IRIS-6: The Chromosphere

Session

Session 8

23 Jun 2016, 14:15

FR4 (AlbaNova University Centre)

340. MHD waves in the solar chromosphere (Invited)

Gary Verth (Sheffield University)

23/06/2016, 14:15

Within the last decade, due to significant improvements in the spatial and temporal resolution of chromospheric data, MHD wave studies in this fascinating region of the Sun's atmosphere have risen to the forefront of solar physics research. In this talk we review the most interesting MHD wave-related discoveries by space and ground-based instruments such as Hinode, IRIS, CRISP/SST and...

290. Chromospheric heating due to transverse waves in small magnetic elements

Shahin Jafarzadeh (Institute of Theoretical Astrophysics, University of Oslo)

23/06/2016, 14:45

We characterise magnetohydrodynamics (MHD) waves in small magnetic elements and investigate their propagation in the solar atmosphere by exploiting coordinated observations with the Swedish 1 m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS). We use wavelet transform to analyse (horizontal) displacement oscillations in magnetic bright points in several passbands...

334. Generation of upward Alfvénic waves by the chromospheric shock waves

Munehito Shoda (The University of Tokyo)

23/06/2016, 16:00

Classically, the solar chromosphere was thought to be a dissipative medium for Alfvén waves, in that those generated by the convective motions were thought to dissipate most of their energy there. However, recent high-resolution observations near the coronal base strongly suggest that the upward Alfvén waves are generated or amplified in the chromosphere by the large amplitude acoustic...

258. Simulations of Alfven wave driving of the solar chromosphere - efficient heating and spicule launching.

Tony Arber (University of Warwick)

23/06/2016, 16:20

By driving Alfven and kink waves into an expanding flux tube we demonstrated that with a Poynting flux on 2x10^7 erg/s/cm^2 we can reproduce a heating profile broadly consistent with the mid to upper chromosphere. The heating mechanism is through ponderomotive coupling of Alfven waves to shock and it is the shocks which dissipate and heat. These same shocks also produce jets similar to...

332. Wave heating of the partially-ionised atmosphere

Sergiy Shelyag (Northumbria University)

23/06/2016, 16:40

The most energetic part of the Sun, interior, due to its plasma parameters is hidden below the solar surface and invisible to the observer. Nevertheless, the solar interior generates the energy and provokes atmospheric magnetic activity. Despite great progress in both observational and simulation methods, the mechanism of energy transport from the solar convection zone into the...