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Heating Function? E H (s,t). Modeling Long-Lived “Super-Hydrostatic” Active Region Loops. Harry Warren Amy Winebarger John Mariska Naval Research Laboratory Washington, DC Solar-B Science Meeting Japan February 3-5, 2003.

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Heating Function? EH(s,t)

Modeling Long-Lived “Super-Hydrostatic” Active Region Loops

Harry Warren

Amy Winebarger

John Mariska

Naval Research Laboratory

Washington, DC

Solar-B Science Meeting

Japan

February 3-5, 2003


Motivation understanding the properties of active region loops observed with trace
Motivation: Understanding the properties of active region loops observed with TRACE

Aschwanden et al., 2001, ApJ, v550, p1036


Static models don t work
Static Models Don’t Work! loops observed with TRACE

  • RTVS (uniform heating) scaling law predicts very low densities for long loops.

    • TRACE observations show nobs/nuni ~ 100!

  • RTVS (foot point heating) scaling law gives densities that are higher, but only by a factor of about ~3.

    • Highly localized footpoint heating → instability.

Winebarger et al., ApJ, in press


Cargill et al., 1995, ApJ, 439, 1034 loops observed with TRACE

Rosner et al., 1978, ApJ, 220, 643

Dynamic solutions can be much denser than static solutions

Warren et al., 2002, ApJL, v570, p41


Cooling loops can be overdense near 1 mk
Cooling loops can be overdense near 1 MK loops observed with TRACE


Loops cool faster than they drain
Loops cool faster than they drain loops observed with TRACE


Simulated trace light curves

Delay between the appearance of the loop in 195 and 171 loops observed with TRACE

Simulated TRACE light curves


4 jul 1998 aschwanden loop 23
4-Jul-1998 (Aschwanden Loop #23) loops observed with TRACE

Winebarger et al., ApJ, submitted


18 aug 1998 aschwanden loop 2
18-Aug-1998 (Aschwanden Loop #2) loops observed with TRACE


Simulated loop cools too fast
Simulated loop cools too fast! loops observed with TRACE

EF = 2 ergs cm-3 s-1, δ = 680 s


Not one loop many filaments consistent with the light curve
Not one loop, many filaments? – Consistent with the light curve

10 filaments, EF ≈ 0.2-2 ergs cm-3 s-1, δ = 680 s



Sxt trace loops
SXT curve→TRACE Loops


Sxt trace loops1
SXT curve→TRACE Loops





Conclusions implications for solar b
Conclusions/Implications for Solar-B curve

  • Dynamics and filamentation are important in determining what is observed

  • EIS+XRT+SOT will provide an unprecedented opportunity to study the dynamical evolution of active region loops

  • More modeling is needed to identify signatures of coronal heating


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