Studying the solar corona, due to its vicinity, is the starting point to understand stellar activity. The emission measure distribution vs temperature, EM(T), is a useful tool to study coronal plasmas, in fact it allows: to investigate the energy balance of coronal plasmas, to easily compare different stars, and also to compare the solar corona to that of other active stars irrespective of the very different observing techniques. The EM(T) of the solar corona differs significantly, in terms of average plasma temperatures, peak temperatures, and total emission measure, with respect to that of active stars. In this work it is discussed how the evaluation of the EM(T) of the solar corona, and of its components (quiescent plasma, active regions, flares, etc.), parallel to the reconstruction of the EM(T) of stars at different activity levels, can be used to investigate coronal physics.
|Numero di pagine||1|
|Stato di pubblicazione||Published - 2010|