Physics
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999spro.proc...41g&link_type=abstract
Solar Physics with Radio Observations, Proceedings of the Nobeyama Symposium, held in Kiyosato, Japan, Oct. 27-30, 1998, Edited
Physics
3
Scientific paper
Localized increase of the magnetic field observed by routine methods on the photosphere result in the growth of a number of active processes in the solar atmosphere and the heliosphere. These localized regions of increased magnetic field are called active regions (AR). The main processes of transfer, accumulation and release of energy in an AR is, however, out of scope of photospheric observations being essentially a 3D-process and happening either under photosphere or up in the corona. So, to investigate these plasma structures and processes we are bound to use either extrapolation of optical observational methods or observations in EUV, X-rays and radio. In this review, we stress and illustrate the input to the problem gained from radio astronomical methods and discuss possible future development of their applicatications. Historically speaking each new step in developing radio technique of observations resulted in detecting some new physics of ARs. The most significant progress in the last few years in radio diagnostics of the plasma structures of magnetospheres of the solar ARs is connected with the developing of the 2D full disk analysis on regular basis made at Nobeyama and detailed multichannel spectral-polarization (but one-dimensional and one per day) solar observations at the RATAN-600. In this report the bulk of attention is paid to the new approach to the study of solar activity gained with the Nobeyama radioheliograph and analyzing the ways for future progress. The most important new features of the multicomponent radio sources of the ARs studied using Nobeyama radioheliograph are as follow: 1. The analysis of magnetic field structures in solar corona above sunspot with 2000 G. Their temporal evolution and fluctuations with the periods around 3 and 5 minutes, due to MHD-waves in sunspot magnetic tubes and surrounding plasma. These investigations are certainly based on an analysis of thermal cyclotron emission of lower corona and CCTR above sunspot umbra. 2. Magnetography of the solar active regions presenting the weak magnetic fields (with the sensitivity of several G) reflecting longitude component of the magnetic field in chromosphere and corona and solar faculae structure. The method is based on an analysis of the weak polarization (of the order of 1% or less). 3. An analysis of the structure, temperature, and density of arches seen above neutral magnetic field lines (seen in most ARs with spots and without ones). 4. Study of temporal and spatial behavior of inversion of the sign of the circular polarization with the result of magnetography of the solar corona. 5. An analysis of the solar activity at high heliographic latitudes, observed mostly as polar faculae (increased brightness structures having counterparts in optical white light observations). In modern study of the solar activity analysis of the activity of polar zones are of principal importance. Nobeyama probably presents the most reliable way to study this. The above points present not exactly completed results but rather the directions for future studies. These should use full time coverage of observations at different phases of the solar activity and combination of observations with other radio, optical, EUV and X-ray observations whenever possible.
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