IRIS-6: The Chromosphere

Session

Session 4

21 Jun 2016, 14:15

FR4 (AlbaNova University Centre)

288. The chromosphere and transition region as seen with CLASP (Invited)

Ryohko Ishikawa (National Astronomical Observatory of Japan)

21/06/2016, 14:15

The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a NASA sounding-rocket experiment, which was launched from White Sands in the US on September 3, 2015, and successfully made the observations during its 5 minutes ballistic flight. The CLASP observations showed that the scattering polarization in the hydrogen Lya line (121.57 nm), which originates in the upper chromosphere...

378. Flux emergence and reconnection in the solar chromosphere

Viggo Hansteen (Institutt for teoretisk astrofysikk, Universitetet i Oslo)

21/06/2016, 14:45

While the flux emergence of photospheric small-scale structures already are well observed and understood, our understanding of the impact of the emerging flux on the energetics and magnetic structure of the above-lying atmosphere is insufficient, as is the fate of the rising magnetic field and how it couples the different regions of the atmosphere. In this talk we will present realistic"...

282. Spectral analysis and modelling of solar flare chromospheric condensation

David Graham (INAF Osservatorio Astrofisico di Arcetri)

21/06/2016, 16:00

We follow up on our recent analysis of the X-Class flare SOL2014-09-10T17:45, where we studied the impulsive phase dynamics of tens of individual flaring kernels", in both coronal (Fe XXI) and chromospheric (MgII) lines observed at high cadence with IRIS. We concentrate here on the chromospheric aspect of the phenomenon, extending the analysis to multiple spectral lines of Mg II, Fe II,...

254. Self-Consistently Modeling the Chromospheric Response to Flare-Accelerated Electrons and Return Currents

Joel Allred (NASA/GSFC)

21/06/2016, 16:20

During solar flares, copious electrons are accelerated to high energies. These travel along magnetic field lines in the Sun's atmosphere, colliding with and heating the ambient plasma. In addition to this direct heating, these particles induce a return current that further heats the atmosphere via resistive dissipation. The return current produces an electric field that balances...

263. IRIS and RHESSI observations of the chromospheric response to energy input during the 29th March 2014 flare

Marina Battaglia (University of Applied Sciences Northwestern Switzerland)

21/06/2016, 16:40

In the common flare scenario beams of accelerated electrons deposit large amounts of energy into the chromosphere, heating it to MK temperatures and causing chromospheric evaporation, i.e. the expansion of the heated plasma into the magnetic loop. What is the importance of energy deposition by electron beams in driving evaporation relative to other types of energy deposition such as by...