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Gliese 876 b

August 24, 2023

Gliese 876 b is an exoplanet orbiting the red dwarf Gliese 876. It completes one orbit in approximately 61 days. Discovered in June 1998, Gliese 876 b was the first planet to be discovered orbiting a red dwarf.

Gliese 876 b
An artist's impression of Gliese876 b
Discovery[1][2][3]
Discovered byCalifornia and Carnegie Planet Search Team and independently by the Geneva Extrasolar Planet Search Team
Discovery siteLick, Keck, Haute-Provence and La Silla Observatories
Discovery dateJune 22, 1998
Doppler spectroscopy
Orbital characteristics[4]
Epoch 2,450,602.09311 BJD
0.218627±0.000017 AU
Eccentricity0.0325+0.0016
−0.0017
61.1057±0.0074 d
340.6+4.4
−4 º
Inclination53.06±0.85 º[note 1]
35.5+4.1
−4.4 º
Semi-amplitude211.57+0.3
−0.29 m/s
StarGliese 876
Physical characteristics[4]
Mass845.2+9.5
−9.4 M🜨[note 2]
Temperature194 K (−79 °C; −110 °F)[5]

Discovery

Gliese 876 b was initially announced by Geoffrey Marcy on June 22, 1998 at a symposium of the International Astronomical Union in Victoria, British Columbia, Canada. The discovery was made using data from the Keck and Lick observatories.[3][6] Only 2 hours after his announcement, he was shown an e-mail from the Geneva Extrasolar Planet Search team confirming the planet. The Geneva team used telescopes at the Haute-Provence Observatory in France and the European Southern Observatory in La Serena, Chile.[3][2] Like the majority of early extrasolar planet discoveries it was discovered by detecting variations in its star's radial velocity as a result of the planet's gravity. This was done by making sensitive measurements of the Doppler shift of the spectral lines of Gliese 876. It was the first discovered of four known planets in the Gliese 876 system.[7][1][2][8][9]

Characteristics

Mass, radius, and temperature

 
An artist's impression of Gliese 876 b as an enormous Jupiter-like planet with a hypothetical satellite system.

Given the planet's high mass, it is likely that Gliese 876 b is a gas giant with no solid surface. Since the planet has only been 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, it is predicted that the atmosphere of Gliese 876 b is cloudless, though cooler regions of the planet may be able to form water clouds.[10]

A limitation of the radial velocity method used to detect Gliese 876 b is that only a lower limit on the planet's mass can be obtained. This lower limit is around 1.93 times the mass of Jupiter.[8] The true mass depends on the inclination of the orbit, which in general is unknown. However, because Gliese 876 is only 15 light years from Earth Benedict et al. (2002) were able to use one of the Fine Guidance Sensors on the Hubble Space Telescope to detect the astrometric wobble created by Gliese 876 b.[11] This constituted the first unambiguous astrometric detection of an extrasolar planet.[7] Their analysis suggested that the orbital inclination is 84°±6° (close to edge-on).[11] In the case of Gliese 876 b, modelling the planet-planet interactions from the Laplace resonance shows that the actual inclination of the orbit is 59°, resulting in a true mass of 2.2756 times the mass of Jupiter.[7]

The equilibrium temperature of Gliese 876 b, is estimated to be around 194 K (−79 °C; −110 °F).[5]

This planet, like c and e, has likely migrated inward.[12]

Host star

Main article: Gliese 876

The planet orbits a (M-type) star named Gliese 876. The star has a mass of 0.33 M☉ and a radius of around 0.36 R☉. It has a surface temperature of 3350 K and is 2.55 billion years old. In comparison, the Sun is about 4.6 billion years old[13] and has a surface temperature of 5778 K.[14]

Orbit

 
The orbits of the planets of Gliese 876. Gliese 876 b is the third planet from the star.

Gliese 876 b is in a 1:2:4 Laplace resonance with the inner planet Gliese 876 c and the outer planet Gliese 876 e: in the time it takes planet e to complete one orbit, planet b completes two and planet c completes four. This is the second known example of a Laplace resonance, the first being Jupiter's moons Io, Europa and Ganymede.[7] As a result, the orbital elements of the planets change fairly rapidly as they dynamically interact with one another.[15] The planet's orbit has a low eccentricity, similar to the planets in the Solar System. The semimajor axis of the orbit is only 0.208 AU, less than that of Mercury in the Solar System.[7] However Gliese 876 is such a faint star that this puts it in the outer part of the habitable zone.[16]

