solar radiation physical modeling (srpm)
DESCRIPTION
Solar Radiation Physical Modeling (SRPM). J. Fontenla June 30, 2005b. Mean Intensity. Emitted Spectra. Radiative Losses. and Net Radiative. Brackett. Atomic. Molecular. Continua. Continua. Atomic Data. Radiative Transfer. Molecular Data. Non-LTE. Molecular. Atomic. - PowerPoint PPT PresentationTRANSCRIPT
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)