FISM 2.0: Improved spectral
range, resolution, and accuracy
Phillip C. Chamberlin
NASA/GSFC
Outline
• FISM Version 1.0
• New in FISM Version 2.0
– Improvements in range, resolution, and accuracy
– New data sets, new flare variably
• FISM 2.0 Results
– Daily model
– Flare model
• Gradual Phase Modeling
• Impulsive Phase Modeling
FISM 1.0
E(t UTC) E min
ESC (t d )
ESR (t d )
E GP (t UTC)
E IP (t UTC)
Emin: Solar minimum reference spectrum, FISMref, (Constant)
Daily Component Variations (Modeled on a daily basis):
- Solar Cycle (SC) - linear with 108-day smoothed daily proxy
- Solar Rotation (SR) - linear with (daily proxy - SC proxy)
Flare Component Variations (Modeled on a 60 seconds basis):
- Gradual Phase (GP) - Power Law with GOES 0.1-0.8 nm
- Impulsive Phase (IP) - Power Law with d/dt GOES (Neupert Effect)
Center-to-Limb variations accounted for by representative proxies in daily component but
must be corrected for in flare components
FISM 1.0
• Released in 2005, the first version of FISM has contributed
to many studies on the influence of solar variations on
Earth, Mars, and the Moon.
– 1 nm bins, 0.1-190 nm
– 5-20% uncertainties for daily model
– 20-75% uncertainties for flare model
FISM Available Through LISIRD
FISM 1.0 Data Sets
• FISM 1.0 ‘daily’ is based on Level 3 data from TIMED
SEE (EGS and XPS) as well as UARS SOLSTICE
• FISM 1.0 ‘flare’ uses TIMED SEE (Level 1 and 3A EGS
and Level 3A XPS) for flare data
Daily Model:
L3 XPS
L3 EGS
UARS SOLSTICE
Flare Model:
L3A XPS
L1/3A EGS
FISM 2.0 Data Sets
• FISM 2.0 ‘daily’ will be based on L4 XPS, L3 data from
SDO/EVE/MEGS, and UARS (and SORCE?) SOLSTICE
• FISM 2.0 ‘flare’ uses L4 XPS, L2 SDO/EVE/MEGS, L1 and L3A
TIMED/SEE/EGS – and possibly UARS/SORCE SOLSTICE?
Daily Model:
*
* L4 XPS (0.1-6 nm), ESP?
L3 SDO/EVE/MEGS (0.1nm)
**
Flare Model:
*
** L3 TIMED/SEE
UARS/SORCE SOLSTICE
?UARS/SORCE SOLSTICE?
L2 SDO/EVE/MEGS (0.1nm)
**
L1/L3 TIMED/SEE/EGS
FISM 2.0 Improvements
• Higher spectral bins at all wavelengths
– 0.1 nm vs 1.0 nm (FISM 2.0 vs 1.0)
• More accurate flare measurements (EUV only)
– 10-15% vs 20-40%
• Number of flare measurements (EUV ONLY)
– 389 vs 39
• Not only the number of flares observed, but at
every 10 seconds throughout the flare
• More available as SDO continues to observe
• Range of flare magnitudes measured
– C5 to X6.9 vs M1 to X28+
FISM 2.0 New Questions
• How to implement delay in flare response due to cooling?
• How to implement coronal dimming?
• How to model flare variations in FUV long-ward of EVE
– Use FISM 1.0? New SOLSTICE Model?
SDO EVE measurements
showing EUV emissions
of various temperatures
peak at different times
during solar flares.
FISM 2.0 Daily Results (test)
• FISM daily results based on SDO EVE show promising
first results.
Near Solar Maximum
Red: FISM
Solar Minimum
Black: SDO/EVE
FISM 2.0 Daily Results (test)
• FISM daily results based on SDO EVE show promising
first results.
Red: FISM
Black: SDO/EVE
FISM 2.0 Daily Results
• MEGS-B range is not coming out correctly
– Need to make sure EVE L3 data is correct (as is the
case for 30.34 nm data)
• Improve proxy tree?
– Now based on best statistics determine best proxy
• Multiple proxies and weighted fits for each bin?
• Add in XPS and SOLSTICE
– Algorithms only completed so far for SDO/EVE
– UARS SOLSTICE already part of FISM V1.0, just
need to merge
• Lots of validation still needed
FISM 2.0 Flare Results
• Initial results show some good results
• May still have some large uncertainties due to trying
to generalize/model a wide variety of flares
• First run still just uses the Impulsive Phase (IP) and
Gradual Phase (GP) Peak values, not the entire flare
• Now able to model center-to-limb variation (CLV) for
IP as well as GP (didn’t have enough IP observations
prior to EVE).
• Initial results for a generalize flare timing delay look
ok, but hopefully a better way.
FISM 2.0 Flare GP Fits
• Good fits to those wavelengths that have large
variations
17.11 nm
Fe IX
11.44 nm
Fe XXII
FISM 2.0 GP Peak Delay Time
• Median peak delay time for each wavelength shows
some potentially useful results, but need validation
and hopefully another method/proxy
FISM 2.0 Flare IP Fits
• Good fits to those wavelengths that have large
variations – and valid center-to-limb darkening
30.38
He II
FISM 2.0 Flare Results
BLACK: SDO/EVE
Light Blue: FISM Daily
Green: FISM IP
Dark Blue: FISM GP
RED: FISM All
(Daily+IP+GP)
Conclusions (1)
• Initial modeling of SDO/EVE is going well, but still a
lot of work and validation activities remain.
– Find another proxy (XRS A/B temperature) for
peak delay – student working on this now.
– Coronal dimming?
• Will then add on soft X-rays from XPS Level 4 and
SOLSTICE from 116 nm – ???
– Extend wavelength range to cover FUV hole that
will exist after SORCE, at least for daily model
(maybe just use another daily model then?)
• Compare V1.0 to V2.0, to other models, as well as to
the various basis data sets, and to I/T modelers.
• Integrate V2.0 to LISIRD for distribution
Conclusions (2)
• Lots of new, planned science using FISM:
– One example will be in poster session from Huang et al.
– MAVEN LPW/EUV
– Moore et al. paper, in preparation, follow on the Woods et
al., 2005 paper on TIM measurements of flares
• Use FISM to model the IP and GP radiated flare
emission in TSI
– Emslie et al. paper, submitted, SEE energetics comparison
of 38 events