Conveners
Poster Session 7.4
- Francesca Zuccarello (Istituto Nazionale di Astrofisica (INAF))
One of the possible reasons for heating both open and closed magnetic field regions of the solar corona is due to the MHD turbulence. In this work, we have estimated the density filling factor which plays a crucial role as a correction factor for the energy flux for the Alfv{\'e}n waves and kink waves. We have employed an ideal 3D MHD simulation for an open magnetic structure using MPI-AMRVAC...
Oscillations in solar active regions are mainly due to leakage of
acoustic oscillations that are trapped inside the Sun. Doppler
velocity and intensity measurements are known to clearly show these
oscillations in magnetic structures. In recent years, magnetic field
fluctuations have been reported in both the photosphere and
chromosphere. The reason for these observed oscillations in...
Three-dimensional (3D) magnetohydrodynamic simulation is performed to explore the process of magnetic reconnection at the 3D magnetic nulls and quasi-separatrix layers (QSLs). The initial magnetic field is constructed analytically by superposing uniform vertical magnetic field on a linear force-free field. The initial field is characterized by the presence of a...
Solar flares are an explosive manifestation of complex magnetic loop reconfigurations in the vicinity of active regions in the solar atmosphere. During a flaring event, the magnetic field topology changes rapidly, abruptly, and significantly. Some of these eruptive events inject enough energy into the photosphere and sub-photosphere to generate acoustic responses observed as sunquakes. The...
The solar radio emission is usually divided into three parts depending of the time scale of the events: (1) the quiet Sun as a background emission, (2) a slowly varying component mostly associated with the active regions and (3) occasional extreme and sudden energetic phenomena like coronal mass ejections and flares. The quiet Sun emission comes from thermal bremsstrahlung in local...
The solar radiation in the Lyman-alpha and Mg II h&k spectral lines plays a crucial role in the illumination of chromospheric and coronal structures, such as prominences/filaments, spicules, chromospheric fibrils, cores of coronal mass ejections, or solar wind. Moreover, it is important for the investigation of the heliosphere, Earth ionosphere, and the atmospheres of planets, moons, and...
We present a high fidelity snapshot spectroscopic radio imaging study of a weak type I solar noise storm which took place during an otherwise exceptionally quiet time. Using high fidelity images from the Murchison Widefield Array, we track the observed morphology of the burst source for 70 minutes and identify multiple instances where its integrated flux density and area are strongly...
