Coronal mass ejections (CMEs) are the largest-scale eruptive phenomenon in the solar
system, expanding from active region-sized nonpotential magnetic structure to a much larger …

The evolution of active regions (AR) from their emergence through their long decay process
is of fundamental importance in solar physics. Since large-scale flux is generated by the …

We analyze the physical mechanisms that form a three-dimensional coronal flux rope and
later cause its eruption. This is achieved by a zero-β magnetohydrodynamic (MHD) …

Strong solar flares and coronal mass ejections, here defined not only as the bursts of
electromagnetic radiation but as the entire process in which magnetic energy is released …

Solar flares result from some electromagnetic instability that occurs within regions of
relatively strong magnetic field in the Sun's atmosphere. The processes that enable and …

The magnetic field of the Sun is the underlying cause of the many diverse phenomena
combined under the heading of solar activity. Here we describe the magnetic field as it …

We present the first quantitative comparison between the total magnetic reconnection flux in
the low corona in the wake of coronal mass ejections (CMEs) and the magnetic flux in …

In this paper we study a class of three-dimensional magnetohydrodynamic model problems
that may be useful to understand the role of twisted flux ropes in coronal mass ejections. We …

Solar flares and coronal mass ejections are associated with rapid changes in field
connectivity and are powered by the partial dissipation of electrical currents in the solar …

Coronal mass ejections (CMEs) were discovered in the early 1970s when space-borne
coronagraphs revealed that eruptions of plasma are ejected from the Sun. Today, it is known …