Interplanetary Scintillation of Small Diameter Radio Sources

Nature ◽  
1964 ◽  
Vol 203 (4951) ◽  
pp. 1214-1217 ◽  
Author(s):  
A. HEWISH ◽  
P. F. SCOTT ◽  
D. WILLS
Keyword(s):  
Small Diameter ◽  
Radio Sources ◽  
Interplanetary Scintillation

scholarly journals Observations of interplanetary scintillation in China

2012 ◽  
Vol 8 (S294) ◽  
pp. 487-488
Author(s):  
Li-Jia Liu ◽  
Bo Peng
Keyword(s):  
Solar Wind ◽  
Interplanetary Medium ◽  
Interplanetary Space ◽  
Solar Wind Speed ◽  
Small Diameter ◽  
Primary Source ◽  
Radio Sources ◽  
The Sun ◽  
Interplanetary Scintillation ◽  
The Earth

AbstractThe Sun affects the Earth in multiple ways. In particular, the material in interplanetary space comes from coronal expansion in the form of solar wind, which is the primary source of the interplanetary medium. Ground-based Interplanetary Scintillation (IPS) observations are an important and effective method for measuring solar wind speed and the structures of small diameter radio sources. In this paper we will discuss the IPS observations in China.

scholarly journals Intensity Distribution of Interplanetary Scintillation at 408 MHz

1975 ◽  
Vol 28 (5) ◽  
pp. 621 ◽  
Author(s):  
RG Milne
Keyword(s):  
Flux Density ◽  
Intensity Distribution ◽  
Small Diameter ◽  
Point Sources ◽  
Radio Sources ◽  
Interplanetary Scintillation ◽  
The Core ◽  
Intensity Fluctuations

It is shown that interplanetary scintillation of small-diameter radio sources at 408 MHz produces intensity fluctuations which are well fitted by a Rice-squared. distribution, better so than is usually claimed. The observed distribution can be used to estimate the proportion of flux density in the core of 'core-halo' sources without the need for calibration against known point sources.

Interplanetary Scintillation Studies at the Molonglo Radio Observatory

1972 ◽  
Vol 2 (2) ◽  
pp. 88-89
Author(s):  
R. G. Milne
Keyword(s):  
Radio Source ◽  
Radio Telescope ◽  
Interplanetary Medium ◽  
Small Diameter ◽  
Line Of Sight ◽  
Radio Sources ◽  
The Sun ◽  
Interplanetary Scintillation ◽  
Radio Observatory ◽  
Half Power

The structure of small diameter radio sources can be investigated by studying the scintillation of the source due to the interplanetary medium when the line of sight approaches the Sun. Observations of radio source scintillation are currently being undertaken with the separate arms of the 1 mile radio telescope at the Molonglo Observatory. The EW arm allows successive transit observations with three fan beams, 1′.4 EW by 4°.2 NS at 408 MHz, bandwidth 2.5 MHz. Sources transit the half-power points of each beam in 6 sec δ seconds of time (δ is the source declination). The NS arm gives eleven fan beams at neighbouring declination, 1′.5 sec Z NS by 4° EW (Z is the zenith angle). Complete transit of a NS beam takes 15 sec δ minutes.

High-Resolution Observations of Small-Diameter Radio Sources at 18-CENTIMETER Wavelength

1968 ◽  
Vol 153 ◽  
pp. 705 ◽  
Author(s):  
B. G. Clark ◽  
K. I. Kellermann ◽  
C. C. Bare ◽  
M. H. Cohen ◽  
D. L. Jauncey
Keyword(s):  
High Resolution ◽  
Small Diameter ◽  
Radio Sources

A catalog of small-diameter radio sources in the Galactic plane

1990 ◽  
Vol 74 ◽  
pp. 181 ◽  
Author(s):  
S. Zoonematkermani ◽  
D. J. Helfand ◽  
R. H. Becker ◽  
R. L. White ◽  
R. A. Perley
Keyword(s):  
Galactic Plane ◽  
Small Diameter ◽  
Radio Sources

scholarly journals Interplanetary Scintillation Power Spectra

1976 ◽  
Vol 29 (3) ◽  
pp. 201 ◽  
Author(s):  
RG Milne
Keyword(s):  
Power Spectrum ◽  
Power Law ◽  
Scattering Theory ◽  
Power Spectra ◽  
Inverse Power ◽  
Radio Sources ◽  
Interplanetary Scintillation ◽  
Inverse Power Law ◽  
Power Law Index ◽  
Strong Scattering

