I’ve spent a lot of time trying to answer certain questions in astronomy, where I just want a rough approximation for the purpose of a simulation, and don’t need an exact answer. These are some of the equations I’ve come up with.
Temperature (K) → Absolute Magnitude (visual):
Mv = 35.463 * exp(-0.000353 * T)
Roughly accurate between 2000-50000 Kelvin. Probably doesn’t continue accuracy at hotter temperatures.
Absolute Magnitude (visual) → Luminosity (solar luminosities):
Lsun = 100 * exp(-0.944 * Mv)
Accurate between 0-10 Mv. Probably continues accuracy relatively well.
Spectral (UBVRI) Filters:
Ultraviolet, Blue, Visual, Red, Infrared.
Objects are listed in different indexes:
U–V for the hottest objects (stellar remnants, galaxies), then B–V (the majority of stars), and R–I for the coolest (LTY “stars” and below).
B-V index (x) → Temperature (K):
T = -772.2x3 + 3152x2 – 6893x + 9500
Sorta accurate between 0-2. (This equation I am least comfortable with, and don’t plan to use.)
Main Sequence Luminosity/Mass Relation:
Lstar / Lsun = (Mstar / Msun)3.5
Yerkes Classes’ T/Mv Relations
These equations are shown as functions where x is temperature in Kelvin, and f(x) is absolute visual magnitude. Most are valid from 2400 K to a little bit past 30000 K, the exceptions are noted. For the hypergiants and white dwarfs, the range is within an elliptical region, of which these functions define the major axis; for all others, they are a center-point along a Yerkes classification.
f(x) = -8.9
f(x) = -0.00135x3 + 0.0233x2 + 0.0187x – 7.349
f(x) = 0.00329x3 – 0.0962x2 + 0.829x – 7.209
Bright Giants (II):
f(x) = 0.00557x3 – 0.166x2 + 1.505x – 6.816
f(x) = 0.0135x3 – 0.373x2 + 3.019x – 7.233
f(x) = -0.151x2 + 2.216x – 5.128 (4450-100000 K only)
f(x) = 0.00193x5 – 0.0615x4 + 0.742x3 – 4.257x2 + 12.439x – 12.996 (note: this one is the least accurate)
f(x) = 0.131x3 – 3.275x2 + 27.576x – 71.7 (3050-6000 K only)
White Dwarfs (VII):
f(x) = 0.489x + 10.01 (4450-30000 K only)