HOT JETS IN MAGNETIC FIELDS SOLAR ACTIVE REGIONS

AbstractA review of methods of measuring magnetic fields in the solar corona using spectral-polarization observations at microwaves with high spatial resolution is presented. The methods are based on the theory of thermal bremsstrahlung, thermal cyclotron emission, propagation of radio waves in quasi-transverse magnetic field and Faraday rotation of the plane of polarization. The most explicit program of measurements of magnetic fields in the atmosphere of solar active regions has been carried out using radio observations performed on the large reflector radio telescope of the Russian Academy of Sciences — RATAN-600. This proved possible due to good wavelength coverage, multichannel spectrographs observations and high sensitivity to polarization of the instrument. Besides direct measurements of the strength of the magnetic fields in some cases the peculiar parameters of radio sources, such as very steep spectra and high brightness temperatures provide some information on a very complicated local structure of the coronal magnetic field. Of special interest are the results found from combined RATAN-600 and large antennas of aperture synthesis (VLA and WSRT), the latter giving more detailed information on twodimensional structure of radio sources. The bulk of the data obtained allows us to investigate themagnetospheresof the solar active regions as the space in the solar corona where the structures and physical processes are controlled both by the photospheric/underphotospheric currents and surrounding “quiet” corona.

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Determining the spatial configurations of the coronal magnetic fields of solar active regions

Astronomy Reports ◽

10.1134/s1063772913080064 ◽

2013 ◽

Vol 57 (8) ◽

pp. 622-635 ◽

Cited By ~ 4

Author(s):

G. V. Rudenko ◽

I. I. Mysh’yakov ◽

S. A. Anfinogentov

Keyword(s):

Magnetic Fields ◽

Active Regions ◽

Coronal Magnetic Fields ◽

Solar Active Regions ◽

Spatial Configurations

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Numerical Short-Term Solar Activity Forecasting

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318000534 ◽

2017 ◽

Vol 13 (S335) ◽

pp. 243-249 ◽

Cited By ~ 2

Author(s):

Huaning Wang ◽

Yihua Yan ◽

Han He ◽

Xin Huang ◽

Xinghua Dai ◽

...

Keyword(s):

Solar Activity ◽

Magnetic Fields ◽

Solar Atmosphere ◽

Magnetic Energy ◽

Three Dimensional ◽

Active Regions ◽

Short Term ◽

Solar Active Regions ◽

Solar Eruptions ◽

Dimensional Reconstruction

AbstractIt is well known that the energy for solar eruptions comes from magnetic fields in solar active regions. Magnetic energy storage and dissipation are regarded as important physical processes in the solar corona. With incomplete theoretical modeling for eruptions in the solar atmosphere, activity forecasting is mainly supported with statistical models. Solar observations with high temporal and spatial resolution continuously from space well describe the evolution of activities in the solar atmosphere, and combined with three dimensional reconstruction of solar magnetic fields, makes numerical short-term (within hours to days) solar activity forecasting possible. In the current report, we propose the erupting frequency and main attack direction of solar eruptions as new forecasts and present the prospects for numerical short-term solar activity forecasting based on the magnetic topological framework in solar active regions.

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A study of the localization of flares in selected active regions

Symposium - International Astronomical Union ◽

10.1017/s0074180900021720 ◽

1968 ◽

Vol 35 ◽

pp. 318-325 ◽

Cited By ~ 10

Author(s):

M. J. Martres ◽

R. Michard ◽

I. Soru-Iscovici ◽

T. Tsap

Keyword(s):

Magnetic Fields ◽

Magnetic Structure ◽

Active Regions ◽

The Other ◽

Cooperative Study ◽

Solar Active Regions

From the material gathered during the ‘Cooperative Study of Solar Active Regions’, we studied the flare locations in AR magnetic structure, and flare relations to changes in the magnetic fields and spot configurations. Besides a confirmation of previous results, we find that flares are often associated with two features of the spot configuration evolving in opposite senses, one growing, the other declining.

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Cyclotron Lines in the Spectra of Solar Flares and Solar Active Regions

International Astronomical Union Colloquium ◽

10.1017/s025292110003205x ◽

1989 ◽

Vol 104 (1) ◽

pp. 449-456

Author(s):

V. V. Zheleznyakov ◽

E. Ya. Zlotnik

Keyword(s):

Magnetic Field ◽

Magnetic Fields ◽

Cross Section ◽

Active Regions ◽

Kinetic Temperature ◽

Magnetic Tube ◽

Tube Cross Section ◽

Solar Active Regions ◽

Electron Gyrofrequency ◽

The Magnetic Field

AbstractIt was shown by Zheleznyakov and Zlotnik (1980a, b) that in complex configurations of solar magnetic fields (in hot loops above the active centres, in neutral current sheets in the preflare phase, in hot X-ray kernels in the initial flare phase) a system of cyclotron lines in the spectrum of microwave radiation is likely to be formed. Such a line was obtained by Willson (1985) in the VLA observations at harmonics of the electron gyrofrequency. This communication interprets these observations on the basis of an active region model in which thermal cyclotron radiation is produced by hot plasma filling the magnetic tube in the corona above a group of spots. In this model the frequency of the recorded 1658 MHz line corresponds to the third harmonic of electron gyrofrequency, which yields the magnetic field (196 + 4) G along the magnetic tube axis. The linewidth Af/f ∼ 0.1 is determined by the 10% inhomogeneity of the magnetic field over the cross-section of the tube; the line profile indicates the kinetic temperature distribution of electrons over the tube cross-section with the maximum value 4 x 106 K. Analysis shows that study of cyclotron lines can serve as an efficient tool for diagnostics of magnetic fields and plasma in the solar active regions and flares.

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