Temperatur im Inneren der Sonne
Pressure,
density and temperature inside the Sun
To be in a steady state the thermal gas pressure of the star must be in equilibrium with gravitation. First, we estimate the gravitational pressure in the centre of the star:
p = F / A = G·ρ·M / R The ratio p / ρ is given by On
the other hand, the pressure p of the star, considered as an ideal gas
of N atoms of mass m ( k = Boltzmann constant, T = abs. Temperature) With
ρ = N·m _{A}To be stable the following equation must be valid: _{A}For the temperature T we get _{A}·M / (k R)
m M = 2·10 k = 1.4·10 R = 7·10 constant of gravitation mass of hydrogen atom mass of the Sun Boltzmann constant radius of the Sun T =
2.3·10 A more realistic value is 15,000,000 K (surface temperature: 5800 K) The pressure in the centre of the Sun with
the mean density ρ = 1.4·10 ^{14} N / m^{2} =
2.7·10^{9} barThe real value should be greater because the density increases towards the center.
Our Sun and Stellar Structure (Bakersfield College)
The Sun's Power Source (Bakersfield College) How the Sun Shines Last
update 2007 Aug 23 |