Epsilon Eridani
| Epsilon Eridani | |
|---|---|
| |
| Observational Data | |
| Designation | Ran HD 22049 HIP 16537 |
| Right ascension | 03h 32m 55.8450s[1][2] |
| Declination | -09° 27′ 29.7312 ″[1][2] |
| Constellation | Eridanus |
| Type of object | Star |
| Magnitude | Apparent Mag: 3.72[3] Absolute Mag: 6.18[3] |
| Astrometry | |
| Distance from Earth | 10.49 ly[3] |
| Radial velocity | 16.43 ± 0.09 km/s[1][4] |
| Proper motion | RA: -975.17 mas/yr[1][2] Dec.: 19.49 mas/yr[1][2] |
| Parallax | 310.94 ± 0.16 mas[1][2] |
Epsilon Eridani (18 Erandi, Ran, HD 22049, HIP 16537) is a nearby K2 class star some 10.5 light years away in the constellation of Eridanus. In addition to being one of the nearest Sun-like stars, it is the closest known star with a planetary companion, which was discovered in 2000. Because of Epsilon Eridani's proximity to our solar system, the star has been an object of high interest among astronomers, and is a "Tier 1" target for NASA's optical Space Interferometry Mission.
The Star
Epsilon Eridani is a main sequence, orange-red dwarf star of spectral class K2V B.[1][5] Its high level of chromospheric activity, strong magnetic field, and relatively fast rotation rate of only 11 days (less than half the rotation period of the Sun) indicate this age. However, the star also has a low metallicity, estimated at only 49 to 74 of the Sun's abundance of iron.
The star is smaller than our Sun, with an estimated 83 percent of its mass,[6] and 84 percent of the Sun's radius.[7] But even with nearly the size of the Sun, Epsilon Eridani only is 27.8 percent as luminous.[8]
From Earth, Epsilon Eridani has an apparent magnitude of 3.72, making it the third closest star (after Alpha Centauri AB and Sirius) that can be viewed with the unaided eye.[3]
Planetary System
Epsilon Eridani has one confirmed planet orbiting the star, with a possible but unconfirmed second world that possibly shepherds Epsilon Eridani's dust disk.
Planets
Using long term radical velocity observations, scientists announced the discovery of a planet orbiting Epsilon Eridani in August 2000.[9] In 2006, additional astrometic measurements were used to acquire more accurate and detailed information on the planet. The planet is believed to be a gas giant with an estimated mass 1.55±0.24 times that of Jupiter, with a mean orbital distance of 3.39±0.36 AU, taking around 6.9 years to complete one orbit. The orbit itself is highly eccentric (e= 0.702±0.039). The orbit takes the planet as close as 2.4 AUs and as far as 5.8 AUs from Epsilon Eridani itself. This planet orbits just outside the innermost asteroid belt in the system.[10]
A second unconfirmed planet is believed to be possibly orbiting Epsilon Eridani some 35-40 AU away. A planet is proposed as the most likely candidate to explain the "lumpiness" observed in the star's broad, outer belt of icy particles as such action is typically caused by perturbations by one or more planetary bodies, as well as to why the area within 35 AU of the star is relatively depleted of dust. If the planet exists, it is believed to be some 30 times the mass of the Earth (or about a tenth of Jupiter's mass), and an eccentric orbit (e~0.3), taking around 280 years to complete.[11]
Another possible world is also hypothesized due to the discovery of a second asteroid belt between the inner asteroid belt and the broad outer belt of icy bodies, comet-type bodies. Such a world would most likely be a Jupiter-class planet orbiting at roughly 20 AUs around Epsilon Eridani, which would be "shepherding" the icy, rocky bodies at the outer rim of the second outer asteroid belt, just as Epsilon Eridani b shepherds the inner asteroid belt.[12]
There is further indirect evidence of a possible planet orbiting Epsilon Eridani because of asymmetries in the outer icy dust disk, which could be the result of perturbations by a substellar body located around 55-65 AUs. The planet, if it exists, would have around a fifth of the mass of Jupiter.[13]
For an Earth-like planet to have liquid water on its surface around Epsilon Eridani, it would need to be between 0.47 and 0.91 AU from its parent star. However such a planet would have to endure the much heavier meteorite or cometary bombardment in the youthful system, which may have about 1,000 times more cometary bodies than are found in our Solar System today.
Dust Disk
Epsilon Eridani has a large dust disk made up of tiny particles of ice and dust that orbits in a ring that generally stretches between 35 and 90 AU from the star, being densest around 60 AU that was first detected in 1998. The total mass of the dust disk is estimated to be around 1000 times greater than the amount of similar material in our own inner solar system. Inside of 35 AU the dust is depleted. It is believed that this is due to the formation of planets that has cleared out the dust in the region.
In 2008, using the Spitzer Space Telescope, NASA revealed there are two asteroid belts in the system in addition to the outer dust disk. Made of rocky and metallic debris, the closer belt is estimated to be approximately the same distance from Epsilon Eridani as the asteroid belt in our Solar System is from the Sun, while the second belt orbits at a mean distance of around 20 AU.[12]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Epsilon Eridani. Simbad Astronomical Database. simbad.u-strasbg.fr. Retrieved on 2019-07-24.
- ↑ 2.0 2.1 2.2 2.3 2.4 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics 474 (2): 653-664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. arXiv:0708.1752
- ↑ 3.0 3.1 3.2 3.3 Ran (Epsilon Eridani, 18 Eridani). universeguide.com. Retrieved on 2019-07-24.
- ↑ Nidever, D.; Marcy, G.; Butler, R. et al. (2002). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series 141 (2): 503-522. doi:10.1086/340570. Bibcode: 2002ApJS..141..503N. arXiv:astro-ph/0112477
- ↑ Keenan, P. C.; McNeil, R. C. (1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". Astrophysical Journal Supplement 71: 245. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K.
- ↑ Jim Kaler. Epsilon Eridani. stars.astr.illinois.edu. Retrieved on 2019-07-24.
- ↑ Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal, Suppl. Ser. 53: 643-711. doi:10.1086/190905. Bibcode: 1983ApJS...53..643J.
- ↑ Saumon, D.; Hubbard, W. B.; Burrows, A. et al. (1996). "A Theory of Extrasolar Giant Planets". Astrophysical Journal 460: 993. doi:10.1086/177027. Bibcode: 1996ApJ...460..993S. arXiv:astro-ph/9510046
- ↑ Hatzes, A. P.; Cochran, W. D.; McArthur, B. et al. (2000). "Evidence for a Long-period Planet Orbiting Epsilon Eridani". The Astrophysical Journal 544 (2): L145-L148. doi:10.1086/317319. Bibcode: 2000ApJ...544L.145H. arXiv:astro-ph/0009423
- ↑ Planet eps Eridani b. Retrieved on 2019-07-24.
- ↑ Quillen, A. C.; Throndike, S. (2002). "Structure in the ɛ Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron". The Astrophysical Journal 578 (2): L149-L152. doi:10.1086/344708. Bibcode: 2002ApJ...578L.149Q. arXiv:astro-ph/0208279
- ↑ 12.0 12.1 Epsilon Eridani System Diagram. spitzer.caltech.edu (2008-10-27). Retrieved on 2019-07-24.
- ↑ Liou, J. -C.; Zook, H. A. (1999). "Signatures of Giant Planets on the Solar System Kuiper Belt Dust Disk and Implications for Extrasolar Planet in Epsilon Eridani". 30th Annual Lunar and Planetary Science Conference. Bibcode: 1999LPI....30.1698L.
