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Space physics is the study of the natural phenomenon that occur in our solar system. Specifically, the sun, the particles and radiation it creates and how these affect the planets. This includes the solar wind and its interaction with the Earth and near-Earth space; so-called space weather.
What mechanisms power the heating of the solar atmosphere is a long-standing, complex question. Satellite and sounding-rocket observations, coupled with computer simulations, now support the idea that dissipation of electrical currents causes strong heating in the brightest parts of the solar chromosphere and corona.
Magnetohydrodynamic (MHD) waves observed on the Sun help understanding solar plasma and involved processes. Here, the authors show resolved MHD waves in the solar corona displaying MHD lensing effect.
Analysis of high-resolution observations of solar ‘plage’ regions (areas of high magnetic field) shows a correlation between coronal emission and the thermodynamic properties of the chromosphere below. Simulations suggest the same heating source.
Venus lacks a magnetic field, leading to interactions between the solar wind and its atmosphere. During its Venus fly-by, BepiColombo observed planetary C+ and O+ escape into space due to this interaction, which is important for understanding atmospheric evolution.
Turbulence plays a key role in space and astrophysical plasmas. The study reports evidence of the weak-to-strong transition when Alfvénic turbulence cascades from large to small scales revealed from the Cluster observation of space plasma.
What mechanisms power the heating of the solar atmosphere is a long-standing, complex question. Satellite and sounding-rocket observations, coupled with computer simulations, now support the idea that dissipation of electrical currents causes strong heating in the brightest parts of the solar chromosphere and corona.