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Ukrainian T-shaped radio telescope (UTR-2)

Anisotropic density turbulence variation from the low corona to 1 au as deduced from solar radio observations by E. Kontar et al.

2023-11-30

Density turbulence in the solar corona and solar wind is evident via the properties of solar radio bursts; angular scattering-broadening of extra-solar radio sources observed through the solar atmosphere, and can be measured in-situ in the solar wind. A viable density turbulence model should simultaneously explain all three types of density fluctuation observations. Solar radio bursts (e.g. Type I, II, III) observed below ~1 GHz are produced predominantly via plasma […]

Morphology of solar type II bursts caused by shock propagation through turbulent and inhomogeneous coronal plasma by A. Koval et al

2023-09-26

Type II solar bursts are radio signatures of shock waves in the solar corona driven by solar flares or coronal mass ejections. Therefore, these bursts present complex spectral morphologies in solar dynamic spectra. In particular, the radio emission lane may separate into two thinner bands that is known as band-splitting (Vršnak et al., 2002). “Fractured” type II bursts, exhibiting spectrally indented shapes in the form of bumps or breaks, are […]

Remote sensing the coronal magnetic field using solar S-bursts B. Clarke et al.*

2019-04-09

Solar activity is often accompanied by solar radio emission. At low frequencies, radio bursts with short durations of <1 s, known as solar S-bursts, have been identified. These intriguing, low frequency bursts were first identified by McConnell (1982) who named them solar S-bursts, owing to their similarity to Jovian S-bursts: the S stands for short or storm. S-bursts appear as narrow tracks on a dynamic spectrum that usually drift from […]

Properties of Decameter IIIb–III Pairs
by V. Melnik et al.*

2018-05-29

A large number of Type IIIb–III pairs, in which the first component is a Type IIIb burst and the second one is a Type III burst, are often observed during decameter Type III burst storms. From the beginning of their detection, the question of whether the components of these pairs are the first and the second harmonics of radio emission or not has remained open. We discuss properties of decameter […]

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Atacama Large Millimeter Array (ALMA) (11) chromosphere (13) coronal magnetic field (14) Coronal Mass Ejection (CME) (43) density fluctuations (14) electron cyclotron maser (ECM) (4) energetic electrons (14) fine spectral structures (4) free-free emission (8) Giant Metrewave Radio Telescope (GMRT) (3) gyrosynchrotron emission (13) hard X-ray (5) ionosphere (4) Langmuir waves (8) Low Frequency Array (LOFAR) (21) microwave emission (15) Murchison Widefield Array (MWA) (10) Nancay Radio Heliograph (NRH) (5) Nobeyama Radioheliograph (NoRH) (8) Parker Solar Probe (PSP) (11) particle acceleration (8) plasma radio emission (6) Quasi-periodic pulsations (QPP) (4) quiet Sun (9) radio spikes (11) radio wave scattering (13) shock wave (8) simulations (4) Solar Dynamics Observatory (SDO) (4) solar energetic particles (SEP) (24) solar flare (29) Solar Orbiter (SolO) (7) solar radio emission (20) space weather (4) STEREO (10) submillimeter emission (4) turbulence (18) Type III solar radio bursts (66) Type II solar radio bursts (38) Type I solar radio bursts (7) Type IV solar radio bursts (11) Ukrainian T-shaped radio telescope (UTR-2) (4) Ultraviolet (UV)/extreme ultraviolet (EUV) emissions (6) Wind (spacecraft) (7) zebra-structure (7)
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  • Connecting energetic electrons at the Sun and in the heliosphere through X-ray and radio diagnostics by D. Paipa-Leon et al.

    2025-06-10

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