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TRACE and RHESSI observations of the failed eruption of the magnetic flux rope Tomasz Mrozek PowerPoint PPT Presentation


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TRACE and RHESSI observations of the failed eruption of the magnetic flux rope Tomasz Mrozek Astronomical Institute University of Wrocław. CSHKP ( „standard”) model. Hirayama 1974. bipolar configuration is destabilized -> raising filament drags arcade field lines ->

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TRACE and RHESSI observations of the failed eruption of the magnetic flux rope Tomasz Mrozek

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Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

TRACE and RHESSI observations

of thefailederuption of

themagneticfluxrope

Tomasz Mrozek

AstronomicalInstitute

University of Wrocław


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

CSHKP („standard”) model

Hirayama 1974

bipolarconfigurationisdestabilized->

raisingfilamentdragsarcade field lines ->

magneticreconnectionoccursbelow

thefilament ->

thereclosedarcade and theflyingblobare

the products of thisscenario

Shibata et al., 1995


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

„standard” model

Hyder, C. L. 1967

Basic problems:

- thedarkfilamentexistsdue to

sagging of the field lines atthetops

of theconvexarcade - verystrong

assumption

Shibata et al., 1995


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

„standard” model

Hirayama 1974

Basic problems:

- thekinetic energy of theraisingfilamentshould be largerthanthe

energy of theflareitself. Thus, in

this model, theflareisonlythe

repairingprocess of a moreenergetic

break-upcaused by therisingfilament.

Shibata et al., 1995


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

„standard” model

Hirayama 1974

Basic problems:

- observations show (Leroy et al. 1983)thatthedirection of magnetic field perpendicular to thefilamentisopposite to thedirectionexpectedfromthesimpleconnection of thebipolarfiledbelow

Shibata et al., 1995


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

quadrupolar model

50 (!) years ago Sweet suggestedthatflares

mayoccurinthequadrupolarmagneticfiled

configuration.

Thequadrupolar model describesobserved

features of solarflaresin a more natural way.

For somereasonthe theoretical work has ignored this kind of complexity and try to developthetheory of simple, bipolarconfiguration – the „standard” model

Fortunately, thetheory of Sweet hasbeen

ressurectedrecently.

Sweet, P. A. 1958


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

quadrupolar model

In this model theexistence of thedark

filamentisobvious. Moreover, iteasily

explainstheobservedverythinvertical

structure of thefilament

The energy isbuiltupinthe system

beforethedarkfilamenteruption

Thedarkfilamentisacceleratedupward,

and inthelower region recconnected

field lines shrink to form magnetic

arcade

A quotationfromHirose et al. (2001):

In thissimulation (…) theupwardmotion

of thedarkfilament (…) mayeventually

be arrested by theoverlyingclosed field.

Uchida et al. 1999

Hirose et al. 2001


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

theflare

July 14th, 2004

M6.2 GOES class

N14 W61

Observations

RHESSI: entireevent

TRACE: 171 Å (severalseconds

cadence)


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

observatories

TRACE (1998)

30 cm Cassegraintelescopegiving 1 arcsec

spatial resolution

Theobservationsaremadeinthe EUV (transition

region, colonalloops) and UV (chromosphere)

ranges. Moreover, white-lightimagesaremade

RHESSI (2002)

9 large, germaniumdetectors

observationsaremadeintherange

from 3 keV to 17 Mevwith high

energy resolution

spatial resolution isup to 2.5 arc sec


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

theflare

  • Relativelystrongflareisconnectedwith

  • smallmagneticarcade (less than 104km).

  • Severalepisodeswereobserved:

  • - brighteningsbeforetheflare

  • eruptionwhich was startedduringtheimpulsivephase

  • deceleration of theeruption and sideeruptions

  • radialoscillations of the system of loopsobserved high inthecorona


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

preflareactivity

Preflarebrighteningswereobserved

between 5:03 and 5:17 UT.

In the TRACE imageswe observed

brighteningsinsmallsystems of loops

Thereisenoughsignal for reconstructing

RHESSI imageswithdetector 1 giving

thehighestspatial resolution (about 2.5

arc sec)


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

preflareactivity

Contours – RHESSI sources

observedintherange 8-16 keV


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

thebeginnig of theimpulsivephase

Abruptbrighteningconnectedwiththeflareisvisible on

the TRACE imageobtained on 5:17:30 UT

Theeruption of themagneticfluxtubeisobserved

severalsecondsafter

Theeruptionstartedin a very compact region (about

3000 km indiameter!)


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

theeruption

Theheight of theeruptingstructure

was calculatedalongtheyellowline.

On each TRACE imagethedistance

betweenthe front of theeruption

and thereferenceline was calculated


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

evolution of theeruption

Initialphase,

theeruption

moveswith

small, constant

velocity

3

H[km]

2

1

Fast evolution

followingthe

strongest HXR

peakvisible

in 25-50 keV

range

25-50 keV

Deceleration

phase. Main

front changes

itsshape. Side

eruptionsare

observed


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithlow-lyingloops

Thedecelerationvalue (about 600 m/s2) and theshape of theeruption front show that „something”stoppedit. Itispossiblethattwo systems of loopswereinvolvedinbrakingtheeruption.

Brighteningsobservedduringthedeceleration of themain front.


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithlow-lyingloops

Brighteningsinthe region markedwith

the red boxsuggesttheinteraction

betweentheeruption and surrounding

magneticstructures


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithlow-lyingloops

Theshape of theeruptionsuggeststhatthereis a low-lying (but stillabovetheflare) system

of loopsexistingduringtheimpulsivephase. Moreover, therearebrighteningsobservedin

the same locationwherelow-lying system of loopsisanchored. Possiblytheloopswhere

heateddue to interactionwiththeeruption – theyare not „post-flareloops” within

themeaning of the standard model


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithlow-lyingloops

We observedthe 8-16 keVsourcelocatedinthe region of possibleinteractionbetween

theeruption and thelow-lyingloops


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithhigh-lyingloops

Abovetheerupting

structure we observed

the system of high-lying

loops.

Theseloopschanged

theirheight as the

eruptionevolved.


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

interactionwithhigh-lyingloops

Theend of theforemosteruption

(and theend of theforcedrivingthe

movement of thehigh-lyingloops)

Thebeginning of the northern eruption

High-lyingloopsstarted to rise


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

theevolution of thehigh-lyingloops

theend of theforcedrivingthe

movement of thehigh-lyingloops

loopsstarted to move back


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

global oscillations of coronalloops

Tangential, horizontal

No change of radius

About 20 observationsreported by severalauthors

Radial, transversal

Change of radius

One observation (Wang & Solanki 2004)

We observedradialoscillations of coronalloops – veryrareevent. In ourcase we saw „thefinger” thatpulledloops – themagneticstructureejectedfrombelowtheseloops


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

theevolution of thehigh-lyingloops


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

summary

–smallbrighteningsobservedbeforetheflarewithintheflaringstructure 

– brighteningsoutsidetheflaringstructureduringtheinteractionbetweentheeruption

and surroundingloops

– deceleration of theeruptioncaused by theexistence of surrounding system of loops 

– theeruptionstartedin a very compact region, not inthelarge system of loops


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

THANK YOU

FOR

YOUR ATTENTION


Trace and rhessi observations of the failed eruption of the magnetic flux rope tomasz mrozek

summary


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