Guo, Y.; Pariat, E.; Valori, G.; Anfinogentov, S.; Chen, F.; Georgoulis, M. K.; Liu, Y.; Moraitis, K.; Thalmann, J. K.; Yang, S.: Magnetic Helicity Estimations in Models and Observations of the Solar Magnetic Field. III. Twist Number Method. Astrophysical Journal 840 (1), 40 (2017)
Hong, J.; Ding, M. D.; Li, Y.; Yang, K.; Cheng, X.; Chen, F.; Fang, C.; Cao, W.: Bidirectional Outflows as Evidence Of Magnetic Reconnection Leading to a Solar Microflare. Astrophysical Journal 820 (1), L17 (2016)
Valori, G.; Pariat, E.; Anfinogentov, S.; Chen, F.; Georgoulis, M. K.; Guo, Y.; Liu, Y.; Moraitis, K.; Thalmann, J. K.; Yang, S.: Magnetic Helicity Estimations in Models and Observations of the Solar Magnetic Field. Part I: Finite Volume Methods. Space Science Reviews 201 (1-4), pp. 147 - 200 (2016)
Chen, F.; Peter, H.: Using coronal seismology to estimate the magnetic field strength in a realistic coronal model. Astronomy and Astrophysics 581, A137 (2015)
Cheung, M. C. M.; Boerner, P.; Schrijver, C. J.; Testa, P.; Chen, F.; Peter, H.; Malanushenko, A.: Thermal Diagnostics with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions. Astrophysical Journal 807, 143 (2015)
Zhang, J.; Zhang, B.; Li, T.; Yang, S.; Zhang, Y.; Li, L.; Chen, F.; Peter, H.: Coronal Heating By the Interaction between Emerging Active Regions and the Quiet Sun Observed By the Solar Dynamics Observatory. Astrophysical Journal 799, L27 (2015)
Chen, F.; Peter, H.; Bingert, S.; Cheung, M. C. M.: A model for the formation of the active region corona driven by magnetic flux emergence. Astronomy and Astrophysics 564, A12 (2014)
Li, L. P.; Peter, H.; Chen, F.; Zhang, J.: Conversion from mutual helicity to self-helicity observed with IRIS. Astronomy and Astrophysics 570, A93 (2014)
Chen, F.; Peter, H.: Using coronal seismology to estimate the magnetic field strength in a realistic coronal model. 2nd International Sino-German Symposium of Solar Physics: Multi Waveband Observations and Modeling of Solar Activity, Bad Honnef, Germany (2015)
Chen, F.; Peter, H.; Bingert, S.: Magnetic Field Lines and Coronal Loops A Difficult Relation. Living With a Star / Iris / Hinode Meeting, Portland, USA (2014)
Chen, F.; Peter, H.; Bingert, S.; Cheung, M. C. M.: Magnetic field lines and coronal loops. 14th European Solar Physics Meeting, Dublin, Ireland (2014)
Chen, F.; Peter, H.: Using coronal seismology to estimate the magnetic field strength in a realistic coronal model. Hinode 9 Science Meeting, Belfast, Ireland (2015)
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".