Gliese 777

Last updated
Gliese 777
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cygnus
Right ascension 20h 03m 37.41s [1]
Declination +29° 53′ 48.5″ [1]
Apparent magnitude  (V)+5.73 [2] / +14.40
Characteristics
Spectral type G6IV [2] / M4.5V
B−V color index 0.749[ citation needed ]
Astrometry
Radial velocity (Rv)-45.3[ citation needed ] km/s
Proper motion (μ)RA: 683.94 ± 0.22 [1]   mas/yr
Dec.: -524.70 ± 0.27 [1]   mas/yr
Parallax (π)63.06 ± 0.34  mas [1]
Distance 51.7 ± 0.3  ly
(15.86 ± 0.09  pc)
Absolute magnitude  (MV)+4.70[ citation needed ] / +13.39
Details [2]
Mass 0.82±0.17  M☉
Radius 1.061±0.013  R☉
Luminosity 1.127±0.019  L☉
Surface gravity (log g)4.3±0.09  cgs
Temperature 5,781±37  K
Metallicity [Fe/H]0.2  dex
Age 6.7[ citation needed ]  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
Extrasolar Planets
Encyclopaedia 		data

Gliese 777, often abbreviated as Gl 777 or GJ 777, is a yellow subgiant 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.

Contents

Stellar components

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

In 2002, a discovery of a long-period, wide-orbiting, planet (Gliese 777 b) was announced by the Geneva extrasolar planet search team. [3] 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). [4] 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. [5]

In 2005, further observation of the star showed another amplitude with a period of 17.1 days. [4] 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.

The HD 190360 (Gliese 777 A) planetary system [6] [5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c ≥0.0600 ± 0.0076  MJ 0.1304 ± 0.007517.1110 ± 0.00480.237 ± 0.082——
b 1.8 ± 0.2  MJ 3.9 ± 0.22,854 ± 130.340 ± 0.01880.2 ± 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. [7]

See also

Related Research Articles

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References

  1. 1 2 3 4 5 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600. Vizier catalog entry
  2. 1 2 3 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.
  3. ↑ 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.
  4. 1 2 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.
  5. 1 2 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.
  6. ↑ 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.
  7. ↑ (in Russian) http://www.cplire.ru/rus/ra&sr/VAK-2004.html Archived 2019-05-30 at the Wayback Machine
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