Search results
Results from the WOW.Com Content Network
In 2016, the IAU organised a Working Group on Star Names (WGSN) [31] to catalogue and standardise proper names for stars. In its first bulletin of July 2016, [32] the WGSN explicitly recognised the names of exoplanets and their host stars that were produced by the competition. Epsilon Eridani is now listed as Ran in the IAU Catalog of Star ...
In modern usage, the names applied to K-type main sequence stars vary. When explicitly defined, late K dwarfs are typically grouped with early to mid-M-class stars as red dwarfs, [4] but in other cases red dwarf is restricted just to M-class stars. [5] [6] In some cases all K stars are included as red dwarfs, [7] and occasionally even earlier ...
The planet and its host star are one of the planetary systems selected by the International Astronomical Union as part of NameExoWorlds, their public process for giving proper names to exoplanets and their host star (where no proper name already exists). [4] [5] The process involved public nomination and voting for the new names. [6]
K-type main-sequence stars, also known as orange dwarfs, may be candidates for supporting extraterrestrial life.These stars are known as "Goldilocks stars" as they emit enough radiation in the non-UV ray spectrum [1] to provide a temperature that allows liquid water to exist on the surface of a planet; they also remain stable in the main sequence longer than the Sun by burning their hydrogen ...
The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun. [4] It is currently predicted to pass 0.1696 ± 0.0065 ly (10 635 ± 500 au) from the Sun in 1.290 ± 0.04 million years from the present, close enough to significantly disturb the Solar System's Oort ...
The red dwarf, of magnitude 11, orbits the white dwarf every 250 years. The 40 Eridani system is 16 light-years from Earth. p Eridani is a binary star with two orange components, 27 light-years from Earth. The magnitude 5.8 primary and 5.9 secondary have an orbital period of 500 years. [1] Artist's impression of a Jupiter-mass planet orbiting ...
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. [14] The brown dwarfs were discovered in 2003. 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.
HD 189733, also catalogued as V452 Vulpeculae, is a binary star system 64.5 light-years (19.8 parsecs) away in the constellation of Vulpecula (the Fox).The primary star is suspected to be an orange dwarf star, [2] while the secondary star is a red dwarf star. [5]