Hydrodynamic instabilities such as Rayleigh–Taylor (RT) and Richtmyer–Meshkov (RM)
instabilities usually appear in conjunction with the Kelvin–Helmholtz (KH) instability and are …

Abstract Rayleigh–Taylor (RT) and Richtmyer–Meshkov (RM) instabilities are well-known
pathways towards turbulent mixing layers, in many cases characterized by significant mass …

Solar prominences are one of the most common features of the solar atmosphere. They are
found in the corona but they are one hundred times cooler and denser than the coronal …

Magnetic flux emergence from the solar convection zone into the overlying atmosphere is
the driver of a diverse range of phenomena associated with solar activity. In this article, we …

Prominences and filaments are manifestations of magnetized, levitated plasma within the
solar coronal atmosphere. Their structure is assumed to be driven by the ambient magnetic …

Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot
corona. A comprehensive understanding of solar prominences ultimately requires complex …

Flows and instabilities play a major role in the dynamics of magnetized plasmas including
the solar corona, magnetospheric and heliospheric boundaries, cometary tails, and …

Partially ionized plasmas are found across the Universe in many different astrophysical
environments. They constitute an essential ingredient of the solar atmosphere, molecular …

Hinode is Japan's third solar mission following Hinotori (1981–1982) and Yohkoh (1991–
2001): it was launched on 2006 September 22 and is in operation currently. Hinode carries …

Current analytical and numerical modeling suggest the existence of ubiquitous thin current
sheets in the corona that could explain the observed heating requirements. On the other …