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Modeling Long-Lived “Super-Hydrostatic” Active Region Loops PowerPoint PPT Presentation


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

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Modeling long lived super hydrostatic active region loops

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!

  • 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


Modeling long lived super hydrostatic active region loops

Cargill et al., 1995, ApJ, 439, 1034

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 cool faster than they drain

Loops cool faster than they drain


Simulated trace light curves

Delay between the appearance of the loop in 195 and 171

Simulated TRACE light curves


4 jul 1998 aschwanden loop 23

4-Jul-1998 (Aschwanden Loop #23)

Winebarger et al., ApJ, submitted


18 aug 1998 aschwanden loop 2

18-Aug-1998 (Aschwanden Loop #2)


Simulated loop cools too fast

Simulated loop cools too fast!

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


Filaments lead to flat filter ratios

Filaments lead to flat filter ratios


Sxt trace loops

SXT→TRACE Loops


Sxt trace loops1

SXT→TRACE Loops


Light curves of loop cooling from sxt to trace

Light curves of loop cooling from SXT to TRACE


Single cooling loop produces too much intensity in trace

Single cooling loop produces too much intensity in TRACE


Sxt trace intensity ratios are consistent with filamentation

SXT/TRACE intensity ratios are consistent with filamentation


Conclusions implications for solar b

Conclusions/Implications for Solar-B

  • 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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