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Song, P.; Vasyliūnas, V. M.: Effect of horizontally inhomogeneous heating on flow and magnetic field in the chromosphere of the Sun. Astrophys. J. Lett. 796, L23 (2014)
Tu, J.; Song, P.; Vasyliūnas, V. M.: Inductive-dynamic magnetosphere-ionosphere coupling via MHD waves. J. Geophys. Res. Space Phys. 119, pp. 530 - 547 (2014)
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First Light for Sunrise III: the first tests with real sunlight were successful. The balloon-borne solar observatory should be ready for launch at the end of May.
First icy cold, then midnight sun: at the Arctic Circle, the team will prepare the next flight of the balloon-borne solar observatory - and hopes for solar fireworks.
Astronomical teamwork: By combining data from Solar Orbiter and SDO, a group of researchers has unambiguously determined the magnetic field at the solar surface.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.