Observations and Analysis of Interplanetary Scintillation |
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Page 3
... scale size , and at an elongation of 0.5 a.u. , found that the scale size must be less than 103 km . Hewish , Scott , and Wills ( 1964 ) interpreted the observed intensity fluctuations as the consequence of electron density ...
... scale size , and at an elongation of 0.5 a.u. , found that the scale size must be less than 103 km . Hewish , Scott , and Wills ( 1964 ) interpreted the observed intensity fluctuations as the consequence of electron density ...
Page 68
... scale size , or by some combina- tion of the two . Sharp and Harris ( 1967 ) in a similar an- alysis , found no evidence for a change in irregularity scale based on solar wind velocity data from Wolfe , et . al . ( 1966 ) and Neugebauer ...
... scale size , or by some combina- tion of the two . Sharp and Harris ( 1967 ) in a similar an- alysis , found no evidence for a change in irregularity scale based on solar wind velocity data from Wolfe , et . al . ( 1966 ) and Neugebauer ...
Page 154
... scale is not related to the pulse period or pulse width , then by in- tegrating over a time interval more than an order of magnitude greater than the characteristic time scale ( as for NP0527 ) much of the fluctuation power will be lost ...
... scale is not related to the pulse period or pulse width , then by in- tegrating over a time interval more than an order of magnitude greater than the characteristic time scale ( as for NP0527 ) much of the fluctuation power will be lost ...
Contents
EXAMINATION OF SCINTILLATION BEHAVIOR | 10 |
FLUCTUATION SPECTRA AND SOURCE STRUCTURE | 78 |
INTERPLANETARY SCINTILLATION OF PULSARS | 127 |
2 other sections not shown
Common terms and phrases
angular diameter angular structure Ap.J arc sec Arecibo calculated Cohen complex source CORNELL CORNELL CORNELL LIBRARY Cornell University curve Ekers Elongation Modulation index equation F₂ Hz factor flare fluctuation power flux at 430 frequency proportional frequency spectrum function of frequency function of solar Gaussian Hewish index and square-root indicate intensity fluctuations interplanetary medium interplanetary scintillations interstellar medium interstellar scattering Jauncey km/sec LIBRARY CORNELL Lovelace lunar occultation measured meter wavelengths Nyquist frequency observations point source position angle Power spectrum power-law pulsar pulse radiation radio frequency radio sources Relative power density resolved Salpeter samples scale scattering angle scin screen second-moment values signal/noise Sine of Solar Solar Elongation Figure Solar Elongation Modulation solar wind velocity spectra square-root second square-root second moment strong scintillation regime tillation tion tiplied UNIVERSITY CORNELL value of µ VLBI VLBI data VLBI results wavenumber spectrum weak scintillation regime