Solar Radiation Physical Modeling (SRPM)
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Transcript of Solar Radiation Physical Modeling (SRPM)
2
Emitted Spectra Radiative Losses
Mean Intensity
and Net Radiative Brackett
Radiative Transfer
Non-LTE
AtmosphericParameters
Continua
Molecular
LinesAtomicLines
Molecular
Continua
Populations & Ionization
Populations & Ionization Balance
Momentum & Energy Balance
Atomic
Atomic Data
Molecular Data
3
Critical Next Steps• Adjust photospheric models and abundances
– Low first-ionization-potential (FIP) contribute to ne and photospheric opacity
– High FIP are needed for upper layers• Re-think lower chromosphere
– Account for radio data showing Tmin<4200 K– Account for UV continua from SOHO-SUMER showing high Tmin– Account for molecular lines (CN, CH, CO) showing low Tmin
• Re-think upper chromosphere with current abundances and observations
• Re-compute transition region with updated abundances, atomic data, diffusion and flows, and energy-balance
• MHD, full-NLTE, 3D simulations of chromospheric variations
• Prominence eruptions-CMEs
4
Low Chromosphere Issues
5380 5381 5382 5383 5384 5385 53860
1 106
2 106
3 106
4 106
SynthesisKitt Peak
Wavelength (A)
Inte
nsity
C I line in between Fe I and Ti II lines - the large line is also Fe I
The CN band head, an Fe I and/or Cr I line is blend with the first CN line
3883 3884 3885 3886 3887 38880
1 106
2 106
3 106
SynthesisKitt Peak
Wavelength (A)
Inte
nsit
y
Fe & C abundanceseem good
But computed CN lines arenot good.Are abundancesincorrect?Or is the modelchromosphereincorrect?
C I line
5
H Ionization and Ly Alpha Line
2.16 108
2.165 108
2.17 108
2.175 108
2.18 108
2.185 108
2.19 108
1 105
1 106
1 107
1 108
1 109
1 1010
1 1011
Local IonizationWith Diffusion (PRD)With Diffusion (CRD)
Height (cm)
Neu
tral
H d
ensi
ty (
cm^-
3)
H Neutal Particle Density
1 104
2 104
3 104
4 104
5 104
6 104
7 104
8 104
9 104
1 105
1 104
1 105
1 106
1 107
1 108
1 109
1 1010
1 1011
Local IonizationWith Diffusion (PRD)With Diffusion (CRD)
Temperature (K)
Neu
tral
H D
ensi
ty (
cm^-
3)
H Neutal Particle Density
1214 1214.5 1215 1215.5 1216 1216.5 1217 1217.5 12180
2 104
4 104
6 104
8 104
1 105
1.2 105
With diffusionLocal ionizat ion
Wavelength (A)
Inte
nsit
y (e
rg/c
m^2
/s/s
r)
Ly Alpha Line
1213 1214 1215 1216 1217 12180
2 104
4 104
6 104
8 104
1 105
1.2 105
UVSP DataWith diffusion
Wavelength (A)
Inte
nsit
y (e
rg/c
m^2
/s/s
r)
Observed and Computed Ly Alpha
6
V1.5 Ly Computed Profiles
•Continuum too high due to Sulphur continuum•Not enough contrast for faculae and plage•Umbra profile has reversal unlike the observed
7
Trace Species Ionization
• For each species and ionization stage
kkekkkekkkkkekkjHkk CnnRnnRCnnVnt
n,11,111,1,u
w
• Or split the abundance and ionization 0w
1
jHH
H ann
at
aV
kkekkkekkkkkek
kHH
kH
k
CnxRnxRCnx
axnan
xant
x
,11,111,1,
kelem u
1
F
kppkaaTH
k
kAkakpH
ap
T
THjkHk
nnkT
VmD
TVn
nn
kT
Vm
kT
gm
kT
eEz
kT
kTn
1
0 lnQ
8
0.8
0.6
0.4
0.2
0.0
Ioniz
ati
onF
racti
on
104
2 3 4 5 6 7 8 9
105
2 3 4 5 6 7 8 9
106
Temperature (K)
Carbon Ionization and Mass FLow......... Static case (w/dif)_____ Upflow case (w/dif)
1.0
0.8
0.6
0.4
0.2
0.0
Ioniz
ati
onF
racti
on
104
2 3 4 5 6 7 8 9
105
2 3 4 5 6 7 8 9
106
Temperature (K)
Carbon Ionization in Static Case......... local ionization_____ including diffusion
9
Chromospheric Magnetic Heating Mechanism
Farley-Buneman Threshold Term
B
U, JHall
E,JPed
Uthr=Cs(1+ψ)