Semester 1 - Formulas Flashcards
Gravity
g(r) = Gm(r)/r^2
Hydrostatic Equilibrium
dP/dr = -p(r)g(r)
Gravitational Potential Energy
Ω = -GM^2/R
number density
n = p/mH
Mass
M = Vp
M = 4/3 πR^3 p
M = ( R ∫ 0) dm(r)
Core Pressure
P(c) = P(gas,i) + P(deg,e)
i = ions
e = electrons
Adiabatic Index
gamma = 1 + 1/n
Mean Free Path Derivation
s(bar) = l1(bar) + l2(bar) + l3(bar) + … + lN(bar)
s^2 = Nl^2
t = l/c
l = 1/nσ
Mean Free Path
l = 1/nσ
Gas Pressure
Pg = nkT
Radiation Pressure
Prad = 1/3 aT^4
a = 4σ/c
Degeneracy Pressure (non-relativistic and relativistic)
P = Kn^5/3 (non-relativistic)
P = Kn^4/3 (relativistic)
characteristic energy-loss timescale
τ = E/L
kelvin-helmholtz timescale
τ = Ω/L
potential energy of a star
m(r) = ( r ∫ 0) dm
if m = 4/3πr^3 p
dm = 4πp(r)r^2dr
Ω = - ( M* ∫ 0) Gm(r)dm/r
hydrostatic equilibrium derivation
A[P(r) - P(r+∆r)] - g(r)p(r)A∆r = 0
Taylor expand P(r+∆r)
P(r) + dP/dr ∆r + …
free-fall timescale derivation
a = dv/ dt = -Gm/r^2
dv/dt = 1/2 dv^2/dr
integrate and solve for v
free fall timescale = (0 ∫ r0) dt/dr dr
substitute in 1/v , change variables x = r/r0 and integrate
x = sin^2 theta => pi^2/4
Virial Theorem Derivation
start from hydrostatic equilibrium
multiply both sides by volume and integrate over r
RHS
dm = 4πr^2pdr
Ω = (M ∫ 0) Gmdm/r
LHS
integrate by parts at R, P=0
dm = 4πr^2pdr
- (V ∫ 0) PdV
P = nkT