Gliese 876 c

Gliese 876 c
Exoplanet List of exoplanets

An artist's impression of Gliese 876 c, depicting it as a Saturn-like gas giant planet
Parent star
Star Gliese 876
Constellation Aquarius
Right ascension (α) 22h 53m 16.73s
Declination (δ) −14° 15′ 49.3″
Apparent magnitude (mV) 10.17
Distance15.20±0.01[1] ly
(4.660±0.004[1] pc)
Spectral type M4V
Mass (m) 0.334 ± 0.030 M☉
Radius (r) 0.36 R☉
Temperature (T) 3350 ± 300 K
Metallicity [Fe/H] 0.05 ± 0.20
Age 0.1 – 5.0 Gyr
Orbital elements
Epoch HJD 2,450,602.093
Semi-major axis(a) 0.129590 ± 0.000024 [2][note 1] AU
Eccentricity (e) 0.25591 ± 0.00093 [2]
Orbital period(P) 30.0881 ± 0.0082 [2] d
Inclination (i) 59 [2]°
Argument of
periastron		 (ω) 48.76 ± 0.70 [2]°
Mean anomaly (M) 294.59 ± 0.94 [2]°
Semi-amplitude (K) 88.34 ± 0.47 [2] m/s
Physical characteristics
Mass(m)0.7142 ± 0.0039 [2][note 1] MJ
Stellar flux(F⊙)0.77 ⊕
Maximum stellar flux(F⊙max)1.40 ⊕
Minimum stellar flux(F⊙min)0.49 ⊕
Discovery information
Discovery date April 4, 2001
Discoverer(s) Marcy et al.
Discovery method Radial velocity
Other detection methods Astrometry
Discovery site California and
Carnegie Planet Search
Discovery status Published
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

Gliese 876 c is an exoplanet orbiting the red dwarf Gliese 876, taking about 30 days to complete an orbit. The planet was discovered in April 2001 and is the third planet in order of increasing distance from its star.

Discovery

At the time of discovery, Gliese 876 was already known to host an extrasolar planet designated Gliese 876 b. In 2001, further analysis of the star's radial velocity revealed the existence of a second planet in the system, which was designated Gliese 876 c.[3] The orbital period of Gliese 876 c was found to be exactly half that of the outer planet, which meant that the radial velocity signature of the second planet was initially interpreted as a higher eccentricity of the orbit of Gliese 876 b.

Orbit and mass

The orbits of the planets of Gliese 876. Gliese 876 c is the second planet from the star.

Gliese 876 c is in a 1:2:4 Laplace resonance with the outer planets Gliese 876 b and Gliese 876 e: for every orbit of planet e, planet b completes two orbits and planet c completes four.[2] This leads to strong gravitational interactions between the planets,[4] causing the orbital elements to change rapidly as the orbits precess.[2][5] This is the second known example of a Laplace resonance, the first being Jupiter's moons Io, Europa and Ganymede.

The orbital semimajor axis is only 0.13 AU, around a third of the average distance between Mercury and the Sun, and is more eccentric than the orbit of any of the major planets of our solar system.[2] Despite this, it is located in the inner regions of the system's habitable zone, since Gliese 876 is such an intrinsically faint star.[6]

A limitation of the radial velocity method used to detect Gliese 876 c is that only a lower limit on the planet's mass can be obtained. This is because the measured mass value depends on the inclination of the orbit, which is not determined by the radial velocity measurements. However, in a resonant system such as Gliese 876, gravitational interactions between the planets can be used to determine the true masses. Using this method, the inclination of the orbit can be determined, revealing the planet's true mass to be 0.72 times that of Jupiter.[2]

Characteristics

Based on its high mass, Gliese 876 c is likely to be a gas giant with no solid surface. Since it was detected indirectly through its gravitational effects on the star, properties such as its radius, composition, and temperature are unknown. Assuming a composition similar to Jupiter and an environment close to chemical equilibrium, the planet is predicted to have a cloudless upper atmosphere.[7]

