Star whose pressure support is degenerate electrons.

[the ads 13]

My professor gave us a question to think about for discussion next week. He asked how the radius of a star, who is composed of ionized hydrogen and degenerate electrons, varies with mass. I am not quite sure where to start. How could I estimate the radius?

 

[Chronos]

Your professor is asking a question that requires you to consider hydrostatic equilibrium.

 

[marcus]

My professor gave us a question to think about for discussion next week. He asked how the radius of a star, who is composed of ionized hydrogen and degenerate electrons, varies with mass. I am not quite sure where to start. How could I estimate the radius?

If the pressure support is degenerate electrons then you are talking about "electron degeneracy pressure"
http://en.wikipedia.org/wiki/Electron_degeneracy_pressure
That might be a place to start.

 

[Radrook]

My professor gave us a question to think about for discussion next week. He asked how the radius of a star, who is composed of ionized hydrogen and degenerate electrons, varies with mass. I am not quite sure where to start. How could I estimate the radius?

You might find these two links helpful as well.

White dwarf star matter/pressure radius correlation.
http://abyss.uoregon.edu/~js/ast122/lectures/lec17.html


Lecture 19: Extreme Stars
White Dwarfs & Neutron Stars
http://www.astronomy.ohio-state.edu/~pogge/Ast162/Unit3/extreme.html

 

[pmacias]

The radius of a star is primarily determined by its mass, as well as its composition and internal structure. In the case of a star composed of ionized hydrogen and degenerate electrons, the radius will be affected by the pressure support provided by the degenerate electrons.

Degenerate electrons are a result of the Pauli exclusion principle, which states that no two electrons can occupy the same quantum state. This leads to a highly dense and compact state of matter, with the electrons being tightly packed together and unable to collapse further.

The pressure support provided by degenerate electrons is significant, as it can counteract the gravitational force trying to compress the star. As a result, the radius of the star will be smaller compared to a star of the same mass but without degenerate electrons.

To estimate the radius of such a star, we would need to consider the equation of hydrostatic equilibrium, which relates the pressure and density within the star to its mass and radius. However, the exact calculation would depend on the specific equations of state for the degenerate electrons and ionized hydrogen.

In general, as the mass of the star increases, the pressure from degenerate electrons also increases, leading to a smaller radius. However, the exact relationship between mass and radius would also depend on other factors such as the composition and temperature of the star.

In conclusion, the radius of a star composed of ionized hydrogen and degenerate electrons would be smaller than a star of the same mass without degenerate electrons. To estimate the radius, we would need to consider the equations of hydrostatic equilibrium and the specific properties of the degenerate electrons and ionized hydrogen within the star.