the interior of stars i overview hydrostatic equilibrium pressure equation of state stellar energy...
TRANSCRIPT
The Interior of Stars I
• Overview• Hydrostatic Equilibrium• Pressure Equation of State• Stellar Energy Sources
Next lecture• Energy Transport and
Thermodynamics• Stellar Model Building• The Main Sequence
The Interior of Stars I• Calculate This!!!
– Use Knowledge of:• Thermodynamics• Properties of light and how
it interacts with matter• Nuclear Fusion
• Basic Parameters of Star– M: Mass– L: Luminosity
– Te: Effective Surface Temperature
– R: Radius
Energy Generation: Thermonuclear Fusion
Binding Energy of Nuclei can be released in the form of Energy (photons,…)
Overview: Equations of Stellar Structure
• Pressure
• Mass
• Luminosity
• Temperature
• http://abyss.uoregon.edu/~js/ast121/lectures/lec22.html
THERMODYNAMICS(ENERGY
TRANSPORT)
NUCLEAR PHYSICS
GEOMETRY/ DEFINITION OF DENSITY
HYDROSTATIC EQUILIBRIUM
Hydrostatic Equilibrium
• Let’s determine the internal structure of stars!!!
• Some guidance:– Hydrostatic Equilibrium: Balance
between gravitational attraction and outward pressure
Gravity Pressure Gradient
Net Force on Cylinder
Derivation of Hydrostatic Equilibrium
• Substituting 10.2 and 10.3 into 10.1
• Density of Gas Cylinder
• Gives
• Dividing by volume of cylinder
• If star is static, we then obtain:
Pressure Gradientfor hydrostatic equilibrium
The Equation of Mass Conservation
• Relationship between mass, density and radius
• Mass of shell at distance r
Where is the local density of the gas at radius r.
• Rearranging we obtain
Pressure Equation of State
• Where does the pressure “come from”? How is it described?
• Equation of State relates pressure to other fundamental parameters of the material
• Example: Ideal Gas Law
• Derivation of the Pressure Integral for a cylinder of gas of length x and area A
– Newton’s 2nd law
– Impulse delivered to wall
– Average force exerted on wall by a single particle
•What is the distribution of particle momenta?
•The average force per particle is then
•If the number of particles with momenta between p and p+dp is Npdp. Then the total number of particles in the cylinder is
•Contribution to the total force by all particles in the momentum range p and p+dp is
Pressure Equation of stateThe Ideal Gas Law in Terms of the Mean Molecular Weight
• Integrating over all possible values of momenta the total Force is:
• Dividing both sides by the surface area of the wall A gives the pressure P=F/A. Noting that V=Ax and defining npdp to be the number of particles per unit volume
• We find that the pressure exerted on the wall is:
Pressure Integral
Given the distribution function npdp. The pressure can be computed
•Recast in terms of velocities for non-relativistic particles with p=mv
•In the case of an Ideal Gas the velocity distribution is given by the Maxwell-Boltzmann distribution
• Particle number density is
•Substituting into Pressure integral we obtain
Pressure Equation of stateThe Ideal Gas Law in Terms of the Mean Molecular Weight
• Expressing particle number density in terms of mass density and mean particle mass
• The Ideal gas law becomes
• Mean Molecular Weight
• Re-expressing in terms of mean molecular weight
Mean Molecular Weight
• The mean molecular weight depends on the composition of the gas as well as the state of ionization for each species. For completely neutral of completely ionized the calculation simplifies.
• For Completely neutral
• Dividing by mH
•For completely ionized gases, we have
•Where (1+zj) accounts for the nucleus plus the number of free electrons that result from completely ionizing an atom of type j
The Average Kinetic Energy Per Particle
• Combining 10.10 and 10.9 we see that
• This can be re-written as:
• For the maxwell-boltzmann distribution
• Hence the average kinetic energy per particle is
• 3 from 3 degrees of freedom from 3-d space
Fermi-Dirac Statistics
• Particles of half-integral spin are known as Fermions and satisfy fermi-dirac statistics
• Some Fermions: electrons,protons,neutrons
• Influences Pressure….
http://en.wikipedia.org/wiki/Fermi%E2%80%93Dirac_statistics
Bose-Einstein Statistics• Particles of integral spin
are known as Bosons and satisfy Bose-Einstein statistics
• Photons are Bosons
• Influences Pressure….
http://en.wikipedia.org/wiki/Bose%E2%80%93Einstein_statisticshttp://demonstrations.wolfram.com/BoseEinsteinFermiDiracAndMaxwellBoltzmannStatistics/
The Contributions due to Radiation Pressure
• Because photons possess momentum they can generate a pressure on other particles during absorption or reflection
• The Pressure integral can be generalized to photons
• In terms of energy density
• For a blackbody distribution one has
Total Pressure=Gas Pressure+Radiation Pressure
http://hyperphysics.phy-astr.gsu.edu/hbase/starlog/staradpre.html#c1
Stellar Energy SourcesGravitation and the Kelvin-Helmholtz Timescale
• One likely source of stellar energy is gravitational potential energy.
• Graviational potential energy between two particles is
• Gravitational force on a point particle dmi located outside of a spherically symmetric mass Mr is:
• The potential energy is then
• Consider a shell with
Integrating over all mass shells from the
center to the surface
Where is the mass density…Thus
Energy Generation: Thermonuclear Fusion
Binding Energy of Nuclei can be released in the form of Energy (photons,…)
The Nuclear Timescale
• The binding energy of He nucleus is
• This energy can be released thru a process in which 4 protons are combined into a He nucleus through the process known as Fusion. This particular reaction can occur through several processes …p-p chain, CNO cycle,….
• How much energy is available in a star from this fusion process?