Ning, Z.; Innes, D. E.; Solanki, S. K.: Line profile characteristics of solar explosive event bursts. Astronomy and Astrophysics 419, pp. 1141 - 1148 (2004)
Innes, D. E.; McKenzie, D. E.; Wang, T.: Observations of 1000 km s−1 Doppler shift in 107 K solar flare supra-arcade. Solar Physics 217, pp. 267 - 279 (2003)
Landi, E.; Feldman, U.; Innes, D.; Curdt, W.: Mass motions and plasma properties in the 107 K flare solar corona. Astrophysical Journal 582, pp. 506 - 519 (2003)
Innes, D. E.: Coordinated observations of the quiet Sun transition region using SUMER spectra, TRACE images and MDI magnetograms. Astronomy and Astrophysics 378, pp. 1067 - 1077 (2001)
Torsti, J.; Kocharov, L.; Innes, D. E.; Laivola, J.; Sahla, T.: Injection of energetic protons during solar eruption on 1999 May 9: Effect of flare and coronal mass ejection. Astronomy and Astrophysics 365, pp. 198 - 203 (2001)
Brooks, D. H.; Fischbacher, G. A.; Fludra, A.; Harrison, R. A.; Innes, D. E.; Landi, E.; Landini, M.; Lang, J.; Lanzafame, A. C.; Loch, S. D.et al.; McWhirter, R. W. P.; Summers, H. P.: A study of opacity in SOHO-SUMER and SOHO-CDS spectral observations. I. Opacity deduction at the limb. Astronomy and Astrophysics 357, pp. 697 - 715 (2000)
Brooks, D. H.; Fischbacher, G. A.; Fludra, A.; Harrison, R. A.; Innes, D. E.; Landi, E.; Landini, M.; Lang, J.; Lanzafame, A. C.; Loch, S. D.et al.; McWhirter, R. W. P.; Summers, H. P.; Thompson, W. T.: The quiet Sun extreme ultraviolet spectrum observed in normal incidence by the SOHO coronal diagnostic spectrometer. Astronomy and Astrophysics 347, pp. 277 - 312 (1999)
Harrison, R. A.; Lang, J.; Brooks, D. H.; Innes, D. E.: A study of extreme ultraviolet blinker activity. Astronomy and Astrophysics 351, pp. 1115 - 1132 (1999)
Innes, D. E.; Inhester, B.; Srivastava, N.; Brekke, P.; Harrison, R. A.; Matthews, S. A.; Noëns, J. C.; Schmieder, B.; Thompson, B. J.: Multi-wavelength observations of the onset phase of a coronal mass ejection. Solar Physics 186, pp. 337 - 361 (1999)
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.