The chandrasekhar limit states that the final mass of a star can be no greater than 1.4 solar masses.

The chandrasekhar limit states that the final mass of a star can be no greater than 1.4 solar masses.

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  1. Normally a newborn star is about 150 times the mass of the sun. So the sun is 10.6 kg/s. So multiply it and you get 1590 kg/s.

  2. C. Binary star systems

    Let’s see your options:

    a) The color of the star: the color is not used in calculating the mass of a star, because it has no relation to it. Think about a red supergiant and a red dwarf: they have the same color, but they are completely different stars, with respectively a big and a small mass.

    b) Kepler’s laws: these laws can be applied in what is called the “approximation of 1 body”, which means that is assumed that one body has a much bigger mass than the other and can be considered at rest. This is the case of a star-planet system and the mass that can be calculated is that of the planet.

    c) Binary star systems: these are the only cases in which is possible the direct measure of the mass of the stars. Binary systems are classified as follows:
    - Visual binaries: each star can be resolved and the motion around the center of mass can be measured.
    - Astrometric binaries: only one star is visible, but the presence of the companion can be inferred by the movement of the first star around the system’s center of mass.
    - Eclipse binaries: the two stars are not resolved (separated), but the luminosity varies periodically when one star eclipses the other.
    - Spectroscopic binaries: the two stars are not resolved, but their spectrum reveals that they are a binary system.
    In all these cases we have a “two-body problem” that can be solved by changing system of reference: the motion of bodies 1 and 2 is equivalent to the motion of a body of mass equal to the system’s reduced mass [tex]\mu = \frac{M_{1} \cdot M_{2}}{M_{1} + M_{2}}[/tex] moving in the potential generated by the total mass (M1 + M2) considered at rest. Hence, we can determine the masses of the two stars. 

  3. Answer:

    The mass of a star can be determined by studying binary star systems.


    In this system it consists of two stars, revolving round the same bary-centre. The systems having two or may say more than two are called as the multiple star system. This zone is also a habitable zone, here the water exists in the liquid form. We could have sometime seen the two stars together. They are also very capable of strengthening the terrestrial planets inside the stable orbital ranges. They have generally two orbits like P-type as well as circumbinary.  

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