Μάθημα : Ενημέρωση φοιτητών κατεύθυνσης Αστροφυσικής

Abstract: Powerful solar eruptions are known to produce large variety of physical phenomena: energetic flares resulting from magnetic reconnection, driving fast and wide mass ejections and shock waves, producing energetic non-thermal particles, etc. The relationship between these phenomena is a subject of long-lasting research activity. During a solar eruption two distinct zones appear to efficiently convert some part of free energy into energetic particles and radiation: (1) flaring region where magnetic reconnection triggers the eruption and (2) shock front that develops during the expansion of the coronal mass ejection. In this presentation we will address some observational and modelling aspects of coronal shock reconstruction and their link with solar energetic particles which are measured in-situ by the heliospheric spacecraft fleet. The properties of the shock depend strongly on the state of the highly structured solar corona, modulating the efficiency of different parts of the shock in accelerating particles. We will present a couple of case studies that demonstrate a tight link between the evolution of the shock and properties of SEPs. 

https://uoa.webex.com/uoa/j.php?MTID=md5bca92b822191c0461fcaa5de4119bf

Meeting number: 2784 895 5209     

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