Overview of Solar Flares

Regularization Methods for the Solution of Inverse Problems in Solar X-ray and Imaging Spectroscopy

“…. , φ N } and Y N = R(A) are two subspaces of X and Y respectively whose dimension is N < N; it follows that a solution of problem (27) exists if and only if the datum belongs to Y N . On the contrary, if g does not belong to the range of A, then it is natural to introduce the least-squares problem…”

“…In the cases of the Kramers and the BetheHeitler cross sections, we can follow the approach described in Sect. 2.3 and compute analytically the functions φ n (E) defined in (27) and the entries of the Gram matrix given in (33). If we adopt the Kramers approximation, the explicit form of the functions φ n is given by…”

“…These transients phenomena are characterized by a sudden release of huge amounts of energy and their typical manifestations are the acceleration of electrons in the solar plasma, a notable heating of the solar atmosphere and a significant electromagnetic emission particularly in the X-ray range. All the theoretical modelizations of the physics of the solar flares formulated in the last thirty years are essentially based on the well-established equations of solar plasma physics and magnetohydrodynamics [27]. Common ground for these models is the assumption that the X-ray emission during flares is the consequence of a collisional interaction between the accelerated electrons and the ions of the plasma.…”

Preliminary analysis for a new sub-type III Solar Radio Burst (Type VI) on 11th July 2023

“…IOP Publishing doi:10.1088/1742-6596/2793/1/012011 2 SRBs are frequently associated with solar activities such as solar flares and Coronal Mass Ejection (CME). Solar flares are energetic events on the Sun that release energy from current-carrying magnetic fields [7]. It coincides with solar burst events particularly great solar flares of class X and M producing major storms [8].…”