Future habitability

See also: Habitability of red dwarf systems and Habitability of natural satellites

Gliese 876 b currently lies beyond the outer edge of the habitable zone but because Gliese 876 is a slowly evolving main-sequence red dwarf its habitable zone is very slowly moving outwards and will continue to do so for trillions of years. Therefore, Gliese 876 b will, in trillions of years time, lie inside Gliese 876's habitable zone, as defined by the ability of an Earth-mass planet to retain liquid water at its surface, and remain there for at least 4.6 billion years.[17] While the prospects for life on a gas giant are unknown, large moons may be able to support a habitable environment. Models of tidal interactions between a hypothetical moon, the planet and the star suggest that large moons should be able to survive in orbit around Gliese 876 b for the lifetime of the system.[18] On the other hand, it is unclear whether such moons could form in the first place.[19] However, the large mass of the gas giant may make it more likely for larger moons to form.[citation needed]

For a stable orbit the ratio between the moon's orbital period Ps around its primary and that of the primary around its star Pp must be < 1/9, e.g. if a planet takes 90 days to orbit its star, the maximum stable orbit for a moon of that planet is less than 10 days.[20][21] Simulations suggest that a moon with an orbital period less than about 45 to 60 days will remain safely bound to a massive giant planet or brown dwarf that orbits 1 AU from a Sun-like star.[22] In the case of Gliese 876 b, the orbital period would have to be no greater than a week (7 days) in order to have a stable orbit.

Tidal effects could also allow the moon to sustain plate tectonics, which would cause volcanic activity to regulate the moon's temperature[23][24] and create a geodynamo effect which would give the satellite a strong magnetic field.[25]

To support an Earth-like atmosphere for about 4.6 billion years (the age of the Earth), the moon would have to have a Mars-like density and at least a mass of 0.07 MEarth.[26] One way to decrease loss from sputtering is for the moon to have a strong magnetic field that can deflect stellar wind and radiation belts. NASA's Galileo's measurements hints large moons can have magnetic fields; it found that Jupiter's moon Ganymede has its own magnetosphere, even though its mass is only 0.025 MEarth.[22]

See also

Notes

  1. ^ The inclination assumes the planets in the system are coplanar, long-term orbital stability simulations strongly favor low mutual inclinations.
  2. ^ Uncertainties in the planetary masses and semimajor axes do not take into account the uncertainty in the mass of the star.

