Astrophysics (Index) | About |

There is a general model of **stellar structure**
(**stellar-structure model** or **stellar model**) consisting of
a hot region in the center where fusion is
releasing energy (the stellar core), a region near the apparent
surface of the star that generates the light that escapes
(the photosphere), and regions in between that transfer the
energy from core to photosphere via electromagnetic radiation (i.e., radiative transfer)
and/or **convection**
(transfer of heat by movement of bulk amounts the material holding the heat)
with **conduction**
(transfer of heat by collision of particles)
generally only a minor factor.
The structural details depend nearly entirely
on the mass and age of the star, the smaller or rarer
factors including the initial chemical composition
(characterized by its metallicity),
the rotation rate, and nearby companions.

Large mass stars (during their main sequence) have CNO cycle fusion in the core, with a region surrounding it conveying energy via radiative transfer, the inner part of which also has some proton-proton chain fusion, which can be triggered by somewhat lower temperatures. Small mass stars such as red dwarves have only proton-proton chain fusion in the core, and transfer energy through convection. Between are stars like the Sun, which have an inner portion much like a large star, with a convection layer surrounding it.

The most basic mathematical model includes four differential equations
(**stellar-structure equations**)
relating changes in mass, temperature, luminosity, and
pressure to the distance from the center of the star.
They presume local thermodynamic equilibrium and hydrostatic equilibrium.

dm —— = 4πr²ρ dr

(The **mass continuity equation** aka **mass conservation equation**:
density is assumed constant at distance r from the center)

dP Gmρ —— = - ——— dr r²

(pressure counteracts gravity at distance r from the center)

dL —— = 4πr²ε dr

(The **luminosity equation**: energy is conserved,
any addition is from fusion at that level)

dT 3κρL —— = ———————— dr 64πr²σT³

(Opacity directly affects the rate at which temperature changes with radius,
i.e., the **temperature gradient**.
This is the equation for radiative transfer, i.e., energy transfer via
EMR; Other equations are needed if heat conduction is significant
or if there is convection, which can happen if the temperature
gradient is sufficiently high.)

- r - distance from the center of the star, i.e., radius of a spherical portion of the star centered at the star's center.
- m - mass of the star within distance r from the center.
`ρ`- density, a function of r, i.e., the same at all points equidistant from the center.- L - luminosity, the rate at which energy is flowing from inside r to outside r.
- T - temperature at r, also modeled as being the same at all points equidistant from the center.
- P - pressure at r, also modeled as being the same at all points equidistant from the center.
- ε - nuclear energy generation rate, the amount of energy generated by fusion per unit of volume at r.
`κ`- opacity at r.- G - gravitational constant.
- σ - Stefan-Boltzmann constant.

Opacity, density, and energy generation are functions of temperature and pressure and it is key that simple-but-effective approximate models have been developed (equations of state).

Among approximations used to make the behavior of a star's atmosphere (stellar atmosphere) more tractable are the plane-parallel atmosphere approximation (ignoring the curvature of its layers) and the gray atmosphere approximation (ignoring the wavelength-dependence by using values averaged over wavelength). Also used is the Eddington approximation.

To model a star,
these are generally solved using **difference equations**, approximating
the differential equations by calculating differences over a small value.
A star with these equations, a set of consistent
**boundary conditions** needs to be determined/selected.
Some are clear: m, L must be zero at the center (where r = 0), while
ρ, P, and T must be (essentially) zero at the surface
(the maximum value of r).
Since any numerical calculations must begin at a point
with values for all the variables,
guessing is required and multiple calculation attempts
are likely needed to satisfy the above five constraints.
Codes using this approach are called **Eulerian codes**:
an alternative is **Lagrangian codes**, that specify (changes in)
values in relation to dm rather than dr, i.e., mass rather than
radius.

A stellar model specific to the Sun is a **solar model**,
the current favorite being designated the **standard solar model** (**SSM**).

http://en.wikipedia.org/wiki/Stellar_structure

http://personal.psu.edu/rbc3/A534/lec2.pdf

http://www.vikdhillon.staff.shef.ac.uk/teaching/phy213/phy213_solution.html

https://www.astro.princeton.edu/~gk/A403/stellar.pdf

binary star

binding energy

Boltzmann equation

Eddington approximation

emission coefficient (j)

FGK star

giant planet

gray atmosphere

Lane-Emden equation

line blanketing

luminosity (L)

mass shell

mixing length theory

nuclear energy generation rate (ε)

planet structure

presolar grain

quantum tunneling

equation of radiative transfer (RTE)

RT instability

shell

specific heat

spectral class

stellar astronomy

stellar evolution

stellar temperature determination

subgrid-scale physics

Sun

variable star