state of stellar material
Having determined an expression for the
minimum mean temperature of a star,
we can now determine the physical state of the material of
which stars are composed.
We have the inequality:
We know the values of Ms and rs
for the Sun. We can estimate the mean particle mass, m, by
assuming that the Sun is composed of nothing other than hydrogen atoms,
the most abundant element in stars, which have a mass of
1.67 × 10-27 kg.
These values can be inserted into the inequality to give:
4 × 106 K.
This is much higher than the measured surface temperature of the Sun
(Te = 5780 K).
We can obtain a more accurate constraint by noting that the above
minimum mean temperature
far exceeds the temperature at which hydrogen is fully ionized. There will
then be two particles for each hydrogen atom - a proton and an electron -
and the mean particle mass will hence become
½(1.67 × 10-27) kg,
resulting in a revised inequality:
2 × 106 K.
We can also estimate the mean density of the Sun using the relation:
1.4 × 103 kg m-3.
So, the above figures tell us that the mean density of the Sun is
similar to that of ordinary liquids like water. We know that liquids like
water turn to gases at temperatures far lower than
2 × 106 K. Furthermore, at these extreme temperatures,
the average kinetic energy of the particles is much higher than the energy
required to remove all but the most tightly bound electrons from the atoms,
hence the gas will be highly ionised. Such a gas is known as a
plasma. Since the gas is ionised, it can withstand much greater
compression without deviating from an ideal gas (which, in effect,
demands that the distances between particles are much greater than their
sizes, so that the inter-particle forces are negligible except during a
collision) because a typical
nuclear dimension is 10-15 m compared with a typical atomic
dimension of 10-10 m.
But what about our assumption that the radiation pressure is negligible?
Radiation pressure is the pressure exerted by photons on the particles
in a gas and is given by:
Prad = aT4 / 3,
where a is the radiation density constant.
We can estimate the importance of radiation pressure at a typical point
in the Sun by comparing it with the gas pressure, as follows:
Taking T ~ Tav = 2 × 106 K,
~ av = 1.4 × 103 kg m-3
and m = ½(1.67 × 10-27) kg,
Pgas ~ 10-4.
It does appear as if radiation pressure is indeed negligible at an average
point in the Sun.
In summary, with no knowledge of how energy is generated in
stars, we have been able to derive a value for the Sun's internal
temperature and deduce that:
Stars are composed of near ideal gases (plasmas) with negligible
This is not true of all stars, however. Radiation pressure is of
importance in the hottest stars, and some stars are much denser than
the Sun and hence corrections to the
ideal gas law are very important.
©Vik Dhillon, 27th September 2010