Power spectrum measurements of interplanetary scintillation at 408 MHz show that an inverse power law spectrum provides the best description for all scintillating radio sources. The inverse power law index is reasonably constant at ~ 2�4 for solar elongation angles 8 > 10�, and this agrees well with spacecraft observations. For 8 < 10� the index apparently decreases with decreasing 8, and this appears to be consistent with recent strong scattering theory. A Bessel analysis attempted in order to detect Fresnel structure proved unsuccessful because of noise on the power spectra.

scholarly journals 8·8 GHz Radio Observations of 12 Suggested Supernova Remnants

1973 ◽  
Vol 26 (3) ◽  
pp. 379 ◽  
Author(s):  
JR Dickel ◽  
DK Milne ◽  
AR Kerr ◽  
JG Ables
Keyword(s):  
Flux Density ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Galactic Plane ◽  
Small Diameter ◽  
Radio Sources ◽  
Radio Observations ◽  
Frequency Measurements ◽  
Thermal Spectrum

Brightness distributions and flux densities at 8�8 GHz are presented for 12 small-diameter radio sources near the galactic plane. Each of these sources has been classified at one time or another as a supernova remnant. For one source, G295� 2 - 0�6, the flux density at 8�8 GHz confirms the thermal spectrum suggested by lower frequency measurements and indicates that it is not a supernova remnant. Another source, G309� 6+ 1�7, is thought to be extragalactic.

scholarly journals Australian Journal of Physics Astrophysical Supplements

1975 ◽  
Vol 28 (3) ◽  
pp. 357
Author(s):  
FF Gardner ◽  
JB Whiteoak ◽  
D Morris
Keyword(s):  
Linear Polarization ◽  
Small Diameter ◽  
Australian Journal ◽  
Radio Sources

The results of surveys made at Parkes of linear polarization at wavelengths of 6, 11, 18 and 21 cm are presented for a total of 1121 small-diameter radio sources or source components

scholarly journals I. Observations Of Small Diameter Sources

1966 ◽  
Vol 19 (3) ◽  
pp. 441 ◽  
Keyword(s):  
Wavelength Range ◽  
Small Diameter ◽  
Short Wave ◽  
Polarization Angle ◽  
Radio Sources ◽  
Slight Variation ◽  
Fine Scale ◽  
Antenna Gain ◽  
System Noise ◽  
Made In

This paper is concerned with the observations of the polarization of small diameter radio sources made in 1963 with the Parkes 210 ft telescope over the wavelength range 11-74 cm. The sources of error in making such measurements with a single dish are discussed. At the short-wave end, the main limitation is system noise, and there is some complication from a slight variation of antenna gain with polarization angle; at long wavelengths, the limitation is the fine-scale structure of the galactic polarization in the direction of the source. The latter varies greatly across the sky.

scholarly journals IPS Observations at STELAB for the Fruitful Coming Decade

1996 ◽  
Vol 154 ◽  
pp. 247-250
Author(s):  
K. Asai ◽  
Y. Ishida ◽  
M. Kojima ◽  
K. Maruyama ◽  
H. Misawa ◽  
...  
Keyword(s):  
Solar Wind ◽  
Temporal Resolution ◽  
Observation System ◽  
Present System ◽  
Radio Sources ◽  
Interplanetary Scintillation ◽  
Wind Measurements ◽  
Insufficient Sensitivity

AbstractWe have been carrying out solar wind measurements using the interplanetary scintillation (IPS) method. Our IPS observation system is operated at a frequency of 327MHz and consists of four stations located at Toyokawa, Fuji, Sugadaira and Kiso. The present system, however, has insufficient sensitivity to measure enough IPS sources for observing the solar wind with adequate spatial and temporal resolution. Therefore we have been excuting the upgrade project since 1994 in order to observe a larger number of compact radio sources. The Fuji system has been improved successfully and has achieved sensitivity by a factor over five compared with the previous system. The upgrade project is now in progress for the Toyokawa and Sugadaira station.

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