|System:||HIP 20485 - All bodies|
|Distance to Sol:||153.45 ly|
|Spectral Class:||M - Scoopable|
|Distance To Arrival:||2,965 ls|
|Luminosity Class:||IVb - Subgiant|
|Age:||10,882 Million years|
|Surface Temperature:||2,320 K|
|Orbital Period:||4,292.0 D|
|Semi Major Axis:||4.34 AU|
|Orbital Inclination:||-13.29 °|
|Arg Of Periapsis:||0.27 °|
Class M stars are red stars that form the bulk of the main sequence stars in the galaxy. Their mass is low, as is their surface temperature.
A subgiant is a star that is slightly brighter than a normal main-sequence (dwarf) star of the same spectral class, but not as bright as true giant stars. Although certain subgiants appear to be simply unusually bright metal-rich hydrogen-fusing stars (in the same way subdwarfs are unusually dim metal-poor hydrogen-fusing stars), they are generally believed to be stars that are ceasing or have already ceased fusing hydrogen in their cores. In stars of roughly a solar mass (M☉), this causes the core to contract, which increases the star's central temperature enough to move hydrogen fusion into a shell surrounding the core. This swells the star on the way to becoming a true giant.