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Epsilon Eridani

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18 Eri, HD 22049, HR 1084, BD-09°697, GCTP 742.00, WDS 03330-0928, SAO 130564, LHS 1557
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Epsilon Eridani (ε Eri / ε Eridani) is a main-sequence K2 class star in the constellation of Eridanus. It is the third closest star outside of the solar system visible without a telescope. It has 85% of the Sun's mass, almost that much of its diameter, and 28% of its luminosity.

Its spectrum is extremely variable, with many emission lines. It has a very strong magnetic field. It spins about every 11 days.2. The reason for all this is its youth; it is only about half a billion years old. For this reason, it is considered unlikely to have intelligent life in its system. Tau Ceti is a much better candidate, and like Epsilon Eridani, is also deficient in iron. A planet orbiting Epsilon Eridani at a distance of around 0.53 astronomical units would have temperatures suitable for liquid water.

Its closest neighbour is Luyten 726-8 (UV Ceti and BL Ceti), 5.22 ly (1.60 pc) away.

Dust disc

In 1988, a dust disk was discovered around the star, at a similar distance as the Kuiper belt is from our Sun. Bruce Campbell and others interpreted doppler measurements as clumps in the dust ring that suggest another planet orbits the star, causing the clumps through resonance. The dust disc contains approximately 1000 times more dust than is present in the inner system around our Sun, which may mean it has about 1000 times as much cometary material as our solar system.

Within 35 AU of the star the dust is depleted, which may mean that the system has formed planets which have cleared out the dust in this region. This is consistent with currently accepted models of the inner solar system, and so there may be terrestrial planets around the star.

Planetary system

As Epsilon Eridani is one of the nearest solar-type stars to our Sun, many attempts to search for orbiting planets have been made. However, the star's high activity and variability means that finding planets with the radial velocity method is difficult, and stellar activity may mimic the presence of planets.

Epsilon Eridani b

Epsilon Eridani b is a extrasolar planet candidate around Epsilon Eridani, announced in 2000 by a team led by Artie Hatzes. The discoverers gave its mass as 1.2 ± 0.33 times that of Jupiter, with a mean distance of 3.3 AU from the star. The object's orbit is highly eccentric. Other observers, including Geoffrey Marcy required more information on the star's doppler noise behaviour created by its large and varying magnetic field, and the discovery remains controversial. Its existence had also been previously suspected by a Canadian team led by Bruce Campbell and Gordon Walker in the early 1990s, but their observations weren't definitive enough to make a solid discovery.

Epsilon Eridani c

A hypothetical planet designated Epsilon Eridani c was proposed in 2002 based on analysis of the structure of the dust disk around the star. Clumping in the dust disk can be modelled by dust particles being trapped in resonances with a planet in an eccentric orbit. As of 2006 the existence of this planet has not been confirmed.

Epsilon Eridani in fiction

Because of its status as the closest, single Sun-like star, Epsilon Eridani appears frequently in science fiction.

See also

References

External links

Notes

 


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