The luminosity of a star is related to its surface temperature and radius as:
`L = 4piR^2 sigma T^4`
Where L is the luminosity in Watts, R is the radius in meters, `sigma` is the Stefan-Boltzmann constant (5.67 x 10^-8 Wm^-2K^-4), and T is the star's surface temperature in Kelvin. In solar units,
`L_(Star)/L_(Sun) = R^2/(R_S^2 ) ×T^4/(T_S^2 ) `
`=3^2*(10000/5800)^4` (assuming the surface temperature of Sun to be 5800K)
Therefore, the star has a luminosity, 80 times that of the Sun.
In units of `Wm^-2` , the luminosity is obtained by putting the values of `sigma` and the solar radius,
`L_(Sun)=4 xx pi xx(1.5 xx 10^11m)^2xx1.4xx10^3 wm^-2=3.85xx10^26 W`