Solar Dynamics Observatory (SDO)

Spectroscopic Imaging of the Sun with MeerKAT: Opening a New Frontier in Solar Physics by Kansabanik et al.

2024-04-10

Since the discovery of solar radio emission in the late 1940s, the Sun has been studied in great detail across a wide range of frequencies from a few tens of kHz to several hundreds of GHz. Solar radio emissions provide several unique diagnostics of the solar corona, which are otherwise simply inaccessible. Despite this long history of observations and studies, the Sun still harbors several mysteries. Improved observations from the […]

Energy budget of plasma motions, heating, and electron acceleration in a three-loop solar flare
by G. Motorina et al.*

2021-07-06

The solar flare phenomenon is a complex process in the solar atmosphere where non-potential magnetic energy is released and converted into other forms of energy, such as nonthermal energy of accelerated particles, thermal energy of heated flaring plasma, kinetic energy of eruptions, jets, up/down flows, and stochastic (turbulent) plasma motions. The processes lying behind initial division between energy components, distribution of these components among flaring loops and their evolution are […]

Solar Radio Burst Associated with a Falling Bright EUV Blob
by M. Karlický et al.*

2018-06-12

In several papers the thermal conduction front formed between hot and cold plasmas was studied (Brown et al. 1979, McKean et al 1990, Arber & Melnikov 2009). Karlický (2015) has studied the thermal front using a 3-D particle-in-cell electromagnetic code and found that the thermal front can produce radio emission. Here we present a very rare radio burst which we interpreted as generated by the thermal conduction front formed in […]

The Brightness Temperature of the Quiet Solar Chromosphere at 2.6 mm
by Kazumasa Iwai et al

2017-04-25

The brightness temperature of the Sun constitutes a basic property of the solar atmosphere. The main emission mechanism of the Sun at millimeter and submillimeter wavelengths is thermal free–free emission from the chromosphere, which is an atmospheric layer with a temperature ranging between 6000 to 20,000 K. The opacity of thermal free–free emission depends on the temperature and density in the emission region. In addition, the Rayleigh– Jeans law is applicable […]

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