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HD 177830 is a 7th magnitude binary star system located approximately 205 light-years away in the constellation of Lyra. The primary star is slightly more massive than the Sun, but cooler being a type K star. Therefore, it is a subgiant clearly more evolved than the Sun. In visual light it is four times brighter than the Sun, but because of its distance, about 205 light years, it is not visible to the unaided eye. With binoculars it should be easily visible.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 19h 05m 20.7732s[1] |
| Declination | +25° 55′ 14.372″[1] |
| Apparent magnitude (V) | 7.175 |
| Characteristics | |
| Spectral type | K0IV[2]/M4V[3] |
| Astrometry | |
| Radial velocity (Rv) | −71.86 ± 0.06[4] km/s |
| Proper motion (μ) | RA: −41.228±0.024[1] mas/yr Dec.: −52.587±0.032[1] mas/yr |
| Parallax (π) | 15.94 ± 0.37 mas[1] |
| Distance | 205 ± 5 ly (63 ± 1 pc) |
| Details | |
| Mass | 1.48[5] M☉ |
| Radius | 2.99[5] R☉ |
| Surface gravity (log g) | 4.03[5] cgs |
| Temperature | 4948[5] K |
| Metallicity [Fe/H] | 0.55 ± 0.03[6] dex |
| Rotational velocity (v sin i) | 2.54[5] km/s |
| Age | 4.4 ± 2.2[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The primary star is known to have two extrasolar planets orbiting around it.
Stellar system
The secondary star is a Red dwarf star orbiting at a distance of 100 to 200 AU with a likely period of roughly 800 years.[3]
Planetary system
On November 1, 1999,[8] the discovery of a planet HD 177830 b was announced by the California and Carnegie Planet Search team using the very successful radial velocity method and an analysis on data released by the team performed by amateur astronomer Peter Jalowiczor along with two other planets. This planet is nearly 50% more massive than Jupiter (MJ) and takes 407 days to orbit the star in an extremely circular orbit.[2] In 2000 a group of scientists proposed, based on preliminary Hipparcos astrometrical satellite data, that the orbital inclination of HD 177830 b is as little as 1.3°. If that was the case, the planet would have a mass of 67 MJ, making it a brown dwarf instead of a planet. However, it is very unlikely that the planet would have such orbit. Furthermore, brown dwarfs with short orbits around solar-mass (M☉) stars are exceedingly rare (the so-called "brown dwarf desert") making the claim even more unlikely.
On November 17, 2010, the discovery of a second planet HD 177830 c was announced along with four other planets. The planet has 50% the mass of Saturn and takes 111 days to orbit the star in a very eccentric orbit. This planet is in a near 4:1 resonance with the outer planet.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | ≥0.15 ± 0.03 MJ | 0.5137 ± 0.0006 | 110.9 ± 0.3 | 0.3495 ± 0.0002 | — | — |
| b | ≥1.49 ± 0.03 MJ | 1.2218 ± 0.0008 | 406.6 ± 0.4 | 0.009 ± 0.004 | — | — |
See also
- List of extrasolar planets
References
- Brown, A. G. A; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID 1828208.Gaia Data Release 1 catalog entry
- Vogt, Steven S.; et al. (2000). "Six New Planets from the Keck Precision Velocity Survey". The Astrophysical Journal. 536 (2): 902–914. arXiv:astro-ph/9911506. Bibcode:2000ApJ...536..902V. doi:10.1086/308981. S2CID 119375519.
- Roberts Jr., Lewis C.; et al. (2015). "Know the Star, Know the Planet. V. Characterization of the Stellar Companion to the Exoplanet Host Star HD 177830". The Astronomical Journal. 150 (4): 103. arXiv:1507.07913. Bibcode:2015AJ....150..103R. doi:10.1088/0004-6256/150/4/103. S2CID 51812235.
- Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; Artur de la Villarmois, E.; Chavero, C.; Gómez, M.; Mauas, P. J. D. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
- Fischer, Debra A.; Valenti, Jeff (2005). "The Planet‐Metallicity Correlation". The Astrophysical Journal. 622 (2): 1102. Bibcode:2005ApJ...622.1102F. doi:10.1086/428383.
- Meschiari, Stefano; et al. (2011). "The Lick-Carnegie Survey: Four New Exoplanet Candidates". The Astrophysical Journal. 727 (2): 117. arXiv:1011.4068. Bibcode:2011ApJ...727..117M. doi:10.1088/0004-637X/727/2/117. S2CID 59065004.
- "HD 177830 -- Double or multiple star". SIMBAD Astronomical Database. Centre de données astronomiques de Strasbourg. Retrieved 2014-10-11.
- "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. November 1, 1999. Retrieved December 19, 2017.
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На других языках
[de] HD 177830
HD 177830 ist ein etwa 190 Lichtjahre von der Erde entfernter Unterriese der Spektralklasse K0. Er besitzt eine scheinbare Helligkeit von 7,2 mag. HD 177830 hat einen spektroskopischen Begleiter mit der systematischen Bezeichnung HD 177830 b, bei dem es sich um einen Exoplaneten oder einen Braunen Zwerg handeln könnte. Das Objekt hat eine Umlaufperiode von ca. 400 Tagen und eine Mindestmasse von nur etwa 1,3 Jupitermassen sowie eine große Halbachse von ca. 1 Astronomischen Einheit. Es wurde von Vogt et al. entdeckt.- [en] HD 177830
[ru] HD 177830
HD 177830 — звезда в созвездии Лиры на расстоянии около 192 световых лет от нас. Вокруг звезды обращается, как минимум, одна планета.Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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