Schühle, U.; Curdt, W.; Wilhelm, K.; Solanki, S. K.; Stucki, K.: Signatures of coronal hole spectra between 660 and 1460 Å measured with SUMER on SOHO. Space Science Reviews 87, pp. 299 - 302 (1999)
Sheminova, V. A.; Solanki, S. K.: Is the FIP effect present inside solar photospheric magnetic flux tubes? Astronomy and Astrophysics 351, pp. 701 - 706 (1999)
Stucki, K.; Solanki, S. K.; Rüedi, I.; Stenflo, J. O.; Brkovic, A.; Schühle, U.; Wilhelm, K.; Huber, M. C. E.: Coronal Holes Properties Observed with SUMER. Space Science Reviews 87, pp. 315 - 318 (1999)
Stucki, K.; Solanki, S. K.; Rüedi, I.; Stenflo, J. O.; Brkovic, A.; Schühle, U.; Wilhelm, K.; Huber, M. C. E.: Coronal holes versus normal quiet Sun observed with SUMER. Astrophysics and Space Science 264, pp. 53 - 61 (1999)
Balogh, A.; Cliver, E.; Petrie, G.; Solanki, S. K.; Thompson, M.; von Steiger, R. (Eds.): Solar Magnetic Fields: from measurement towards understanding. Springer, Dordrecht (2018), 426 pp.
Thompson, M. J.; Balogh, A.; Culhane, J. L.; Nordlund, Å.; Solanki, S. K.; Zahn, J.-P. (Eds.): The Origin and Dynamics of Solar Magnetism. Springer, Berlin (2009), 428 pp.
Kneer, F.; Solanki, S. K.; Strassmeier, K. G.; von der Lühe, O.; Arbeitsgemeinschaft Forschung, E. (Eds.): Perspektiven der Erforschung von Sonne und Heliosphäre in Deutschland. Copernicus GmbH, Katlenburg-Lindau (2003), 46 pp.
Shapiro, A.; Peter, H.; Solanki, S. K.: The Sun's Atmosphere. In: The Sun as a Guide to Stellar Physics, pp. 59 - 85 (Eds. Engvold, O.; Vial, .-C.; Skumanich, A.). Elsevier, Amsterdam (2019)
Loukitcheva, M.; Solanki, S.; White, S.; Carlsson, M.: Probing the Sun with ALMA: observations and simulations. In: Revolution in Astronomy with ALMA: The Third Year, Vol. 499, pp. 349 - 350. Astronomical Soc Pacific, San Francisco (2015)
Krivova, N. A.; Solanki, S. K.: Models of Solar Total and Spectral Irradiance Variability of Relevance for Climate Studies. In: Climate and Weather of the Sun-Earth System (CAWSES), pp. 19 - 38 (Ed. Lübken, F.-J.). Springer, Dordrecht (2013)
Solanki, S. K.; Marsch, E.: Solar Space Missions: present and future. In: Formation and Evolution of Cosmic Structures: Reviews in Modern Astronomy, Volume 21, pp. 229 - 248 (Ed. Röser, S.). Wiley-VCH, Weinheim (2009)
Solanki, S. K.: The magnetic field from the solar interior to the heliosphere. In: The Sun and the Heliosphere as an Integrated System, pp. 373 - 395 (Eds. Poletto, G.; Suess, S. T.). Kluwer, Dordrecht (2004)
Pauluhn, A.; Lang, J.; Schühle, U.; Solanki, S. K.; Wilhelm, K.; Thompson, W. T.; Pike, C. D.; Rüedi, I.; Hollandt, J.; Huber, M. C. E.: Intercalibration of CDS and SUMER. In: The Radiometric Calibration of SOHO, (SR-002), pp. 235 - 247 (Eds. Pauluhn, A.; Huber, M. C. E.; von Steiger, R.). ESA Publ. Div., Noordwijk (2002)
Solanki, S. K.; Schüssler, M.; Schwenn, R.; Wilhelm, K.; Fligge, M.: Das Magnetfeld der Sonne: Quelle des Weltraumwetters und möglicher Klimafaktor. In: Jahrbuch der Max-Planck-Gesellschaft 2001, pp. 399 - 405. Verlag Vandenhoeck & Ruprecht, Göttingen (2002)
Solanki, S. K.: Solar photospheric magnetic flux tubes: Observations. In: Encyclopedia of Astronomy and Astrophysics, pp. 2675 - 2682 (Ed. Murdin, P.). Institute of Physics Publishing, London (2001)
Solanki, S. K.: Sunspot magnetic fields. In: Encyclopedia of Astronomy and Astrophysics, pp. 3177 - 3180 (Ed. Murdin, P.). Institute of Physics Publishing, London (2001)
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.