A Nonlinear Force-Free Field Model to Reconstruct the Sun's Coronal Magnetic Fields
2019
Sun is a magnetically active star. Magnetic activity of the Sun has a significant impact on
Earth as intense solar eruptions like flares and coronal mass ejections (CMEs) can cause
disturbances in our telecommunication systems, degradation of satellites, power cutoffs, and
pose a danger of life-threatening radiation for astronauts. The magnetic field in solar corona
plays a major role in these solar eruptions. The free (non-potential) energy stored in coronal
magnetic fields determines the occurrence and intensity of these outbursts from the Sun. So,
studying the magnetic field in corona is essential to understand the origin and evolution of
these eruptive phenomena. At present, it difficult to directly measure the vector magnetic
field in the corona through observations, therefore computational models are required to
study the coronal magnetic fields.
In this thesis, a Nonlinear Force-Free Field (NLFFF) model is developed in spherical
geometry to study the magnetic field structures in the solar corona. This model is based
on extrapolation techniques utilizing the vector magnetic field measurements of the solar
photosphere (visible surface of the Sun). The model reconstructs magnetic field for solar
corona that is in a force-free equilibrium state.
We evaluate the quality of reconstruction of the coronal magnetic fields obtained from
the NLFFF model by comparing it with the configuration given by an analytical solution. We
consider two such cases, and the associated results are presented in this thesis in the context
of model validation.
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