References

  1. ^ a b Marcy, Geoffrey W.; et al. (1998). "A Planetary Companion to a Nearby M4 Dwarf, Gliese 876". The Astrophysical Journal Letters. 505 (2): L147–L149. arXiv:astro-ph/9807307. Bibcode:1998ApJ...505L.147M. doi:10.1086/311623.
  2. ^ a b c Delfosse, Xavier; Forveille, Thierry; Mayor, Michel; Perrier, Christian; Naef, Dominique; Queloz, Didier (1998). "The closest extrasolar planet. A giant planet around the M4 dwarf GL 876". Astronomy and Astrophysics. 338: L67–L70. arXiv:astro-ph/9808026. Bibcode:1998A&A...338L..67D.
  3. ^ a b c "Astronomers find planet orbiting nearby star" (Press release). W. M. Keck Observatory. 1998-06-22. from the original on 2018-09-24. Retrieved 2018-09-23.
  4. ^ a b Millholland, Sarah; et al. (2018). "New Constraints on Gliese 876—Exemplar of Mean-motion Resonance". The Astronomical Journal. 155 (3). Table 4. arXiv:1801.07831. Bibcode:2018AJ....155..106M. doi:10.3847/1538-3881/aaa894.
  5. ^ a b "Archived copy". from the original on 2016-08-19. Retrieved 2016-08-03.{{cite web}}: CS1 maint: archived copy as title (link)
  6. ^ Boss, Alan (2009-02-01). The Crowded Universe: The Race to Find Life Beyond Earth. Basic Books. p. 53. ISBN 978-0-465-00936-7.
  7. ^ a b c d e 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.
  8. ^ a b Rivera, Eugenio J.; et al. (2005). "A ~7.5 M🜨 Planet Orbiting the Nearby Star, GJ 876". The Astrophysical Journal. 634 (1): 625–640. arXiv:astro-ph/0510508. Bibcode:2005ApJ...634..625R. doi:10.1086/491669.
  9. ^ 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.
  10. ^ 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.
  11. ^ a b 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.
  12. ^ Gerlach, Enrico; Haghighipour, Nader (2012). "Can GJ 876 host four planets in resonance?". Celestial Mechanics and Dynamical Astronomy. 113 (1): 35–47. arXiv:1202.5865. Bibcode:2012CeMDA.113...35G. doi:10.1007/s10569-012-9408-0. S2CID 119210665.
  13. ^ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. from the original on 18 August 2010. Retrieved 19 February 2011.
  14. ^ Fraser Cain (September 15, 2008). "Temperature of the Sun". Universe Today. from the original on 29 August 2010. Retrieved 19 February 2011.
  15. ^ 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.
  16. ^ 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.
  17. ^ Kasting, James F.; et al. (1993). "Habitable Zones around Main Sequence Stars" (PDF). Icarus. 101 (1): 108–128. Bibcode:1993Icar..101..108K. doi:10.1006/icar.1993.1010. PMID 11536936. (PDF) from the original on 2014-04-07. Retrieved 2012-08-05.
  18. ^ 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)
  19. ^ 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. S2CID 4327454.
  20. ^ Kipping, David (2009). "Transit timing effects due to an exomoon". Monthly Notices of the Royal Astronomical Society. 392 (1): 181–189. arXiv:0810.2243. Bibcode:2009MNRAS.392..181K. doi:10.1111/j.1365-2966.2008.13999.x. S2CID 14754293.
  21. ^ Heller, R. (2012). "Exomoon habitability constrained by energy flux and orbital stability". Astronomy & Astrophysics. 545: L8. arXiv:1209.0050. Bibcode:2012A&A...545L...8H. doi:10.1051/0004-6361/201220003. ISSN 0004-6361. S2CID 118458061.
  22. ^ a b Andrew J. LePage (August 2006). "Habitable Moons:What does it take for a moon — or any world — to support life?". SkyandTelescope.com. from the original on 2012-04-06. Retrieved 2011-07-11.
  23. ^ Glatzmaier, Gary A. "How Volcanoes Work – Volcano Climate Effects". from the original on 23 April 2011. Retrieved 29 February 2012.
  24. ^ . Solar System Exploration. NASA. Archived from the original on 16 December 2003. Retrieved 29 February 2012.
  25. ^ Nave, R. "Magnetic Field of the Earth". from the original on 15 May 2019. Retrieved 29 February 2012.
  26. ^ "In Search Of Habitable Moons". Pennsylvania State University. from the original on 2019-06-01. Retrieved 2011-07-11.

External links

  •   Media related to Gliese 876 b at Wikimedia Commons
  • 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.


