|System:||Wredguia BK-E b39-4 - All bodies|
|Distance to Sol:||482.26 ly|
|Spectral Class:||M - Scoopable|
|Distance To Arrival:||2,460 ls|
|Luminosity Class:||Va - Main-sequence star (dwarf)|
|Age:||634 Million years|
|Surface Temperature:||2,669 K|
|Orbital Period:||6,696.0 D|
|Semi Major Axis:||3.63 AU|
|Orbital Inclination:||-47.29 °|
|Arg Of Periapsis:||327.12 °|
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.
The term dwarf star refers to a variety of distinct classes of stars. The term was originally coined in 1906 when the Danish astronomer Ejnar Hertzsprung noticed that the reddest stars - classified as K and M in the Harvard scheme - could be divided into two distinct groups. They are either much brighter than the Sun, or much fainter. To distinguish these groups, he called them "giant" and "dwarf" stars, the dwarf stars being fainter and the giants being brighter than the sun.