169830 is known to be orbited by two large Jupiter-like exoplanets.
This is an F-type main-sequence star[6] with a stellar classification of F7V.[3] It is 3.83[8] billion years old and chromospherically inactive[8] with a slow rotation rate,[8] having a projected rotational velocity of 3.83 km/s.[5] This star is 40% more massive and 84% larger than the Sun. Combining the mass and radius makes the surface gravity only 41% that of the Sun. It is radiating 4.6[6] times the luminosity of the Sun from its photosphere at an effective temperature of 6,300 K.[6]
A candidate stellar companion, designated component B, lies at an angular separation of 11″ along a position angle of 265°.[11]
Planetary system
On April 15, 2000, the Geneva Extrasolar Planet Search Team announced the discovery of a minimum mass 3 MJ planet in a 226-day orbit.[12][6] Three years later on June 30, 2003, the same team, using the same method, discovered a minimum mass 3.5 MJ second planet orbiting the star.[7] In 2022, the inclination and true mass of HD 169830 c were measured via astrometry.[13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥2.956+0.070 −0.069 MJ |
0.8130+0.0083 −0.0084 |
225.789+0.074 −0.081 |
0.306+0.012 −0.013 |
— | — |
| c | 7.669+1.937 −2.755 MJ |
3.075+0.132 −0.146 |
1818.8+5.7 −6.4 |
0.246+0.022 −0.018 |
24.469+12.739 −7.205° |
— |
See also
References
- ^ a b c d e 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 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 Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ 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 Fischer, Debra A.; Valenti, Jeff (2005). "The Planet‐Metallicity Correlation". The Astrophysical Journal. 622 (2): 1102. Bibcode:2005ApJ...622.1102F. doi:10.1086/428383.
- ^ a b c d e f Naef, D.; et al. (2001). "The CORALIE survey for southern extrasolar planets V. 3 new extrasolar planets". Astronomy and Astrophysics. 375 (1): 205–218. arXiv:astro-ph/0106255. Bibcode:2001A&A...375..205N. doi:10.1051/0004-6361:20010841. S2CID 16606841.
- ^ a b Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
- ^ a b c d Saffe, C.; et al. (2005). "On the Ages of Exoplanet Host Stars". Astronomy and Astrophysics. 443 (2): 609–626. arXiv:astro-ph/0510092. Bibcode:2005A&A...443..609S. doi:10.1051/0004-6361:20053452. S2CID 11616693.
- ^ "HD 169830". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-03-16.
- ^ Bailer-Jones, C.A.L.; Rybizki, J; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
- ^ Raghavan, Deepak; et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv:astro-ph/0603836. Bibcode:2006ApJ...646..523R. doi:10.1086/504823. S2CID 5669768.
- ^ "Exoplanets Galore!" (Press release). Garching, Germany: European Southern Observatory. April 15, 2000. Retrieved December 30, 2012.
- ^ 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). arXiv:2208.12720. Bibcode:2022arXiv220812720F. doi:10.3847/1538-4365/ac7e57.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ "HD 169830". NASA Exoplanet Archive. Retrieved 2 September 2022.
External links
- "Notes for star HD 169830". The Extrasolar Planets Encyclopaedia. Retrieved 2006-04-14.
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