August 24, 2023
gliese, exoplanet, orbiting, dwarf, gliese, completes, orbit, approximately, days, discovered, june, 1998, first, planet, discovered, orbiting, dwarf, artist, impression, gliese876, bdiscovery, discovered, bycalifornia, carnegie, planet, search, team, independ. Gliese 876 b is an exoplanet orbiting the red dwarf Gliese 876 It completes one orbit in approximately 61 days Discovered in June 1998 Gliese 876 b was the first planet to be discovered orbiting a red dwarf Gliese 876 bAn artist s impression of Gliese876 bDiscovery 1 2 3 Discovered byCalifornia and Carnegie Planet Search Team and independently by the Geneva Extrasolar Planet Search TeamDiscovery siteLick Keck Haute Provence and La Silla ObservatoriesDiscovery dateJune 22 1998Detection methodDoppler spectroscopyOrbital characteristics 4 Epoch 2 450 602 09311 BJDSemi major axis0 218627 0 000017 AUEccentricity0 0325 0 0016 0 0017Orbital period sidereal 61 1057 0 0074 dMean anomaly340 6 4 4 4 ºInclination53 06 0 85 º note 1 Argument of perihelion35 5 4 1 4 4 ºSemi amplitude211 57 0 3 0 29 m sStarGliese 876Physical characteristics 4 Mass845 2 9 5 9 4 M note 2 Temperature194 K 79 C 110 F 5 Contents 1 Discovery 2 Characteristics 2 1 Mass radius and temperature 2 2 Host star 2 3 Orbit 3 Future habitability 4 See also 5 Notes 6 References 7 External linksDiscovery EditGliese 876 b was initially announced by Geoffrey Marcy on June 22 1998 at a symposium of the International Astronomical Union in Victoria British Columbia Canada The discovery was made using data from the Keck and Lick observatories 3 6 Only 2 hours after his announcement he was shown an e mail from the Geneva Extrasolar Planet Search team confirming the planet The Geneva team used telescopes at the Haute Provence Observatory in France and the European Southern Observatory in La Serena Chile 3 2 Like the majority of early extrasolar planet discoveries it was discovered by detecting variations in its star s radial velocity as a result of the planet s gravity This was done by making sensitive measurements of the Doppler shift of the spectral lines of Gliese 876 It was the first discovered of four known planets in the Gliese 876 system 7 1 2 8 9 Characteristics EditMass radius and temperature Edit An artist s impression of Gliese 876 b as an enormous Jupiter like planet with a hypothetical satellite system Given the planet s high mass it is likely that Gliese 876 b is a gas giant with no solid surface Since the planet has only been 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 it is predicted that the atmosphere of Gliese 876 b is cloudless though cooler regions of the planet may be able to form water clouds 10 A limitation of the radial velocity method used to detect Gliese 876 b is that only a lower limit on the planet s mass can be obtained This lower limit is around 1 93 times the mass of Jupiter 8 The true mass depends on the inclination of the orbit which in general is unknown However because Gliese 876 is only 15 light years from Earth Benedict et al 2002 were able to use one of the Fine Guidance Sensors on the Hubble Space Telescope to detect the astrometric wobble created by Gliese 876 b 11 This constituted the first unambiguous astrometric detection of an extrasolar planet 7 Their analysis suggested that the orbital inclination is 84 6 close to edge on 11 In the case of Gliese 876 b modelling the planet planet interactions from the Laplace resonance shows that the actual inclination of the orbit is 59 resulting in a true mass of 2 2756 times the mass of Jupiter 7 The equilibrium temperature of Gliese 876 b is estimated to be around 194 K 79 C 110 F 5 This planet like c and e has likely migrated inward 12 Host star Edit Main article Gliese 876 The planet orbits a M type star named Gliese 876 The star has a mass of 0 33 M and a radius of around 0 36 R It has a surface temperature of 3350 K and is 2 55 billion years old In comparison the Sun is about 4 6 billion years old 13 and has a surface temperature of 5778 K 14 Orbit Edit The orbits of the planets of Gliese 876 Gliese 876 b is the third planet from the star Gliese 876 b is in a 1 2 4 Laplace resonance with the inner planet Gliese 876 c and the outer planet Gliese 876 e in the time it takes planet e to complete one orbit planet b completes two and planet c completes four This is the second known example of a Laplace resonance the first being Jupiter s moons Io Europa and Ganymede 7 As a result the orbital elements of the planets change fairly rapidly as they dynamically interact with one another 15 The planet s orbit has a low eccentricity similar to the planets in the Solar System The semimajor axis of the orbit is only 0 208 AU less than that of Mercury in the Solar System 7 However Gliese 876 is such a faint star that this puts it in the outer part of the habitable zone 16 Future habitability EditSee also Habitability of red dwarf systems and Habitability of natural satellites Gliese 876 b currently lies beyond the outer edge of the habitable zone but because Gliese 876 is a slowly evolving main sequence red dwarf its habitable zone is very slowly moving outwards and will continue to do so for trillions of years Therefore Gliese 876 b will in trillions of years time lie inside Gliese 876 s habitable zone as defined by the ability of an Earth mass planet to retain liquid water at its surface and remain there for at least 4 6 billion years 17 While the prospects for life on a gas giant are unknown large moons may be able to support a habitable environment Models of tidal interactions between a hypothetical moon the planet and the star suggest that large moons should be able to survive in orbit around Gliese 876 b for the lifetime of the system 18 On the other