As a red dwarf, Gliese 876 is much less massive than the Sun: estimates suggest it has only 35% of the mass of the Sun.[7] The surface temperature of Gliese 876 is cooler than the Sun and the star has a smaller radius.[15] These factors combine to make the star only 1.3% as luminous as the Sun, and most of this is at infraredwavelengths. Estimating the age and metallicity of cool stars is difficult due to the formation of diatomic molecules in their atmospheres, which makes the spectrum extremely complex. By fitting the observed spectrum to model spectra, it is estimated that Gliese 876 has a slightly lower abundance of heavy elements compared to the Sun (around 75% the solar abundance of iron).[8] Based on chromospheric activity the star is likely to be around 6.5 to 9.9 billion years old, depending on the theoretical model used.[12] However, its membership among the young disk population suggest that the star is less than 5 billion years old but the long rotational period of the star implies that it is at least older than 100 million years.[11] Like many low-mass stars, Gliese 876 is a variable star. Its variable star designation is IL Aquarii and it is classified as a BY Draconis variable. Its brightness fluctuates by around 0.04 magnitudes.[5] This type of variability is thought to be caused by large starspots moving in and out of view as the star rotates.[16] Gliese 876 emits X-rays like most Red Dwarfs would do.[17]
Planetary system
Observation history
The orbits of the planets of Gliese 876. Note that the strong gravitational interactions between the planets causes rapid orbital precession, so this diagram is only valid at the stated epoch.
On June 23, 1998, an extrasolar planet was announced in orbit around Gliese 876 by two independent teams led by Geoffrey Marcy and Xavier Delfosse.[18][19][20] The planet was designated Gliese 876 b and was detected by Doppler spectroscopy. Based on luminosity measurement, the circumstellar habitable zone (CHZ) is believed to be located between 0.116 and 0.227 AU.[21] On January 9, 2001, a second planet designated Gliese 876 c was detected, inside the orbit of the previously-discovered planet.[22][23] The relationship between the orbital periods initially disguised the planet's radial velocity signature as an increased orbital eccentricity of the outer planet. Eugenio Rivera and Jack Lissauer found that the two planets undergo strong gravitational interactions as they orbit the star, causing the orbital elements to change rapidly.[24] On June 13, 2005, further observations by a team led by Rivera revealed a third planet, designated Gliese 876 d inside the orbits of the two Jupiter-size planets.[25] In January 2009, the mutual inclination between planets b and c was determined using a combination of radial velocity and astrometric measurements. The planets were found to be almost coplanar, with an angle of only 5.0+3.9 −2.3° between their orbital planes.[26]
On June 23, 2010, astronomers announced a fourth planet, designated Gliese 876 e. This discovery better constrained the mass and orbital properties of the other three planets, including the high eccentricity of the innermost planet.[27] This also filled out the system inside e's orbit; additional planets there would be unstable at this system's age.[28] In 2014, reanalysis of the existing radial velocities suggested the possible presence of two additional planets, which would have almost the same mass as Gliese 876 d,[29] but further analysis showed that these signals were artifacts of dynamical interactions between the known planets.[30] In 2018 a study using hundreds of new radial velocity measurements found no evidence for any additional planets.[31] If this system has a comet disc, it is not "brighter than the fractional dust luminosity 10−5" according to a 2012 Herschel study.[32] None of these planets transit the star from the perspective of Earth, making it difficult to study their properties.[33]
GJ 876 is a candidate parent system for the ʻOumuamua object. The trajectory of this interstellar object took it near the star about 820,000 years ago with a velocity of 5 km/s, after which it has been perturbed by six other stars.[34]
Orbital arrangement
Gliese 876 has a notable orbital arrangement. It is the first planetary system around a normal star to have mutual inclination between planets measured without transits (previously the mutual inclination of the planets orbiting the pulsarPSR B1257+12 had been determined by measuring their gravitational interactions[35]). Later measurements reduced the value of the mutual inclination,[11] and in the latest four-planet models the incorporation mutual inclinations does not result in significant improvements relative to coplanar solutions.[27] The system has the second known example of a Laplace resonance with a 1:2:4 resonance of its planets. The first known example was Jupiter's closest Galilean moons - Ganymede, Europa and Io. Numerical integration indicates that the coplanar, four-planet system is stable for at least another billion years. This planetary system comes close to a triple conjunction between the three outer planets once per orbit of the outermost planet.[27]
Planets
The outermost three of the known planets likely formed further away from the star, and migrated inward.[28]
Gliese 876 d, discovered in 2005, is the innermost known planet. With an estimated mass 6.7 times that of the Earth, it is possible that it is a dense terrestrial planet.
Gliese 876 c, discovered in 2001, is a 0.74 Jupiter-mass giant planet. It is in a 1:2 orbital resonance with the planet b, taking 30.104 days to orbit the star. The planet orbits within the habitable zone. Its temperature makes it more likely to be a Class III planet in the Sudarsky extrasolar planet classification.[36] The presence of surface liquid water and life is possible on sufficiently massive satellites should they exist.
Gliese 876 b, discovered in 1998, is around twice the mass of Jupiter and revolves around its star in an orbit taking 61.104 days to complete, at a distance of only 0.21 AU, less than the distance from the Sun to Mercury.[37] Its temperature makes it more likely to be a Class II or Class III planet in the Sudarsky model.[36] The presence of surface liquid water and life is possible on sufficiently massive satellites should they exist.
^Lurie, John C; Henry, Todd J; Jao, Wei-Chun; Quinn, Samuel N; Winters, Jennifer G; Ianna, Philip A; Koerner, David W; Riedel, Adric R; Subasavage, John P (2014). "The Solar Neighborhood. Xxxiv. A Search for Planets Orbiting Nearby M Dwarfs Using Astrometry". The Astronomical Journal. 148 (5): 91. arXiv:1407.4820. Bibcode:2014AJ....148...91L. doi:10.1088/0004-6256/148/5/91. S2CID118492541.
^"Two new planetary systems discovered" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. January 9, 2001. Archived from the original on August 13, 2019. Retrieved August 13, 2019.
^ abSudarsky, David; Burrows, Adam; Hubeny, Ivan (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. hdl:10150/280087. ISSN0004-637X. GJ 876b and c are both Class III planets because their temperatures are too cool for a silicate layer to appear in the troposphere, but too hot for H2O to condense ... Given somewhat lower incident irradiation than that of our scaled Kurucz model for GJ 876, or given an observation of GJ 876b at apastron, some water condensation may occur in its outermost atmosphere, rendering it a Class II EGP.
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