Penumbral models in the light of Hinode spectropolarimetric observations

1
Penumbral models in the light of Hinode
spectropolarimetric observations
Jan Jurcák L.R. Bellot Rubio HINODE team
National Astronomical Observatory of
Japan Instituto de Astrofísica de Andalucía from
everywhere
Hinode Science Meeting, Dublin, 22. Aug 2007
2
The spectropolarimeter onboard HINODE gives us
for the first time the oportunity to distinguish
the fine structure of the penumbra. The plasma
properties of individual filaments can be thus
studied using advanced inversion techniques.
This should allow us to compare the
stratifications of plasma parameters predicted
from the suggested models of penumbral fine
structure with those obtained by the inversion
technique.
Introduction
Hinode Science Meeting, Dublin, 22. Aug 2007
3
Analysed data sets
Hinode Science Meeting, Dublin, 22. Aug 2007
4
Field-free gaps
Flux tubes
Schlichenmaier R. 1998,
AA, 337, 897
vs.
Spruit Scharmer 2006, AA, 447, 343
Hinode Science Meeting, Dublin, 22. Aug 2007
5
SIR/GAUSS
Hinode Science Meeting, Dublin, 22. Aug 2007
6
Temperature 2.5 to 6.5 kK Field strength 0.5
to 3.5 kGVelocity -2 to 10 km s-1 Inclination
(LRF) 20 to 140 deg
Resulting maps of plasma parameters
Hinode Science Meeting, Dublin, 22. Aug 2007
7
The inner penumbra
Hinode Science Meeting, Dublin, 22. Aug 2007
8
13.12. 2006heliocentric angle 0.84correlation
in the inner penumbra
The inner/outer penumbra
Hinode Science Meeting, Dublin, 22. Aug 2007
9
13.12. 2006heliocentric angle 0.84correlation
in the outer penumbra
The inner/outer penumbra
Hinode Science Meeting, Dublin, 22. Aug 2007
10
In the inner penumbra, all inversions lead to
similar models of atmosphere. We found weaker and
more horizontal magnetic field and increased
line-of-sight velocities in bright filaments deep
in the photosphere.
Conclusions

• Such behaviour is in agreement with both
  suggested penumbral models in this part of the
  penumbra.

• In the outer penumbra, inversions with different
  height of the gaussian perturbation lead to
  similar quality of the fits.

• The obtained correlation coefficients can be
  hardly explained using the field-free gap model
  of the penumbra, as the weak and more horizontal
  magnetic field together with the maxima of the
  line-of-sight velocity should be always related
  to the bright filaments.

Hinode Science Meeting, Dublin, 22. Aug 2007
11
15.12. 2006heliocentric angle 0.47correlation
in the inner penumbra
The inner/outer penumbra
Hinode Science Meeting, Dublin, 22. Aug 2007
12
15.12. 2006heliocentric angle 0.47correlation
in the outer penumbra
The inner/outer penumbra
Hinode Science Meeting, Dublin, 22. Aug 2007