Gizon, L.; Schunker, H.; Baldner, C. S.; Basu, S.; Birch, A. C.; Bogart, R. S.; Braun, D. C.; Cameron, R.; Duvall Jr., T. L.; Hanasoge, S. M.et al.; Jackiewicz, J.; Roth, M.; Stahn, T.; Thompson, M. J.; Zharkov, S.: Helioseismology of sunspots: a case study of NOAA region 9787. Space Science Reviews 144, pp. 249 - 273 (2009)
Nutto, C.; Roth, M.; Zhugzhda, Y.; Bruls, J.; von der Lühe, O.: Calculation of spectral darkening and visibility functions for solar oscillations. Solar Physics 251, pp. 179 - 188 (2008)
Schad, A.; Roth, M.; Schelter, B.; von der Lühe, O.; Timmer, J.: Cross-spectral analysis of solar oscillation time series. J. Phys.: Conf. Ser. 118, 012091 (2008)
Zaatri, A.; Corbard, T.; Roth, M.; González Hernández, I.; von der Lühe, O.: Comparison of geometrical mapping for ring diagram analysis. J. Phys.: Conf. Ser. 118, 012090 (2008)
Krieger, L.; Roth, M.; von der Lühe, O.: Estimating the solar meridional circulation by normal mode decomposition. Astron. Nachrichten 328, pp. 252 - 256 (2007)
Hanasoge, S. M.; Larsen, R. M.; Duvall Jr., T. L.; DeRosa, M. L.; Hurlburt, N. E.; Schou, J.; Roth, M.; Christensen-Dalsgaard, J.; Lele, S. K.: Computational acoustics in spherical geometry: Steps toward validating helioseismology. Astrophysical Journal 648, pp. 1268 - 1275 (2006)
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.