Optimum algorithm for processing the observational data on polarization of distributed Galaxy radio emission

A. A. Petrovskii

doi:10.1007/bf01038783

A Cyclotron Theory for the Beaming Pattern of Jupiter’s Decametric Radio Emission

Publications of the Astronomical Society of Australia ◽

10.1017/s132335800001643x ◽

1981 ◽

Vol 4 (2) ◽

pp. 221-226 ◽

Cited By ~ 34

Author(s):

R. G. Hewitt ◽

D. B. Melrose ◽

K. G. Rönnmark

Keyword(s):

Magnetic Field ◽

Radio Emission ◽

Observational Data ◽

Theoretical Interpretation ◽

Theoretical Interest ◽

Hollow Cone ◽

The Past ◽

Jovian Magnetosphere ◽

Half Angle ◽

Occurrence Pattern

Ground-based observations of Jupiter’s decametric radio emission (DAM) have been reviewed by Ellis (1965), Warwick (1967, 1970) and Carr and Gulkis (1969). A startling feature of DAM is the modulating effect of Io, and interpretation of the Io effect has dominated theoretical discussions of DAM until quite recently, specifically until the fly-by s of Voyagers 1 and 2. The Voyager data showed that the DAM appears as nested arcs in the frequency-Jovian longitude plane (Warwick et al. 1979, Boischot et al. 1981). The interpretation of this arc structure has been of primary theoretical interest over the past two years. The most widely adopted explanation is that the emission from each point is confined to the surface of a hollow cone (Goldstein and Thieman 1981). This idea is not new: emission on the surface of a cone was discussed by Ellis and McCulloch (1963); Dulk (1967) derived detailed parameters for the cone (half angle 79° width 1°) from the occurrence pattern of DAM; and Goldreich and Lynden-Bell (1969) presented a theoretical interpretation of it. More recently Goldstein et al. (1979) used observational data on the Jovian magnetic field in deriving properties of the required emission cone. It seems that one requires the properties of the emission cone to vary with position in the Jovian magnetosphere to account for the nested arc pattern (Goldstein and Thieman 1981; Gurnett and Goertz 1981).

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Evolution of the Radio Emission from Young SNRs according to Observational Data

Australian Journal of Physics ◽

10.1071/ph790095 ◽

1979 ◽

Vol 32 (2) ◽

pp. 95 ◽

Cited By ~ 3

Author(s):

KS Stankevich

Keyword(s):

Experimental Data ◽

Radio Emission ◽

Flux Density ◽

Observational Data ◽

Spectral Index ◽

Density Measurements ◽

The Past ◽

Absolute Flux ◽

Density Decrease ◽

Frequency Variations

Results are given from a still-continuing series of absolute flux density measurements for the SNR CasA. The measurements have been taken regularly over the past 16 years at 24 wavelengths in the range 3-60 cm. New data are presented for the rate of flux density decrease, and for time and frequency variations in the spectral index. Intensity increases that are localized in frequency are described. The results are generalized in a model for the radio emission from a young SNR, and this is used to analyse experimental data for flux density decreases in the emission from 3C 10 and 58.

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A dependence between optical and radio luminosities of quasars after all?

Symposium - International Astronomical Union ◽

10.1017/s0074180900152398 ◽

1986 ◽

Vol 119 ◽

pp. 109-110

Author(s):

Jerzy Machalski

Keyword(s):

Radio Emission ◽

Observational Data

It is still uncertain whether optical and radio emission mechanisms in AGNs are coupled or not, and how? New observational data give more light on this subject.

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Current status of special planetary and lunar theories and ephemerides

Symposium - International Astronomical Union ◽

10.1017/s007418090010556x ◽

1966 ◽

Vol 25 ◽

pp. 266-267

Author(s):

R. L. Duncombe

Keyword(s):

Observational Data ◽

Current Status ◽

Numerical Errors

An examination of some specialized lunar and planetary ephemerides has revealed inconsistencies in the adopted planetary masses, the presence of non-gravitational terms, and some outright numerical errors. They should be considered of temporary usefulness only, subject to subsequent amendment as required for the interpretation of observational data.

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July 11, 1991 Eclipse Corona Photometry by the Results of Electropolarimetric and CCD-Matrix Observations

International Astronomical Union Colloquium ◽

10.1017/s0252921100026051 ◽

1994 ◽

Vol 144 ◽

pp. 567-569

Author(s):

V. Kulidzanishvili ◽

D. Georgobiani

Keyword(s):

Solar Corona ◽

Observational Data ◽

Solar Limb ◽

Ccd Matrix

AbstractThe observational data of July 11, 1991 eclipse solar corona obtained by both electropolarimeter (EP) and CCD-matrix were processed. Using these data, the solar corona photometry was carried out. The results of EP data are compared with the ones of CCD data. It must be noted here that the CCD data give us only characteristics of the inner corona, while the EP data show the features of both the inner and middle corona up to 4R⊙. Standard flattening indexϵis evaluated from both data. The dependence of the flattening index on the distance from the solar limb is investigated. The isophotes in Na and Ca lines are plotted. Based on these data some ideas and conclusions on the type of the solar corona are presented.

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On The Radii of Ap Stars

International Astronomical Union Colloquium ◽

10.1017/s025292110008043x ◽

1976 ◽

Vol 32 ◽

pp. 49-55 ◽

Cited By ~ 1

Author(s):

F.A. Catalano ◽

G. Strazzulla

Keyword(s):

Observational Data ◽

Line Width ◽

Main Sequence ◽

Main Sequence Stars ◽

Ap Stars

SummaryFrom the analysis of the observational data of about 100 Ap stars, the radii have been computed under the assumption that Ap are main sequence stars. Radii range from 1.4 to 4.9 solar units. These values are all compatible with the Deutsch's period versus line-width relation.

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