French
DeutschGliese 777
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 20h 03m 37.405s[1] |
| Declination | +29° 53′ 48.492″[1] |
| Apparent magnitude (V) | +5.73[2] / +14.40 |
| Characteristics | |
| Spectral type | G6IV[2] / M4.5V |
| Astrometry | |
| Radial velocity (Rv) | −45.34±0.12[1] km/s |
| Proper motion (μ) | RA: 683.196 mas/yr[1] Dec.: -525.501 mas/yr[1] |
| Parallax (π) | 62.4865 ± 0.34 mas[1] |
| Distance | 52.2 ± 0.3 ly (16.00 ± 0.09 pc)[1] |
| Details[3] | |
| Mass | 0.93±0.02 M☉ |
| Radius | 1.142±0.009 R☉ |
| Luminosity | 1.114±0.007 L☉ |
| Surface gravity (log g) | 4.292±0.012 cgs |
| Temperature | 5,557±22 K |
| Metallicity [Fe/H] | 0.17±0.04 dex |
| Age | 4.79[2] Gyr |
| Other designations | |
Gliese 777 | |
| HD 190360: BD+29°3872, Gliese 777 A, HIP 98767, HR 7670, LHS 3510. | |
| G 125-55: Gliese 777 B, LHS 3509. | |
| Database references | |
| SIMBAD | AB |
| A | |
| B | |
| Exoplanet Archive | data |
| ARICNS | data |
| data2 | |
Gliese 777, often abbreviated as Gl 777 or GJ 777, is a binary star approximately 52 light-years away in the constellation of Cygnus. The system is also a binary star system made up of two stars and possibly a third. As of 2005, two extrasolar planets are known to orbit the primary star.
Stellar components
[edit]The primary star of the system (catalogued as Gliese 777 A) is a yellow subgiant, a Sun-like star that is ceasing fusing hydrogen in its core. The star is much older than the Sun, about 6.7 billion years old. It is 4% less massive than the Sun. It is also rather metal-rich, having about 70% more "metals" (elements heavier than helium) than the Sun, which is typical for stars with extrasolar planets.
The secondary star (Gliese 777 B) is a distant, dim red dwarf star orbiting the primary at a distance of 3,000 astronomical units (0.047 light years). One orbit takes at least tens of thousands of years to complete. The star itself may be a binary, the secondary being a very dim red dwarf. Not much information is available on the star system.
Planetary system
[edit]In 2002, a discovery of a long-period, wide-orbiting, planet (Gliese 777 b) was announced by the Geneva extrasolar planet search team.[4] The planet was estimated to orbit in a circular path with low orbital eccentricity, but that estimate was increased with later measurements (e=0.36).[5] Initially therefore, the planet was believed to be a true "Jupiter-twin" but was later redefined as being more like an "eccentric Jupiter", with a mass of at least 1.5 times Jupiter and about the same size. In 2021, the true mass of Gliese 777 Ab was measured via astrometry.[6]
In 2005, further observation of the star showed another amplitude with a period of 17.1 days.[5] The mass of this second planet (Gliese 777 c) was only 18 times more than Earth, or about the same as Neptune, indicating it was one of the smallest planets discovered at the time. It too was initially thought to be on a circular orbital path that with later measurements turned out to be not the case.
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | ≥0.0600 ± 0.0076 MJ | 0.1304 ± 0.0075 | 17.1110 ± 0.0048 | 0.237 ± 0.082 | — | — |
| b | 1.8 ± 0.2 MJ | 3.9 ± 0.2 | 2,854 ± 13 | 0.340 ± 0.018 | 80.2 ± 23.2° | — |
There was a METI message sent to Gliese 777. It was transmitted from Eurasia's largest radar, 70-meter Eupatoria Planetary Radar. The message was named Cosmic Call 1; it was sent on July 1, 1999, and it will arrive at Gliese 777 in April 2051.[8]
See also
[edit]References
[edit]- ^ a b c d e f 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 Ligi, R.; et al. (February 2016), "Radii, masses, and ages of 18 bright stars using interferometry and new estimations of exoplanetary parameters", Astronomy & Astrophysics, 586: 23, arXiv:1511.03197, Bibcode:2016A&A...586A..94L, doi:10.1051/0004-6361/201527054, S2CID 15941645, A94.
- ^ Karovicova, I.; White, T. R.; Nordlander, T.; Casagrande, L.; Ireland, M.; Huber, D. (13 September 2021). "Fundamental stellar parameters of benchmark stars from CHARA interferometry -- II. Dwarf stars". Astronomy & Astrophysics. 658: A47. arXiv:2109.06203. doi:10.1051/0004-6361/202141833. ISSN 0004-6361.
- ^ Naef, D.; et al. (2003). "The ELODIE survey for northern extra-solar planets II. A Jovian planet on a long-period orbit around GJ 777 A". Astronomy and Astrophysics. 410 (3): 1051–1054. arXiv:astro-ph/0306586. Bibcode:2003A&A...410.1051N. doi:10.1051/0004-6361:20031341. S2CID 14853884.
- ^ a b Vogt, Steven S.; et al. (2005). "Five New Multicomponent Planetary Systems" (PDF). The Astrophysical Journal. 632 (1): 638–658. Bibcode:2005ApJ...632..638V. doi:10.1086/432901. S2CID 16509245. Archived (PDF) from the original on 2018-07-22. Retrieved 2020-09-05.
- ^ a b Feng, Fabo; Butler, R Paul; Jones, Hugh R A.; Phillips, Mark W.; Vogt, Steven S.; Oppenheimer, Rebecca; Holden, Bradford; Burt, Jennifer; Boss, Alan P. (2021). "Optimized modelling of Gaia–Hipparcos astrometry for the detection of the smallest cold Jupiter and confirmation of seven low-mass companions". Monthly Notices of the Royal Astronomical Society. 507 (2): 2856–2868. arXiv:2107.14056. Bibcode:2021MNRAS.507.2856F. doi:10.1093/mnras/stab2225.
- ^ Wright, J. T.; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems". The Astrophysical Journal. 693 (2): 1084–1099. arXiv:0812.1582. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084. S2CID 18169921.
- ^ (in Russian) http://www.cplire.ru/rus/ra&sr/VAK-2004.html Archived 2019-05-30 at the Wayback Machine
External links
[edit]- Extrasolar Planet Interactions Archived 2016-05-05 at the Wayback Machine by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
