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Flows in hot coronal loops : mass cycle and coupling from chromosphere to corona. Pia Zacharias, Sven Bingert , Hardi Peter Solar Cycle 24 Napa , California December 11, 2008. 10.  10 5 K.  6.5 10 5 K . 5. 0. Peter (1999) ApJ 516, 490 .

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flows in hot coronal loops mass cycle and coupling from chromosphere to corona

Flows in hot coronalloops:masscycle and couplingfromchromosphere to corona

Pia Zacharias, Sven Bingert, Hardi Peter

Solar Cycle 24

Napa, California

December 11, 2008

doppler shifts in the solar transition region and in the corona

10

 105 K

 6.5105 K

5

0

Peter (1999) ApJ 516, 490

Dopplershift [ km/s ]

5

10

SUMER

Doppler shifts in the solar transitionregionand in thecorona
3d simulation doppler shifts
3D simulation – Doppler shifts

Observation

Simulation

Probably OK for TR (some 105 K)

Not yet good forcoronallines

from observation to simulation
Fromobservation to simulation
  • Input magneticfield - quietSun-like
  • 3D MHD model of coronal box (50x50x30Mm3=2563) (Bingert at al.)
  • includingradiativeloss, heatconduction and Ohmicheatingdue to fluxbraiding
  • Spectralsynthesis (CHIANTI)  Resultingloopstructures

Initial verticalmagneticfield at bottomboundary

Evolving TR loops (snapshop)

doppler velocities in the simulation
Doppler velocities in thesimulation

CIV (1548 Å) Doppler map

Distribution of Doppler velocities

(smaller FWHM thanobserved; 3x)

<vD>=1.52 km/s

meanredshift

blueshiftredshift

global mass balance constant coronal mass
Global massbalance: constantcoronalmass
  • Coronalmassfluctuates ≈ 0.1%
  • Emptycoronaoversimulation time (30 min) wouldneedaverageflow of ≈ max 0.1 km/s
  • Global sinking of atmospheredue to masslossisNOTresponsiblefornetlineshift

N: Number of particles

in the box with T>104.1 K

<N>: meannumber of particles in the box with T>104.1 K

investigation of individual loops hot loops
Investigation of individualloops: hotloops
  • 1st step: restrain to L > 30 Mm andTmax > 105 K
  • Assignthesamefieldlines at eachtimestep

followfieldlinesthroughthe 30 minute time series

snapshot

nature of the flows in hot and long loops
Nature of theflows in hot and longloops

log(T[K])>105 & L>30 Mm

Contradiction:

Whyisthecoronalmassconstantwhiledownflowsdominate ?

Solution ?

Coronalmasssupply

throughtheheating of cool loops?

27 %

62 %

10 %

Siphon flows:

Flowthroughtheloop

Draining / downflows

Flow out of theloop

Strange flowprofiles

heating loops with upflows
Heatingloopswithupflows?

heating

Problem:

Even loopsthatareheated up

aredraining...

Whereareloopswhichfill

due to increasingheatinput ?

Probablyselectioneffect (T>105K) ?

downflow

 NO hot loopswithupflowsfound!

outlook
Outlook
  • Properlyfollowfieldlines in time
  • Whatabouttheupflowswesee in the Doppler maps?
  • Investigate “cool“ loops (T<105 K) withsamelengths