Markiewicz, W. J.; Keller, H. U.; Thomas, N.; Titov, D.; Forget, F.: Optical properties of the Martian aerosols in the visible spectral range. Advances in Space Research 29 (2), pp. 175 - 181 (2002)
Kossacki, K. J.; Markiewicz, W. J.; Keller, H. U.: Effect of surface roughness on ice distribution in the south subpolar region of Mars. Planetary and Space Science 49, pp. 437 - 445 (2001)
Skorov, Y. V.; Kömle, N. I.; Keller, H. U.; Kargl, G.; Markiewicz, W. J.: A model of heat and mass transfer in a porous cometary nucleus based on a kinetic treatment of mass flow. Icarus 153 (1), pp. 180 - 196 (2001)
Skorov, Y. V.; Markiewicz, W. J.; Basilevsky, A. T.; Keller, H. U.: Stability of water ice under a porous nonvolatile layer: implications to the south polar layered deposits of Mars. Planetary and Space Science 49 (1), pp. 59 - 63 (2001)
Smith, P. H.; Reynolds, R.; Weinberg, J.; Friedmann, T.; Lemmon, M. T.; Tanner, R.; Reid, R. J.; Marcialis, R. L.; Bos, B. J.; Oquest, C.et al.; Keller, H. U.; Markiewicz, W. J.; Kramm, R.; Gliem, F.; Rueffer, P.: The MVACS surface stereo imager on Mars Polar Lander. Journal Geophysical Research 106, pp. 17589 - 17608 (2001)
Huebner, W. F.; Markiewicz, W. J.: The temperature and bulk flow speed of a gas effusing or evaporating from a surface into a void after reestablishment of collisional equilibrium. Icarus 148 (2), pp. 594 - 596 (2000)
Thomas, N.; Jorda, L.; Markiewicz, W. J.: Effect of diffuse sky brightness on the spectrophotometry of rough Martian surfaces. Journal Geophysical Research 105 (E11), pp. 26739 - 26744 (2000)
Titov, D. V.; Markiewicz, W. J.; Thomas, N.; Keller, H. U.; Tomasko, M. G.; Lemmon, M.; Smith, P. H.: On the optical studies of the atmospheric water vapour from the surface of Mars. Planetary and Space Science 48 (15), pp. 1423 - 1427 (2000)
Basilevsky, A. T.; Markiewicz, W. J.; Thomas, N.; Keller, H. U.: Morphologies of rocks within and near the Rock Garden at the Mars Pathfinder landing site. Journal Geophysical Research 104, pp. 8617 - 8636 (1999)
Basilevsky, A. T.; Markiewicz, W. J.; Thomas, N.; Keller, H. U.: Morphology of the APXS analyzed Rocks at the Pathfinder site. Solar System Research 33, pp. 170 - 186 (1999)
Basilevsky, A. T.; Markiewicz, W. J.; Thomas, N.; Keller, H. U.: Surface material and landscape characteristics at the Mars Polar Lander Site: A consideration and prediction. Solar System Res. 33, p. 439 (1999)
Kossacki, K. J.; Markiewicz, W. J.; Skorov, Y.; Kömle, N. I.: Sublimation coefficient of water ice under simulated cometary-like conditions. Planetary and Space Science 47, pp. 1521 - 1530 (1999)
Markiewicz, W. J.; Sablotny, R. M.; Keller, H. U.; Thomas, N.: Optical properties of the Martian aerosols as derived from Imager for Mars Pathfinder midday sky brightness data. Journal Geophysical Research 104, pp. 9009 - 9017 (1999)
Markiewicz, W. J.; Sablotny, R. M.; Keller, H. U.; Thomas, N.; Titov, D. V.; Smith, P. H.: Optical properties of the Martian aerosols as derived from Imager for Mars Pathfinder midday sky brightness data. Journal Geophysical Research 104, pp. 9009 - 9017 (1999)
Thomas, N.; Markiewicz, W. J.; Sablotny, R. M.; Wuttke, M. W.; Keller, H. U.; Johnson, J. R.; Reid, R. J.; Smith, P. H.: The color of the Martian sky and its influence on the illumination of the Martian surface. Journal Geophysical Research 104, pp. 8795 - 8808 (1999)
Images from ESA’s Solar Orbiter offer the best look yet at a source region of the solar wind - and challenge our view of the continuous particle stream from the Sun.
Deciphering the magnetic origins of the Sun's hot corona: developing a framework for coronal heating by probing the elusive photosphere-corona connection
Using unique observational data and computer simulations, the MPS scientist is striving to understand the incredibly hot temperatures in the solar corona.
For the first time, images of the Sun have been taken from a distance of only 77 million kilometres enabling a completely new view of our star possible.
In his doctoral thesis, Sudip Mandal investigated how special pressure waves help maintain temperatures of several million degrees in the outermost solar atmosphere.