# Difference between revisions of "Radiative Equilibrium"

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+ | [[Radiative Processes in Astrophysics|Course Home]] | ||

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===Short Topical Videos=== | ===Short Topical Videos=== | ||

* [http://youtu.be/VS3KgsISIqQ Radiative Equilibrium (Aaron Parsons)] | * [http://youtu.be/VS3KgsISIqQ Radiative Equilibrium (Aaron Parsons)] | ||

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Take a sphere at surface temp $T$, with some gas (matter) inside it. Allow | Take a sphere at surface temp $T$, with some gas (matter) inside it. Allow | ||

to come to thermal equilibrium. Inside the sphere, | to come to thermal equilibrium. Inside the sphere, | ||

− | you see a [https://casper.berkeley.edu/astrobaki/index.php/Black-Body_Radiation#Blackbody_Radiation | + | you see a [https://casper.berkeley.edu/astrobaki/index.php/Black-Body_Radiation#Blackbody_Radiation Planckian spectrum] ($I_\nu = B_\nu$). Now suppose you take a box of |

gas (it is both emissive and absorbent) and shoot rays of photons through | gas (it is both emissive and absorbent) and shoot rays of photons through | ||

that box. According to the [[Radiative Transfer Equation]], these photons suffer some absorption: | that box. According to the [[Radiative Transfer Equation]], these photons suffer some absorption: |

## Revision as of 15:25, 5 December 2017

### Short Topical Videos

### Reference Material

### Need a Review?

- Radiative Transfer Equation
- Black-Body Radiation
- Boltzmann distribution
- Local Thermodynamic Equilibrium

### Local Thermodynamic Equilibrium (LTE)

Local Thermodynamic Equilibrium means

where is *local*. Take a sphere at surface temp , with some gas (matter) inside it. Allow to come to thermal equilibrium. Inside the sphere, you see a Planckian spectrum (). Now suppose you take a box of gas (it is both emissive and absorbent) and shoot rays of photons through that box. According to the Radiative Transfer Equation, these photons suffer some absorption:

But those photons also pick up some intensity:

But since the photons should not pick up energy going through the box (everything is at the same temperature),

Now suppose you let all the photons out of this sphere. Those photons will no longer be in thermal equilibrium with the gas. Suppose we magically fix the temperature of the gas at this point. The source function will remain the same (it will still be the case that ) because the source function *is a property of the matter alone* (the absorptive and emissive properties of it). However, .

Suppose we look along a column of this gas. At each point, the source function will be: . Therefore, along that column will be:

### Radiative Equilibrium and Relations among Einstein Coefficients

Assume we have many atoms with 2 energy states, and is the # density in state 1, ditto for . Assume we are in thermal, steady-state equilibrium, so:

This is because as many atoms need to be going from energy state 1 to 2 as visa versa. A second relation is: . Using the Boltzmann distribution, :

In thermal equilibrium is given by the Planck Function:

Combining this with earlier, we get:

and