Results 141 to 150 of about 1,793,812 (174)

Reversal of the Sense of Polarisation in Solar and Stellar Radio Flares

Publications of the Astronomical Society of Australia, 1994
AbstractIt is shown that numerical integration of the equation of polarisation transfer for generalised Faraday rotation provides an alternative to mode-coupling theory for treating propagation through a quasi-transverse (QT) region. At a QT region, where the sign of the component of the magnetic field along the ray path reverses, the sense of circular
D. B. Melrose, P. A. Robinson
openaire   +1 more source

Homology of solar flare-associated radio events

Solar Physics, 1967
The concept of homology, introduced by Ellison, McKenna, and Rceid (1960) for optical flares, can be extended to flare-associated radio events. Successive flares within the same centre of activity sometimes produce radio events that are remarkably similar.
openaire   +1 more source

Directivity of Radio Emission from Solar Flares

Publications of the Astronomical Society of Japan, 1985
Abstract The center-limb variation of the solar microwave burst intensity is investigated statistically with a sufficient number of events (~ 1000) at 17 GHz far above the mean turnover frequency of the microwave burst spectrum. The intensity of bursts (except that of GRF bursts) is independent of the disk longitude, which is slightly ...
openaire   +1 more source

Polarization of radio emission of the turbulent plasma of solar flares

Radiophysics and Quantum Electronics, 1996
We present a mechanism for the appearance of circular polarization due to the scattering of electromagnetic radiation by the turbulent pulsations of a plasma with a magnetic field. The application of this mechanism to the turbulent plasma of solar flares is discussed.
V. V. Tirskii, V. M. Tomozov
openaire   +1 more source

Radio Imaging Observation of a Solar Flare Cusp

1996
A Gradual Rise and Fall type solar radio event on the east limb was observed by the Nobeyama Radio Heliograph. The event started 23 UT on May 1, 1993 and lasted more than four hours. Radio images synthesized every three minutes showed a cusp shape in the later phase of the event. The peak radio flux was 6 sfu and the GOES X-ray classwas C6.
openaire   +1 more source

On the Nature of Modulation of Radio Emission During Solar Flares

Solar Physics, 1998
The distribution of pauses between subsequent elements of a periodic process is symmetric, while a random process produces an asymmetric exponential distribution. The third moment of the pause distribution, which is sensitive to the asymmetry, can therefore be used to discriminate between perodic and random processes.
Y. Yurovsky, A. Magun
openaire   +1 more source

Radio Bursts after a Solar Flare (L)

1987
Solar radio bursts have been classified by Australian radioastronomers (P. Wild and others) — see Figure 57. After a solar flare we observe: (a) several bursts of type III; (b) in some cases a burst of type II. These phenomena become understandable when the radiospectrum is recorded: this is done with a cathode-ray tube on a 35 mm film.
openaire   +1 more source

Radio Bursts after a Solar Flare (L)

1969
After a solar flare we observe: (a) several bursts of type III; (b) in some cases a burst of type II. These phenomena become understandable when the radiospectrum is recorded: this is done with a cathode-ray tube on a 35 mm film.
openaire   +1 more source

The Solar Flare Phenomenon as Seen at Radio Frequencies

1965
Observations of the sun in “white” light detect almost exclusively the light emitted by the photosphere, which is a thin layer of gas between 200 and 400 km thick. Above the photosphere lies the chromosphere, which can be observed during a total eclipse as a faint region of reddish emission around the solar disk when the much brighter photospheric ...
openaire   +1 more source

Solar Flare and Radio Burst Effects on GNSS Signals and the Ionosphere During September 2017

Radio Science, 2022
Inez S Batista, Weverton da Costa Silva, Mangalathayil A Abdu   +2 more
exaly