Since the Sun consists of a plasma and is not solid, it rotates faster at its equator than at its poles. This behavior is known as differential rotation and is caused by convection in the Sun and the movement of mass, due to steep temperature gradients from the core outwards. This mass carries a portion of the Sun’s counter-clockwise angular momentum (as viewed from the ecliptic north pole), thus redistributing the angular velocity. The period of this actual rotation is approximately 25.6 days at the equator and 33.5 days at the poles. However, due to our constantly changing vantage point from the Earth as it orbits the Sun, the apparent rotation of the star at its equator is about 28 days.
the most accurate method of "weighing" a star is by use of the Doppler shift.
To find the mass of the Sun we take advantage of the planets orbiting it. Each planet requires a centripetal force to keep it from flying away; this force is supplied by the Sun's gravity. Setting these two forces equal to each other we can write an equation (also in introductory physics books):
Force of Gravity = Centripetal Force
(G x MSun x Mplanet) / (r x r) = (Mplanet x V x V) / r
simplifying the equation we see the the mass of the planet cancels out (using algebra) so:
MSun = (V x V x r) / G
Binary stars are used to calculate the weight of other stars.
We measure the velocity of each star (V) using the Doppler shift and the distance between each star the their common center of mass (r) (which is found by taking pictures of the stars through a telescope). So we can find the total mass of the stars using the same equation as above.