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JJ
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I have no idea. And how is the pressure/force/intensity of gravitational collapse known?
Forget not the magic words "with varing degrees of accuracy"JJ said:*SNIP
And Nereid, I hadn't approached the problem from such a simple direction. Though couldn't you know the rough density from only two of those variables?
The formula for calculating the density of a white dwarf star is ρ = 3M/4πR^3, where ρ is the density, M is the mass of the star, and R is the radius of the star.
The mass of a white dwarf star is determined through observations of the star's binary system, where the gravitational pull of the white dwarf on its companion star can be measured. This allows astronomers to calculate the mass of the white dwarf using Newton's law of gravitation.
The typical density of a white dwarf star is very high, ranging from 10^5 to 10^9 kg/m^3. This is because the mass of a white dwarf is similar to that of the Sun, but it is compressed into a much smaller volume.
The density of a white dwarf star is much higher than that of other stars, including the Sun. This is due to the fact that white dwarfs are formed from the remnants of low to medium-mass stars, which have exhausted their nuclear fuel and collapsed under their own gravity.
Yes, the density of a white dwarf star can change over time. As it cools and loses heat, the electrons in the star's core become more closely packed, increasing the density. However, this change is very gradual and would not be noticeable over a human timescale.