˘ ˇ ˆ ˙ˇ˝piskunov/TEACHING/NORDITA_MS2006/MasterClass2006_0… · ˝˝ˇ, I+ q I- q t Stellar...
Transcript of ˘ ˇ ˆ ˙ˇ˝piskunov/TEACHING/NORDITA_MS2006/MasterClass2006_0… · ˝˝ˇ, I+ q I- q t Stellar...
! ""# " "!! $" % $ & ' %! % () % ) *&
+ # # # % &, &#&# # # #%, # &
% # #! %"! + & %!% ( % ))% ) * +"- &
. % + %
/ , "
"# % % %& ! ' + % # , -! % # 0
topgas rad
bottomgas rad
( )
( )
F g V P P
P P
ρ σ
σ
↓ ↓
↑ ↑
= − ∆ − + ⋅ +
+ + ⋅
0F =
, , gT P kνρ
ρ∆
σtop
/% , % % $ 1 &#&%!% , # ! $
#+ % " #% , # 2 # $ , 34, " ! # # !&
1 1 nP K ρ +=( )gas rad
22 0
1 1gas
( )
( ) 4r
n
d P Pg r
drG
g r s dsr
P K
ρ
ρ π
ρ +
+= −
=
=
gas rad gas(1 )P P Pβ+ ≡ + ⋅
Example of the Solar atmosphere /
≈96: 1&/ !
,2 % ;6411&/
≈ 644 # #+!
( #+!*3&96<= # "! &4>, % &/ #+! ?% ## &#
3<&<<
% # # !(@ ?*# % &2 + % σ <3
/ % # )% ) ! % + , A
$ / " + 1 % #( 7' *&% + % % !) &#&
+ !" ?,
1 #!%
7' " #! + %%
" , #
P kT N= ⋅k
e eP kT N= ⋅
2 2 3 2m kT=
part total( ) / exp( 2 )N N m kT→ ∆ ∝ − ∆
exp( )i iN E kT∝ −
.% ,
θI+
I-
θτ
Stellar surface
Stellar interiors
s - geometrical depth
τ - optical depth, pointsdown
θ- angle between thebeam and the normalto the surface. Wedefine µ≡cosθ, so thatthe path through thephotosphere is µ∆sor µ∆τ
I± - are the intensities of the two radiation streams
Atmosphere
%(. * ! F #56 5 B'56 56GF #56 5 H56 56G&
$
!% F #56 54 B'56 56G&
?% % % %
" & !F#54G ? " F #56G), + ? F56G&
2E I I I I cλ ν λ ν
νλ ν∆ ≡ ∆ = ∆ =
dI k I ds j dsν ν ν νρ= − +Jν
k dsν ρ
+ #%
%!1=
+ $
)()0()( seIsI ντ−νν =
0 0
e d e dν ντ τν ν ντ τ τ
∞ ∞− −
ν
νντ −τ−
ντ−
ννν +=τ0
)()()0()( dtetSeII t
$ ! $"( ,#+! *
+ , 1 , " , #% ! ++ % , #
, # % , ++ $ #! + $ &
gas rad
2rad
1cos sin
4
dP dPg
ds ds
P I dπ
νπ
ρ
θ θ θπ
+
−
+ = −
= Iνρ
gas kP Tmρ=
! 2$" / % + % % ( &#& )#* ' "!% ! % &" + $1!" , # , % &-' .-/
'()% % # # ! % %&% %, !K#L&
, !%$1!, ! !& % " "! # # ("% % *& *)% &
2 " C 1 % #" &
( )B Tν