![]() The stellar wind of this star expands outward, producing a bow shock at a distance of 63 AU. ![]() The corona of ε Indi A is similar to the Sun, with an X-ray luminosity of 2 ×10 27 ergs s −1 (2 ×10 20 W) and an estimated coronal temperature of 2 ×10 6 K. The metallicity of a star is the proportion of elements with higher atomic numbers than helium, being typically represented by the ratio of iron to hydrogen compared to the same ratio for the Sun ε Indi A is found to have about 87% of the Sun's proportion of iron in its photosphere. Its surface gravity is slightly higher than the Sun's. The star has only about three-fourths the mass of the Sun and 71% of the Sun's radius. Ε Indi A is a main-sequence star of spectral type K5V. The star is among five nearby paradigms as K-type stars of a type in a 'sweet spot' between Sun-analog stars and M stars for the likelihood of evolved life, per analysis of Giada Arney from NASA's Goddard Space Flight Center. ε Indi leads a list, compiled by Margaret Turnbull and Jill Tarter of the Carnegie Institution in Washington, of 17,129 nearby stars most likely to have planets that could support complex life. In 1972, the Copernicus satellite was used to examine this star for the emission of ultraviolet laser signals. In 1923, Harlow Shapley of the Harvard Observatory derived a parallax of 0.45 arcseconds. They derived a parallax estimate of 0.22 ± 0.03 arcseconds. In 1882–3, the parallax of ε Indi was measured by astronomers David Gill and William L. That is, he found that the star had changed position across the celestial sphere over time. In 1847, Heinrich Louis d'Arrest compared the position of this star in several catalogues dating back to 1750, and discovered that it possessed a measureable proper motion. The 1801 star atlas Uranographia, by German astronomer Johann Elert Bode, places ε Indi as one of the arrows being held in the left hand of the Indian. ![]() The constellation Indus (the Indian) first appeared in Johann Bayer's celestial atlas Uranometria in 1603. Observation Įpsilon Indi with SkyMapper and a Hubble NICMOS image of the brown dwarf binary The ε Indi system provides a benchmark case for the study of the formation of gas giants and brown dwarfs. ε Indi Ab is the second-closest Jovian exoplanet, after ε Eridani b. Ε Indi A has one known planet, ε Indi Ab, with a mass of 3.3 Jupiter masses in a nearly circular orbit with a period of about 45 years. ε Indi Ba is an early T dwarf (T1) and ε Indi Bb a late T dwarf (T6) separated by 0.6 arcseconds, with a projected distance of 1460 AU from their primary star. The brown dwarfs were discovered in 2003. It consists of a K-type main-sequence star, ε Indi A, and two brown dwarfs, ε Indi Ba and ε Indi Bb, in a wide orbit around it. The star has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.83. UGP 544, ε Ind, CD−57☈464, CPD−57☁0015, FK5 825, GJ 845, HD 209100, HIP 108870, HR 8387, SAO 247287, LHS 67 Įpsilon Indi, Latinized from ε Indi, is a star system located at a distance of approximately 12 light-years from Earth in the southern constellation of Indus.
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