You ought to be able to get most of this info from links starting on http://www.astronomynotes.com/starprop/chindex.htm" .blumfeld0 said:Hello. what equation do i use to figure out how many .75*Msolar main sequence stars would it take to equal the luminosity of one 3*Msolar O tpe star?
I know O type are much brighter but how many times brighter?
thank you
blumfeld0 said:Hello. what equation do i use to figure out how many .75*Msolar main sequence stars would it take to equal the luminosity of one 3*Msolar O tpe star?
I know O type are much brighter but how many times brighter?
SpaceTiger said:I would use a table, but if you can't find one, the mass-luminosity relation should be fine:
[tex]\frac{L}{L_{sun}} \propto (\frac{M}{M_{sun}})^{3.5}[/tex]
Luminosity refers to the total amount of energy radiated by a star or other astronomical object per unit time.
Luminosity for M type stars is measured using the bolometric luminosity, which takes into account the emission of all wavelengths of light.
The luminosity of M type stars is affected by their size, temperature, and composition. Larger and hotter stars tend to have higher luminosity, while those with a higher metallicity (amount of elements other than hydrogen and helium) may have lower luminosity.
M type stars, also known as red dwarfs, are the smallest and coolest type of main sequence stars. They have relatively low luminosity compared to other types of stars, such as O type stars which are the largest and hottest.
The luminosity of M type stars provides valuable information about their physical properties and evolutionary stage. It can also help us understand the formation and evolution of galaxies, as M type stars are the most common type of star in the universe.