Dimming analysis 13/05/05 Gemma Attrill

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Presentation transcript:

Dimming analysis 13/05/05 Gemma Attrill Mullard Space Science Laboratory This is not another 12/05/97. 13/05/05 is more complex because it follows solar maximum: residue magnetic fields. 12/05/97 13/05/05

Dimming regions of 13/05/05

Selecting regions for analysis Attrill et al., (2006)

Intensity evolution (35 hr) selected regions 1 2 3 4 5 6 7 8 Away from core 1 Away from core 2 Intensity Time Data gap: 17:37 - 22:58 UT 1 2 3 4 5 6 7 8 Quiet Sun Coronal Hole

Magnetic flux dimmings (20 G filter) 1 2 3 4 5 6 7 8 If dimmings 1 and 2 mark flux rope footpoints, then minimum magnetic flux of the flux rope: ((Absolute 1 + Absolute 2) / 2) = 3.98E+21 Mx c.f. Yurchyshyn et al., (2006) use an Erupting Flux Rope model and Hu et al., (2006) use the Grad-Shafranov model: Axial (torroidal) flux in ICME = 2.9E+21 Mx, 2.1E+21 Mx Azimuthal (poloidal) flux in ICME = 4.4E+22 Mx, 4.2E+21 Mx Our magnetic flux measurement (which is a minimum), is too large to be explained just by the axial (torroidal) magnetic flux. So the azimuthal (poloidal) magnetic flux is also required.

How do the dimmings form? 7 3 4 1 2 3 4 5 6 7 8 From SolarSoft Latest events archive. PFSS Derosa & Schrijver 1 2 Analysis of the evolution of the dimmings can give a lot of information (both quantitative & qualitative) regarding the changing magnetic topology of the CME event.