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Magnetic Dissipation in the Photosphere and Heating of the Corona. Valentyna Abramenko Big Bear Solar Observatory and Alexei Pevtsov National Solar Observatory. Soft X-ray luminosity of the corona. Objects: Active regions near the center of the solar disk.

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magnetic dissipation in the photosphere and heating of the corona

Magnetic Dissipation in the Photosphere and Heating of the Corona

Valentyna Abramenko

Big Bear Solar Observatory

and

Alexei Pevtsov

National Solar Observatory

slide3

Objects: Active regions

near the center

of the solar disk

Objects: Active regions

near the center

of the solar disk

?

CORONA

PHOTOSPHERE

Data: Yohkoh/SXT Data:

Al 0.1 μm channel

AlMgMn-sandwich channel

Data: SOHO/MDI high resolution

magnetograms

  • Analyzed Quantities:
  • Averaged (over an area) flux
  • in each channel
  • Temperature
  • Emission Measure
  • Analyzed Quantitiy:
  • Averaged (over an area) magnetic
  • energy dissipation rate
structure of magnetic energy dissipation
Structure of Magnetic Energy Dissipation

Magnetic energy dissipation, ε/η

Line-of-sight Magnetic Field, Bz

energy flux estimation

η = (150 ÷ 300) km2/s

If we accept the effective thickness of the photosphere h = 500 km,

the energy flux F=∫ εَ dh for different ARs varies in the range of

F = (1 ÷ 14)×106 erg cm-2 s-1

Energy Flux Estimation

Abramenko, Pevtsov,

Romano,2006, ApJL 646

poynting flux vs x ray flux area averaged values

Bz Bz Vh

Poynting Flux vs X-ray Flux:area-averaged values

Follow-up study: Tan, Jing, Abramenko, Pevtsov, Song, Park, Haimin Wang,

2007 ApJ, accepted

Poynting Flux ~ Bh Bz Vh

poynting flux vs x ray flux area integrated values
Poynting Flux vs X-ray Flux:area-integrated values

Follow-up study: Tan, Jing, Abramenko, Pevtsov, Song, Park, Haimin Wang,

2007 ApJ, accepted

conclusions
Conclusions
  • Energy input due to the random motions strongly correlates with brightness, temperature and emission measure of the corona.
  • Energy flux is (1 ÷ 14)×106 erg cm-2 s-1, which is quite sufficient to heat the corona above ARs.
  • Magnetic diffusivity in ARs is (150 ÷ 300) km2/s, which is twice lower than in QS areas.