HD_169830 Latitude and Longitude:
Sky map 18h 27m 49.4838s, −29° 49′ 00.715″
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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]
Distance120.1 ± 0.7  ly
(36.8 ± 0.2  pc)
Absolute magnitude (MV)+3.08 [2]
Details [5]
Mass1.4  M☉
Radius1.84  R☉
Luminosity4.63 [6]  L☉
Surface gravity (log g)4.06  cgs
Temperature6,300±50 [6]  K
Metallicity [Fe/H]0.15  dex
Rotation8.3  d [7]
Rotational velocity (v sin i)3.83 km/s
Age4.95 [8]  Gyr
Other designations
CD−29°14965, Gaia DR2 4048037707717866880, GC 25175, HD 169830, HIP 90485, HR 6907, SAO 186838, GSC 06869-01277, 2MASS J18274949-2949007 [9]
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]

The HD 169830 planetary system [14] [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

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  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.
  5. ^ 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ "HD 169830". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-03-16.
  10. ^ 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.
  11. ^ 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.
  12. ^ "Exoplanets Galore!" (Press release). Garching, Germany: European Southern Observatory. April 15, 2000. Retrieved December 30, 2012.
  13. ^ 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.
  14. ^ "HD 169830". NASA Exoplanet Archive. Retrieved 2 September 2022.

External links


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