Chitta, L. P.; Zhukov, A. N.; Berghmans, D.; Peter, H.; Parenti, S.; Mandal, S.; Aznar Cuadrado, R.; Schühle, U.; Teriaca, L.; Auchère, F.et al.; Barczynski, K.; Buchlin, É.; Harra, L.; Kraaikamp, E.; Long, D. M.; Rodriguez, L.; Schwanitz, C.; Smith, P. J.; Verbeeck, C.; Seaton, D. B.: Picoflare jets power the solar wind emerging from a coronal hole on the Sun. Science 38, pp. 867 - 872 (2023)
Li, Z.; Cheng, X.; Ding, M. D.; Chitta, L. P.; Peter, H.; Berghmans, D.; Smith, P. J.; Auchère, F.; Parenti, S.; Barczynski, K.et al.; Harra, L.; Schühle, U.; Buchlin, É.; Verbeeck, C.; Aznar Cuadrado, R.; Zhukov, A. N.; Long, D. M.; Teriaca, L.; Rodriguez, L.: Evidence of external reconnection between an erupting mini-filament and ambient loops observed by Solar Orbiter/EUI. Astronomy and Astrophysics 673, p. A83 (2023)
Chitta, L. P.; Seaton, D. B.; Downs, C.; DeForest, C. E.; Higginson, A. K.: Direct observations of a complex coronal web driving highly structured slow solar wind. Nature Astronomy (2022)
Chitta, L. P.; Peter, H.; Young, P.R.: Extreme-ultraviolet bursts and nanoflares in the quiet-Sun transition region and corona. Astronomy and Astrophysics 647, A159 (2021)
Chitta, L. P.; Priest, E. R.; Cheng, X.: From Formation to Disruption: Observing the Multiphase Evolution of a Solar Flare Current Sheet. The Astrophysical Journal 911 (2), 133 (2021)
Dr. Theodosios Chatzistergos receives award by the European Space Weather and Space Climate Association for his research findings on the historical activity of the Sun.
The Zdenĕk Švetska Senior Prize of the Solar Physics Division of the European Physical Society (EPS) recognizes Solanki’s pioneering contributions to solar research.
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 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.