Radio Echo in the Turbulent Corona and Simulations of Solar Drift-pair Radio Bursts

0534354 - ASÚ 2021 RIV US eng J - Článek v odborném periodiku
Kuznetsov, A.A. - Chrysaphi, N. - Kontar, E. P. - Motorina, Galina
Radio Echo in the Turbulent Corona and Simulations of Solar Drift-pair Radio Bursts.
Astrophysical Journal. Roč. 898, č. 2 (2020), č. článku 94. ISSN 0004-637X. E-ISSN 1538-4357
Institucionální podpora: RVO:67985815
Klíčová slova: solar coronal radio emission * radio spectroscopy * noise storms
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 5.877, rok: 2020
Způsob publikování: Open access

Drift-pair bursts are an unusual type of solar low-frequency radio emission, which appear in the dynamic spectra as two parallel drifting bright stripes separated in time. Recent imaging spectroscopy observations allowed for the quantitative characterization of the drifting pairs in terms of source size, position, and evolution. Here, the drift-pair parameters are qualitatively analyzed and compared with the newly developed Monte Carlo ray-tracing technique simulating radio-wave propagation in the inhomogeneous anisotropic turbulent solar corona. The results suggest that drift-pair bursts can be formed due to a combination of refraction and scattering processes, with the trailing component being the result of turbulent reflection (turbulent radio echo). The formation of drift-pair bursts requires an anisotropic scattering with the level of plasma density fluctuations comparable to that in type III bursts, but with a stronger anisotropy at the inner turbulence scale.
Trvalý link: http://hdl.handle.net/11104/0312566