# 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.

## This Post Has 10 Comments

1. jennyderath12 says:

D. Binary Star Systems

Explanation:

2. Nerdyprincesd8689 says:

D.

Explanation:

3. melaniegilbreath says:

Stable white dwarf star

4. Angel4345 says:

The answer is a white dwarf star

5. babycakesmani says:

1:D
2:A
3:D
4:B
5:D

6. brianna8739 says:

1:D
2:A
3:D
4:B
5:D

7. ethanm2685 says:

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.

8. murtaghliam1 says:

C. Binary star systems

Explanation:

9. julielebo8 says:

C. Binary star systems

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 $\mu = \frac{M_{1} \cdot M_{2}}{M_{1} + M_{2}}$ moving in the potential generated by the total mass (M1 + M2) considered at rest. Hence, we can determine the masses of the two stars.