NOTE: See below for credit on the data source

Credit:

The table data was obtained from SpaceGear.Org's SCTable version 3.0 09/23/2003. The following data source was obtained from their SCTable web page:

Absolute magnitude was derived from the standard Hertzsprung-Russell (HR) diagram. The book Stars and Their Spectra by James B. Kaler was used as a resource for deriving the absolute magnitude for each possible luminosity class. Classifications N, S, WC, WN, C, and R are mapped as follows:

• N and S are equivalent to M.

• WC and WN are equivalent to O.

• C spans G4 to M9.

• R spans G4 to M0.

Temperature was derived from the relationship between luminosity class and spectral class. The book Stars and Their Spectra by James B. Kaler and Mitchell Charity's work on star colors was used as a resource for deriving temperature for Main Sequence (V), Supergiant (Ia), Giant (II), and Dwarf (D) luminosity classes. Luminosity classes Ia0, Ib, III, IV, and VI are mapped as follows:

• Temperatures of Ia0 and Ib are equivalent to Ia.

• Temperatures of II is equivalent to III.

• Temperatures of IV and VI are equivalent to V.

Color was derived from Mitchell Charity's work on star colors. Each designated color is defined with at least one field (R, G, or B) at full saturation (value equals 255). Actual color values for display would be attenuated across all color components based on the star's apparent magnitude in a given situation.

Mass was derived from many sources including Astrophysical Formulae by Kenneth R. Lang. Many rows are heavily interpolated from known data on star mass.

NOTE:

On the Data page, SpaceGear.org indicate that their Stellar Classification Table has no usage restrictions. It is published WITHOUT ANY WARRANTY; without even the implied warranty of MERCHANTABILITY, FITNESS FOR A PARTICULAR PURPOSE, or ACCURACY.

Extension of SCTable:

The Stellar Classification Table was extended by chongo to include a number of Stellar parameters:

• Luminosity L_star/L_sun
  

  L_star = 10^{((4.75 - M_bol)/2.5)}
  M_{bol_sun} = 4.75
  L_sun = 10^{((4.75 - 4.75)/2.5)} = 1

• Radius R_star/R_sun
  

  R_star/R_sun = (L_star/L_sun)^1/2 / (T_star / T_sun)²
  R_sun = 1
  T_sun = 5780 K

• Color Index B-V
  

  if log₁₀(T_star) ≤ 3.961
  

  B-V = -3.684*log₁₀(T_star) + 14.551
  

  if log₁₀(T_star) > 3.961
  

  B-V = 0.344*(log₁₀(T_star))² + -3.402*log₁₀(T_star) + 8.037

• Bolometric Correction BC(Temp)
  

  BC(T_star) = -8.499*(log₁₀(T_star)-4)⁴ + 13.421*(log₁₀(T_star)-4)³ + -8.131*(log₁₀(T_star)-4)² + -3.901*(log₁₀(T_star)-4) + -0.438

• Bolometric Magnitude M_bol
  

  M_{bol_star} = M_{v_star} + BC(T_star)
  M_{v_sun} = 4.83