Forward Modeling from Simulations: Full -Sun and Active Regions
description
Transcript of Forward Modeling from Simulations: Full -Sun and Active Regions
![Page 1: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/1.jpg)
Forward Modeling from Simulations: Full-Sun and Active Regions
Cooper Downs
ISSI Workshop on Coronal Magnetism (2nd Meeting), March 10 2014
![Page 2: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/2.jpg)
Outline
- I’m hoping that we (PSI) can provide models/ideas that can support you with your coronal magnetometry interests.
- I’ll talk briefly about the general types of MHD modeling that we do.
- Show a couple of example models that we could use with FORWARD.
![Page 3: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/3.jpg)
Why Forward Model Simulations?- Magnetic and thermal states of the corona are closely related.
- Oftentimes the thermal structure strongly influences observables. (i.e. coronal line-emission / scattering).
- We’d really like to be able to test our physical assumptions and interpretations of observations.
- Even better we’d love to infer or ‘invert’ physical conditions from the measurements themselves.
3D Thermodynamic MHD simulations can help with these tasks by:
- Forward modeling observables from simulation data.
- Testing inversion methods using forward modeled data. - Q? Do we get the same answer back?
![Page 4: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/4.jpg)
Modeling Overview
![Page 5: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/5.jpg)
(see Lionello et al. 2009 for more details)
![Page 6: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/6.jpg)
Corona is not Ideal!- Non-ideal terms dictate thermodynamic state in the low corona.
- For the Transition region we add:- Electron heat conduction (due to high T, steep gradients).- Radiative losses.- Empirical term to encompass coronal heating: e.g. Unresolved Waves / Reconnection / resistive dissipation.
- Turbulence based heating model is next.
See Lionello 2009, and Downs 2010 for case-studies.
Thermodynamic Energy EQ
![Page 7: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/7.jpg)
Global Coronal ModelingFull-sun 3D Thermodynamic MHD simulations:- Driven by static or time-dependent magnetogram observations:
![Page 8: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/8.jpg)
Global Coronal ModelingFull-sun 3D Thermodynamic MHD simulations:- Coronal Comparisons to EUV observables.
![Page 9: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/9.jpg)
Active Region ModelingLocalized Hi-Res MHD.- Freeze 3D NLFF solution- Solve for parallel plasma dynamics in time (to study coronal heating).
Mok et al. 2008
![Page 10: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/10.jpg)
CME/Flux-Rope ModelingTime-dependent Eruption Modeling- Insert or construct energized magnetic configuration.- Slowly drive the system towards eruption.
![Page 11: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/11.jpg)
CME/Flux-Rope ModelingTime-Dependent Eruption Modeling- Thermal-Magnetic evolution can be connected to observables!- e.g. coronal dimmings:
![Page 12: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/12.jpg)
FORWARD Examples
![Page 13: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/13.jpg)
Coronal Simulations from the Web• Our website: http://www.predsci.com/hmi
Thermodynamic runs from CR2096 to present are freely available for download
2 heating models to choose from (Density stratification and amount of opened up field differ slightly)
I can provide the IDL routine to read and interpolate the simulation to a standard datacube.
Even better, its compatible with FORWARD!
![Page 14: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/14.jpg)
High Res Global CasesIf you don’t like our website, we also have high res-runs for a few cases.
- e.g. the July 2010 Eclipse, or the 2011 Comet Lovejoy perihelion.
- We can run new ones as well!
Fe XIII 1075 nm Stokes I
(Intensity)
Fe XIII 1075 nm Stokes L/I
(total linear over intensity)
AIA 193Å
![Page 15: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/15.jpg)
MHD Field + MHD Plasma MHD Field + Symmetric Plasma
Test 1: Spherical Symmetry I
![Page 16: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/16.jpg)
MHD Field + MHD Plasma MHD Field + Symmetric Plasma
Test 1: Spherical Symmetry L/I
![Page 17: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/17.jpg)
POS MHD Field + MHD PlasmaLOS integrated MHD Field + MHD Plasma
Test 2: Plane of Sky Vs. Full Integration
![Page 18: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/18.jpg)
PFSS + Symmetric PlasmaLOS integrated MHD Field + MHD Plasma
Test 3: MHD vs. PFSS
![Page 19: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/19.jpg)
Active Region ModelYung Mok and collaborators at PSI have studied AR 7986 (August 1996) extensively (Mok et al. ‘05, ‘08, ‘14 in prep).
- Current method is to freeze a NLFF state, and solve for the parallel plasma dynamics in time.
- This gives time-dependent snapshots of loop heating and cooling cycles.
- The time-dependent plasma state seems to agree well with observations.
- (paper in-prep) but more importantly for us, it provides a high-res, strong field AR with a self-consistent temperature and density background.
![Page 20: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/20.jpg)
Active Region Model Magnetic Configuration
![Page 21: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/21.jpg)
Active Region Model AIA Synthesis (Disk View)
![Page 22: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/22.jpg)
Active Region Model AIA Synthesis (Limb View)
![Page 23: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/23.jpg)
Active Region Model Example Fe XIII 1075 nmfrom FORWARD
L/I V/I
I L
![Page 24: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/24.jpg)
• The Solar Atmosphere is inherently complex and 3D.– LOS effects need to at least be considered, particularly when studying
specific events or complex geometric structures with density contrasts.
• Models and Observations can go hand in hand!– We can use them to interpret/understand the complexity / limitations of data.– We can use them to test inversion methods.
• Polarization measurements are rich in information content, and we have a range of simulations/tools at our disposal.
Closing Words
![Page 25: Forward Modeling from Simulations: Full -Sun and Active Regions](https://reader035.fdocuments.us/reader035/viewer/2022062521/5681668f550346895dda64d1/html5/thumbnails/25.jpg)
End