Gliese 876 c lies at the inner edge of the system's habitable zone. While the prospects for life on gas giants are unknown, it might be possible for a large moon of the planet to provide a habitable environment. Unfortunately tidal interactions between a hypothetical moon, the planet, and the star could destroy moons massive enough to be habitable over the lifetime of the system.[8] In addition it is unclear whether such moons could form in the first place.[9]

This planet, like b and e, has likely migrated inward.[10]

See also

Notes

  1. 1 2 Uncertainties in the planetary masses and semimajor axes do not take into account the uncertainty in the mass of the star.

References

  1. 1 2 Benedict, G. F; et al. (2002). "A Mass for the Extrasolar Planet Gliese 876b Determined from Hubble Space Telescope Fine Guidance Sensor 3 Astrometry and High-Precision Radial Velocities". The Astrophysical Journal. 581 (2): L115–L118. arXiv:astro-ph/0212101. Bibcode:2002ApJ...581L.115B. doi:10.1086/346073.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 Rivera, Eugenio J.; et al. (July 2010). "The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration". The Astrophysical Journal. 719 (1): 890–899. arXiv:1006.4244. Bibcode:2010ApJ...719..890R. doi:10.1088/0004-637X/719/1/890.
  3. ↑ Marcy, Geoffrey W.; et al. (2001). "A Pair of Resonant Planets Orbiting GJ 876". The Astrophysical Journal. 556 (1): 296–301. Bibcode:2001ApJ...556..296M. doi:10.1086/321552.
  4. ↑ Rivera, Eugenio J.; Lissauer, Jack J. (2001). "Dynamical Models of the Resonant Pair of Planets Orbiting the Star GJ 876". The Astrophysical Journal. 558 (1): 392–402. Bibcode:2001ApJ...558..392R. doi:10.1086/322477.
  5. ↑ Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
  6. ↑ Jones, Barrie W.; et al. (2005). "Prospects for Habitable "Earths" in Known Exoplanetary Systems". The Astrophysical Journal. 622 (2): 1091–1101. arXiv:astro-ph/0503178. Bibcode:2005ApJ...622.1091J. doi:10.1086/428108.
  7. ↑ Sudarsky, David; et al. (2003). "Theoretical Spectra and Atmospheres of Extrasolar Giant Planets". The Astrophysical Journal. 588 (2): 1121–1148. arXiv:astro-ph/0210216. Bibcode:2003ApJ...588.1121S. doi:10.1086/374331.
  8. ↑ Barnes, Jason W.; O'Brien, D. P. (2002). "Stability of Satellites around Close-in Extrasolar Giant Planets". The Astrophysical Journal. 575 (2): 1087–1093. arXiv:astro-ph/0205035. Bibcode:2002ApJ...575.1087B. doi:10.1086/341477. (paper incorrectly refers to Gliese 876 b as GJ876c)
  9. ↑ Canup, Robin M.; Ward, William R. (2006). "A common mass scaling for satellite systems of gaseous planets". Nature. 441 (7095): 834–839. Bibcode:2006Natur.441..834C. doi:10.1038/nature04860. PMID 16778883.
  10. ↑ Gerlach, Enrico; Haghighipour, Nader (2012). "Can GJ 876 host four planets in resonance?". arXiv:1202.5865. Bibcode:2012CeMDA.113...35G. doi:10.1007/s10569-012-9408-0.
  • Nemiroff, R.; Bonnell, J., eds. (1998-06-26). "A planet for Gliese 876". Astronomy Picture of the Day. NASA. Retrieved 2008-06-21.
  • "Gliese 876 : THE CLOSEST EXTRASOLAR PLANET". Observatoire de Haute Provence. Retrieved 2008-06-21.

Coordinates: 22h 53m 16.7s, −14° 15′ 49″

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