Andreas Lagg MPI for Solar System Research Katlenburg-Lindau, Germany [email protected]
37
Chromospheric magnetic fields with the EST: A new era for He 10830 Andreas Lagg MPI for Solar System Research Katlenburg-Lindau, Germany [email protected]
Andreas Lagg MPI for Solar System Research Katlenburg-Lindau, Germany [email protected]
Andreas Lagg MPI for Solar System Research Katlenburg-Lindau,
Germany [email protected]
Slide 2
EST France 2010 Workshop, May 19-21 2010 Why He 10830? purely
chromospheric B-range 1 G to several kG ideal for coupling science
height diagnostic tool! off-limb AND on-disk easy to interpret
2
Slide 3
EST France 2010 Workshop, May 19-21 2010 Why with EST? photon
efficiency high photon flux spatial & temp. resolution high
polarimetric accuracy (polarization-free telescope) image stability
(MCAO) 3
Slide 4
EST France 2010 Workshop, May 19-21 2010 Centeno et al., 2008
Advantage: NO photospheric contribution! Disadvantage: Coronal
illumination required 4
Slide 5
EST France 2010 Workshop, May 19-21 2010 Centeno et al., 2008
5
Slide 6
EST France 2010 Workshop, May 19-21 2010 Avrett et al. (1994)
6
Slide 7
EST France 2010 Workshop, May 19-21 2010 important parameters
for He formation: 1. density and extent of chromosphere 2. coronal
illumination Avrett et al. (1994) He density 3 S 1 7 plage bright
network cell center average
Slide 8
EST France 2010 Workshop, May 19-21 2010 important parameters
for He formation: 1. density and extent of chromosphere 2. coronal
illumination Avrett et al. (1994) 8 He density 3 S 1 Wavelength []
Stokes I
Slide 9
EST France 2010 Workshop, May 19-21 2010 None. No complex
non-LTE modelling of the solar atmosphere required. Simple
interpretation analysis of complex solar conditions possible 9
Slide 10
EST France 2010 Workshop, May 19-21 2010 Advanced inversion
codes available: HAZEL (Asensio Ramos et al. 2008) (HAnle and
ZEeman Light) HeLIX + (Lagg et al., 2009) (Helium Line Information
Extractor), based on similar synthesis module 10
Slide 11
EST France 2010 Workshop, May 19-21 2010 Animation next slide:
INC=80 to solar vertical formation height: 2000 km broadening: 8
km/s optical thickness: model C 0
EST France 2010 Workshop, May 19-21 2010 Active regions (plage,
pores sunspots): reliable measurements for B > 100 G are easy.
Extremely high spatial and/or temporal resolution coupling science:
photosphere / chromosphere Quiet regions: 10 100 G: saturated Hanle
regime: LP determined by direction of B