The Radio-Wave Scattering Properties of the Solar Corona.

1964 ◽  
Vol 139 ◽  
pp. 1290 ◽  
Author(s):  
W. C. Erickson
Keyword(s):  
Solar Corona ◽  
Radio Wave ◽  
Wave Scattering

scholarly journals LOFAR observations of radio burst source sizes and scattering in the solar corona

2020 ◽  
Vol 645 ◽  
pp. A11
Author(s):  
Pearse C. Murphy ◽  
Eoin P. Carley ◽  
Aoife Maria Ryan ◽  
Pietro Zucca ◽  
Peter T. Gallagher
Keyword(s):  
Solar Corona ◽  
Radio Source ◽  
Radio Wave ◽  
Radio Burst ◽  
Wave Scattering ◽  
Low Frequency ◽  
Density Fluctuations ◽  
Source Size ◽  
Burst Source ◽  
Low Frequencies

Low frequency radio wave scattering and refraction can have a dramatic effect on the observed size and position of radio sources in the solar corona. The scattering and refraction is thought to be due to fluctuations in electron density caused by turbulence. Hence, determining the true radio source size can provide information on the turbulence in coronal plasma. However, the lack of high spatial resolution radio interferometric observations at low frequencies, such as with the LOw Frequency ARray (LOFAR), has made it difficult to determine the true radio source size and level of radio wave scattering. Here we directly fit the visibilities of a LOFAR observation of a Type IIIb radio burst with an elliptical Gaussian to determine its source size and position. This circumvents the need to image the source and then de-convolve LOFAR’s point spread function, which can introduce spurious effects to the source size and shape. For a burst at 34.76 MHz, we find full width at half maximum (FWHM) heights along the major and minor axes to be 18.8′ ± 0.1′ and 10.2′ ± 0.1′, respectively, at a plane of sky heliocentric distance of 1.75 R⊙. Our results suggest that the level of density fluctuations in the solar corona is the main cause of the scattering of radio waves, resulting in large source sizes. However, the magnitude of ε may be smaller than what has been previously derived in observations of radio wave scattering in tied-array images.

scholarly journals Radio wave scattering in the outer heliosphere

2000 ◽  
Vol 105 (A3) ◽  
pp. 5149-5156 ◽  
Author(s):  
J. W. Armstrong ◽  
W. A. Coles ◽  
B. J. Rickett
Keyword(s):  
Radio Wave ◽  
Wave Scattering ◽  
Outer Heliosphere

scholarly journals Non‐Gaussian Radio‐Wave Scattering in the Interstellar Medium

2006 ◽  
Vol 640 (1) ◽  
pp. 344-352 ◽  
Author(s):  
Stanislav Boldyrev ◽  
Arieh Konigl
Keyword(s):  
Interstellar Medium ◽  
Radio Wave ◽  
Wave Scattering ◽  
Non Gaussian

scholarly journals The Galactic Distribution of Electron Density Microstructure Inferred from Radio Scattering Observations

2001 ◽  
Vol 182 ◽  
pp. 11-16
Author(s):  
James Cordes
Keyword(s):  
Interstellar Medium ◽  
Radio Wave ◽  
Electron Density ◽  
Wave Scattering ◽  
Galactic Model ◽  
Dispersion Measures ◽  
Pulse Broadening ◽  
Galactic Distribution

AbstractI first review the observables and optics of interstellar seeing associated with radio wave scattering in the interstellar medium. I then describe the Galactic distribution of electron density and its fluctuations, as inferred from a number of observables, including angular and pulse broadening, diffractive scintillations, and dispersion measures. Propects for improving the Galactic model are outlined.

scholarly journals Monitoring source variability with the Fast All Sky Telescope

1991 ◽  
Vol 131 ◽  
pp. 445-448
Author(s):  
Kenneth J. Johnston ◽  
Ralph L. Fiedler ◽  
Richard S. Simon
Keyword(s):  
Interstellar Medium ◽  
Radio Wave ◽  
Wave Scattering ◽  
Study Time ◽  
Time Variability ◽  
Radio Sources ◽  
Limited Sample ◽  
Extragalactic Radio Sources ◽  
Design Goal ◽  
Celestial Sphere

AbstractThe proposed Fast All Sky Telescope (FAST) is an interferometer which is intended to monitor the northern four-fifths of the celestial sphere every two days at 8.1 GHz and daily at 2.7 GHz. The design goal is to have a rms sensitivity of 10 mJy/beam at both frequencies. The array is planned to comprise 20 3-meter diameter antennas with a maximum baseline of 0.7 km. FAST will provide a valuable database that may be used to study time variability in a sensitivity limited sample of radio sources. This will significantly impact on the understanding of active Galactic and extragalactic radio sources, as well as on the understanding of radio wave scattering in the interstellar medium.

Role of radio wave reflection during radio occultation by the solar corona

1985 ◽  
Vol 28 (7) ◽  
pp. 549-556 ◽  
Author(s):  
A. I. Kucheryavenkov ◽  
A. G. Pavel'ev ◽  
S. N. Rubtsov ◽  
O. I. Yakovlev
Keyword(s):  
Solar Corona ◽  
Radio Wave ◽  
Radio Occultation ◽  
Wave Reflection
Sign in / Sign up

Export Citation Format

Share Document