Tiwari, S. K.; van Noort, M.; Solanki, S. K.; Lagg, A.: Depth-dependent global properties of a sunspot observed by Hinode using the Solar Optical Telescope/Spectropolarimeter. Astronomy and Astrophysics 583, A119 (2015)
Thalmann, J. K.; Tiwari, S. K.; Wiegelmann, T.: Force-free Field Modeling of Twist and Braiding-induced Magnetic Energy in an Active-region Corona. Astrophysical Journal 780 (1), 102 (2014)
Thalmann, J. K.; Tiwari, S. K.; Wiegelmann, T.: Comparison of force-free coronal magnetic field modeling using vector fields from Hinode and Solar Dynamics Observatory. Astrophysical Journal 769, pp. 59 - 68 (2013)
Tiwari, S. K.: Erratum ``On the Force-Free Nature of Photospheric Sunspot Magnetic Fields as Observed from Hinode (SOT/SP)'' (vol 744, pg 65, 2012). Astrophysical Journal 759 (2), 148 (2012)
Joshi, B.; Veronig, A. M.; Lee, J.; Bong, S.-C.; Tiwari, S. K.; Cho, K.-S.: Pre-Flare Activity and Magnetic Reconnection during the Evolutionary Stages of Energy Release in a Solar Eruptive Flare. Astrophysical Journal 743 (2), 195 (2011)
Kumar, B.; Venkatakrishnan, P.; Mathur, S.; Tiwari, S. K.; Garcia, R. A.: On the Flare-Induced Seismicity in the Active Region Noaa 10930 and Related Enhancement of Global Waves in the Sun. Astrophysical Journal 743 (1), 29 (2011)
Ravindra, B.; Venkatakrishnan, P.; Tiwari, S. K.; Bhattacharyya, R.: Evolution of Currents of Opposite Signs in the Flare-productive Solar Active Region NOAA 10930. Astrophysical Journal 740, 19 (2011)
Analyzing the high spatial resolution solar Ca II H and K emission data obtained by the SUNRISE mission and building a model of other stars more active than the Sun
The Planetary Plasma Environments group (PPE) has a strong heritage in the exploration of planetary magnetospheres and space plasma interactions throughout the solar system. It has contributed instruments to several past missions that flew-by or orbited Jupiter (Galileo, Cassini, Ulysses). The PPE participates in the JUICE mission by contributing hardware and scientific expertise to the Particle Environment Package (PEP).
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.