|System:||Cephei Sector RT-R b4-3 - All bodies|
|Distance to Sol:||107.38 ly|
|Spectral Class:||M - Scoopable|
|Luminosity Class:||VI - Subdwarf|
|Age:||8,510 Million years|
|Surface Temperature:||2,160 K|
|Orbital Period:||33,047.0 D|
|Semi Major Axis:||4.17 AU|
|Orbital Inclination:||-27.50 °|
|Arg Of Periapsis:||314.66 °|
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 subdwarf, sometimes denoted by "sd", is a star with luminosity class VI under the Yerkes spectral classification system. They are defined as stars with luminosity 1.5 to 2 magnitudes lower than that of main-sequence stars of the same spectral type. On an Hertzsprung–Russell diagram subdwarfs appear to lie below the main sequence.
The term "subdwarf" was coined by Gerard Kuiper in 1939, to refer to a series of stars with anomalous spectra that were previously labeled as "intermediate white dwarfs".