Semester 1 - Formulae Flashcards

1
Q

Spherical trig

A

sinA/a = sinB/b = sinC/c

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2
Q

Specific flux

A

Fv = (2π ∫ 0) (π/2 ∫ -π/2) Iv (θ,φ) cosθsinθdθdφ

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3
Q

μ and dμ

A

μ = cosθ
dμ = -sinθdθ

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4
Q

integrating factor

A

dy/dx + P(x)y = Q(x)

where the integrating factor is μ(x) = exp^( ∫P(x)dx)

hence the ODE becomes

d/dx (μ(x)y) = μ(x)Q(x)

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5
Q

intensity emitted

A

dIv = p jv ds

where jv is the emission coefficient

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6
Q

intensity absorbed/gained

A

dIv = -p kv Iv ds

where kv is the absorption coefficient

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7
Q

optical depth

A

dτv = pkvds

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8
Q

angle-dependent definition of optical depth

A

dτv,μ = -dτv/μ

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9
Q

mean intensity

A

Jv = 1/4π ∮ Iv dΩ

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10
Q

equation of transfer

A

μ dIv/dτ = Iv - Sv

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11
Q

relation between eddington flux and k integral

A

Hv = dKv/dτ

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12
Q

total momentum

A

dp = dEv/c cosθ

where dp is the total momentum

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13
Q

dEv =

A

IvcosθdAdΩdt

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14
Q

dΩ =

A

sinθdθdφ

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15
Q

Eddington approximation

A

K = I/3 = J/3

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16
Q

Eddington Barbier relation

A

F = π Sv

where Sv ~ Bv

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17
Q

equation of transfer in terms of absorption and emission coefficient

A

dIv/ds = p jv - pkv Iv

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18
Q

Source function

A

Sv = jv/kv

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19
Q

line depth

A

Aλ = 1 - Rλ

where Rλ = Fλ/Fc

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20
Q

in a naturally broadened line to find the normalisation constant.

A

∆v = v - v0 = 0

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21
Q

HWHM

A

HWHM = ∆v

when

I = Ipeak/2

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22
Q

Heisenberg’s Uncertainty Principle

A

∆E∆t > ℏ/2

23
Q

Planck’s law

A

∆E = h∆v

24
Q

apparent equatorial velocity

A

vm = v0sini

25
Q

rotational broadening HWHM

A

HWHM = ∆λ

26
Q

rotational broadening ∆λ =

A

vm λ0 µ/c

27
Q

Intensity is constant along a ray path

A

show that dIv/ds = 0

This occurs when the emission coefficient and total absorption coefficient = 0

which occurs when there are no sources or sinks

28
Q

Energy density

A

du = dE/dV

where dV = dAcosθl

where dt = l/c

29
Q

Components of flux

A

Fv =Fv+ + Fv-

Split the limits

30
Q

Total absorption coefficient

A

kv = kappa v + σv

31
Q

Mean free path

A

L = 1/σvp = 1/Nσ

32
Q

Planckian Atmosphere

A

J = B = S

33
Q

Integrated Planck function B

A

B = σ/pi T^4

34
Q

Integrated flux F

A

F = σTe^4

35
Q

Rosseland Mean Opacity

A

Start from K integral and definition of opacity

Kv = Jv/3 = Bv/3

rewrite for Hv

dB/dT dT/ds

Integrate Hv over all frequencies

divide two versions of H

use relation for B

36
Q

Einstein coefficient Cij and Cji

A

Cij/Cji = gj/gi exp(-hv0/kT)

Collision processes

37
Q

Line formation of a weak atomic line

A

τc = 2/3 + Δτ

and kλ = kl + kc

38
Q

Doppler shifts

A

Δv/v = -Δλ/λ

39
Q

microturbulence

A

V0^2 = Vthermal^2 + Vturb^2

40
Q

line of sight velocity

A

vr = veq sin θ sin φ sin i

41
Q

Show S = 3F/4pi (tau + C)

starting from dKv/dtau= Hv = Fv/4pi

A

grey atmosphere means no frequency dependence
Eddington’s approximation K = I/3 = J/3
J = B = S in a Planckian atmosphere

dB/dtau = 3F/4pi

integrating gives as required

42
Q

At the surface

A

tau = 0

43
Q

At the edge

A

mu = 0

44
Q

at the centre

A

mu = 1

45
Q

Radiation Pressure

A

dPrad/dr = -pgrad

where grad is on the formula sheet

46
Q

Integration limits for solutions to the equation of transfer

A

(τ2 ∫ τ1) for the outward direction τ2 = τ0 and τ1 -> infinity

for the inward direction replace mu with -mu

47
Q

Show that the ratio of intensities at the limb and centre is 40%

A

I(0,0)/I(0,1) = 0.4

48
Q

Doppler shift

A

Δ λ/λ = Δ v/v

49
Q

Show Fv = πIvR^2/r^2

A

Draw a star with a resolvable disc

Start with definition of flux with limits pi/2 to -pi/2 and theta to -theta.

Use spherical trig. relationship and change variables

50
Q

Solving the equation of transfer ; dIv/dτ = Sv - Iv.

A

State equation of transfer

Use an integrating factor

Integration limits are τv and 0.

51
Q

Show that dFv/dτ = 4pi(Jv -Sv)

A

dHv/dτ = 1/4pi dFv/dτ

use equation of transfer

52
Q

Determine the constant, C, if I = 3F/4pi (τ+mu+C) by considering the conditions at the surface of a star.

A

At the surface of the star τ = 0 and looking radially outwards.

Definition of flux insert definition of I. Solve for C. Where C = 2/3.

53
Q

Eddington-barbier source function.

A

S(τ) = a0 + a1τ

54
Q

Show that A = 2/3 kL/kc d(lnBv)/dτ

A

Line depth use Eddington barrier relation Fv = piBv

Taylor expand around small t

replace τ through definition of opacity