Gliese 876

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Gliese 876
Aquarius constellation map.svg
Red Circle(small).svg
Location of Gliese 876 in Aquarius (red dot)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Aquarius
Pronunciation /ˈɡliːzə/
Right ascension 22h 53m 16.73258s [1]
Declination −14° 15′ 49.3041″ [1]
Apparent magnitude  (V)10.1920(17) [2]
Characteristics
Spectral type M4V [3]
Apparent magnitude  (J)5.934(19) [4]
Apparent magnitude  (H)5.349(49) [4]
Apparent magnitude  (K)5.010(21) [4]
Variable type BY Draconis [5]
Astrometry
Radial velocity (Rv)−2.09±0.15 [1]  km/s
Proper motion (μ)RA: 957.715(41)  mas/yr [1]
Dec.: −673.601(31)  mas/yr [1]
Parallax (π)214.0380 ± 0.0356  mas [1]
Distance 15.238 ± 0.003  ly
(4.6721 ± 0.0008  pc)
Absolute magnitude  (MV)11.81 [6]
Details
Mass 0.346±0.007 [7]   M☉
Radius 0.372±0.004 [7]   R☉
Luminosity 0.01309±0.00011 [7]   L☉
Surface gravity (log g)4.89 [8]   cgs
Temperature 3,201+20
−19 [7]   K
Metallicity [Fe/H]+0.19±0.17 [9]   dex
Rotation 83.7±2.9  d [10]
Rotational velocity (v sin i)0.16 [11]  km/s
Age 0.1–9.9 [11] [12]   Gyr
Other designations
IL Aquarii, BD−15°6290, Gaia DR3  2603090003484152064, HIP  113020, G 156-057, LHS  530, Ross  780 [13]
Database references
SIMBAD Gliese 876
d
c
b
e
Exoplanet Archive data
ARICNS data

Gliese 876 is a red dwarf star 15.2 light-years (4.7 parsecs ) away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance (a type of resonance first noted in Jupiter's inner three Galilean moons). It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

Contents

Distance and visibility

Gliese 876 is located fairly close to the Solar System. According to astrometric measurements made by the Gaia space observatory, the star shows a parallax of 214.038 milliarcseconds, which corresponds to a distance of 4.6721 parsecs (15.238  ly ). [1] Despite being located so close to Earth, the star is so faint that it is invisible to the naked eye and can only be seen using a telescope.

Stellar characteristics

A visual band light curve for IL Aquarii, adapted from Hosey et al. (2015) ILAqrLightCurve.png
A visual band light curve for IL Aquarii, adapted from Hosey et al. (2015)

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 infrared wavelengths. 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. Gliese876Orbits.svg
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 pulsar PSR 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]

The Gliese 876 planetary system [10] [note 1]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
d 6.68±0.22  M🜨 0.0210205251.9377904+0.0000064
−0.0000073		0.035+0.033
−0.024		56.7±1.0 ° —
c 0.740±0.008  MJ 0.130874+0.00002
−0.000019		30.1039+0.0069
−0.0066		0.257+0.0018
−0.0019		56.7±1.0 ° —
b 2.357±0.027  MJ 0.209805+0.000014
−0.000016		61.1035+0.0062
−0.0069		0.0296+0.003
−0.0013		56.7±1.0 ° —
e 16.0±1.0  M🜨 0.3355+0.0019
−0.0011		123.55+1.0
−0.59		0.0545+0.0069
−0.022		56.7±1.0 ° —
Gliese 876 d

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

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

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.

Gliese 876 e

Gliese 876 e, discovered in 2010, has a mass similar to that of the planet Uranus and its orbit takes 124 days to complete.

See also

Notes

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

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<span class="mw-page-title-main">Gliese 876 d</span> Super-Earth orbiting Gliese 876

Gliese 876 d is an exoplanet 15.2 light-years away in the constellation of Aquarius. The planet was the third planet discovered orbiting the red dwarf Gliese 876, and is the innermost planet in the system. It was the lowest-mass known exoplanet apart from the pulsar planets orbiting PSR B1257+12 at the time of its discovery. Due to its low mass, it can be categorized as a super-Earth.

<span class="mw-page-title-main">Gliese 876 c</span> Gas giant orbiting Gliese 876

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<span class="mw-page-title-main">Gliese 876 b</span> Extrasolar planet orbiting Gliese 876

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.

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<span class="mw-page-title-main">Gliese 876 e</span> Exoplanet orbiting the star Gliese 876

Gliese 876 e is an exoplanet orbiting the star Gliese 876 in the constellation of Aquarius. It is in a 1:2:4 Laplace resonance with the planets Gliese 876 c and Gliese 876 b: for each orbit of planet e, planet b completes two orbits and planet c completes four. This configuration is the second known example of a Laplace resonance after Jupiter's moons Io, Europa and Ganymede. Its orbit takes 124 days to complete.

References

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  34. ↑ Dybczyński, Piotr A.; Królikowska, Małgorzata (February 2018). "Investigating the dynamical history of the interstellar object 'Oumuamua". Astronomy & Astrophysics. 610: 12. arXiv: 1711.06618 . Bibcode:2018A&A...610L..11D. doi:10.1051/0004-6361/201732309. S2CID   119513894. L11.
  35. ↑ Konacki, Maciej; Wolszczan, Alex (July 2003). "Masses and Orbital Inclinations of Planets in the PSR B1257+12 System". The Astrophysical Journal. 591 (2): L147–L150. arXiv: astro-ph/0305536 . Bibcode:2003ApJ...591L.147K. doi:10.1086/377093. S2CID   18649212.
  36. 1 2 Sudarsky, 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. ISSN   0004-637X. 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.
  37. ↑ Butler, R. P.; et al. (December 2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv: astro-ph/0607493 . Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID   119067572.

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