hand it is unclear whether such moons could form in the first place 19 However the large mass of the gas giant may make it more likely for larger moons to form citation needed For a stable orbit the ratio between the moon s orbital period Ps around its primary and that of the primary around its star Pp must be lt 1 9 e g if a planet takes 90 days to orbit its star the maximum stable orbit for a moon of that planet is less than 10 days 20 21 Simulations suggest that a moon with an orbital period less than about 45 to 60 days will remain safely bound to a massive giant planet or brown dwarf that orbits 1 AU from a Sun like star 22 In the case of Gliese 876 b the orbital period would have to be no greater than a week 7 days in order to have a stable orbit Tidal effects could also allow the moon to sustain plate tectonics which would cause volcanic activity to regulate the moon s temperature 23 24 and create a geodynamo effect which would give the satellite a strong magnetic field 25 To support an Earth like atmosphere for about 4 6 billion years the age of the Earth the moon would have to have a Mars like density and at least a mass of 0 07 MEarth 26 One way to decrease loss from sputtering is for the moon to have a strong magnetic field that can deflect stellar wind and radiation belts NASA s Galileo s measurements hints large moons can have magnetic fields it found that Jupiter s moon Ganymede has its own magnetosphere even though its mass is only 0 025 MEarth 22 See also EditAppearance of extrasolar planetsNotes Edit The inclination assumes the planets in the system are coplanar long term orbital stability simulations strongly favor low mutual inclinations Uncertainties in the planetary masses and semimajor axes do not take into account the uncertainty in the mass of the star References Edit a b Marcy Geoffrey W et al 1998 A Planetary Companion to a Nearby M4 Dwarf Gliese 876 The Astrophysical Journal Letters 505 2 L147 L149 arXiv astro ph 9807307 Bibcode 1998ApJ 505L 147M doi 10 1086 311623 a b c Delfosse Xavier Forveille Thierry Mayor Michel Perrier Christian Naef Dominique Queloz Didier 1998 The closest extrasolar planet A giant planet around the M4 dwarf GL 876 Astronomy and Astrophysics 338 L67 L70 arXiv astro ph 9808026 Bibcode 1998A amp A 338L 67D a b c Astronomers find planet orbiting nearby star Press release W M Keck Observatory 1998 06 22 Archived from the original on 2018 09 24 Retrieved 2018 09 23 a b Millholland Sarah et al 2018 New Constraints on Gliese 876 Exemplar of Mean motion Resonance The Astronomical Journal 155 3 Table 4 arXiv 1801 07831 Bibcode 2018AJ 155 106M doi 10 3847 1538 3881 aaa894 a b Archived copy Archived from the original on 2016 08 19 Retrieved 2016 08 03 a href Template Cite web html title Template Cite web cite web a CS1 maint archived copy as title link Boss Alan 2009 02 01 The Crowded Universe The Race to Find Life Beyond Earth Basic Books p 53 ISBN 978 0 465 00936 7 a b c d e 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 a b Rivera Eugenio J et al 2005 A 7 5 M Planet Orbiting the Nearby Star GJ 876 The Astrophysical Journal 634 1 625 640 arXiv astro ph 0510508 Bibcode 2005ApJ 634 625R doi 10 1086 491669 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 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 a b 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 Gerlach Enrico Haghighipour Nader 2012 Can GJ 876 host four planets in resonance Celestial Mechanics and Dynamical Astronomy 113 1 35 47 arXiv 1202 5865 Bibcode 2012CeMDA 113 35G doi 10 1007 s10569 012 9408 0 S2CID 119210665 Fraser Cain 16 September 2008 How Old is the Sun Universe Today Archived from the original on 18 August 2010 Retrieved 19 February 2011 Fraser Cain September 15 2008 Temperature of the Sun Universe Today Archived from the original on 29 August 2010 Retrieved 19 February 2011 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 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 Kasting James F et al 1993 Habitable Zones around Main Sequence Stars PDF Icarus 101 1 108 128 Bibcode 1993Icar 101 108K doi 10 1006 icar 1993 1010 PMID 11536936 Archived PDF from the original on 2014 04 07 Retrieved 2012 08 05 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 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 S2CID 4327454 Kipping David 2009 Transit timing effects due to an exomoon Monthly Notices of the Royal Astronomical Society 392 1 181 189 arXiv 0810 2243 Bibcode 2009MNRAS 392 181K doi 10 1111 j 1365 2966 2008 13999 x S2CID 14754293 Heller R 2012 Exomoon habitability constrained by energy flux and orbital stability Astronomy amp Astrophysics 545 L8 arXiv 1209 0050 Bibcode 2012A amp A 545L 8H doi 10 1051 0004 6361 201220003 ISSN 0004 6361 S2CID 118458061 a b Andrew J LePage August 2006 Habitable Moons What does it take for a moon or any world to support life SkyandTelescope com Archived from the original on 2012 04 06 Retrieved 2011 07 11 Glatzmaier Gary A How Volcanoes Work Volcano Climate Effects Archived from the original on 23 April 2011 Retrieved 29 February 2012 Solar System Exploration Io Solar System Exploration NASA Archived from the original on 16 December 2003 Retrieved 29 February 2012 Nave R Magnetic Field of the Earth Archived from the original on 15 May 2019 Retrieved 29 February 2012 In Search Of Habitable Moons Pennsylvania State University Archived from the original on 2019 06 01 Retrieved 2011 07 11 External links Edit Media related to Gliese 876 b at Wikimedia Commons 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 Retrieved from https en wikipedia org w index php title Gliese 876 b amp oldid 1160408698, wikipedia, wiki, book, books, library,

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