Long Baseline Interferometer Observations at 408 and 448 MHz--II: The Interpretation of the Observations

Clarke, R. W.; Broten, N. W.; Legg, T. H.; Locke, John; Yen, J. L.

doi:10.1093/mnras/146.4.381

Cited by 32 publications

(6 citation statements)

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“…The spectrum ofthis component is shown in figure 6. Assuming that this is the same component that Clarke et al (1969) observed at 448 MHz, its spectrum is practically flat in the 100---500 MHz range. Remnants of the complex structure observed at 408 MHz by Anderson and Donaldson (1967) may make a simple interpretation of our observation impossible.…”

Section: D) 3c 273supporting

confidence: 55%

A new wideband, fully steerable, decametric array at Clark Lake

Erickson

Fisher

1974

Radio Science

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A new, fully steerable, decametric array for radio astronomy is under construction at the Clark Lake Radio Observatory near Borrego Springs, California. This array will be a “T” of 720 conical spiral antennas (teepee‐shaped antennas, hence the array is called the TPT), 3.0 by 1.8 km capable of operating between 15 and 125 MHz. Both its operating frequency and beam position will be adjustable in less than one msec, and the TPT will provide a 49‐element picture around the central beam position for extended‐source observations. Considerable experience has been gained in the operation of completed portions of the array, and successful operation of the final array is assured. This paper describes the results of the tests which have been conducted with the conical spirals and outlines the planned electronics.

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Section: D) 3c 273supporting

confidence: 55%

A new wideband, fully steerable, decametric array at Clark Lake

Erickson

Fisher

1974

Radio Science

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“…Very compact radio sources are extremely rare and it has been established at a number of frequencies, using both IPS (Bourgois 1969;Bourgois & Creynet 1972;Milne 1976) and long baseline interferometry (Clark et al 1968;Clarke et al 1969), that the radio source 1148-001 has an angular diameter of ≈10 milliarcsecond (mas) at meter wavelengths. Thus, the source 1148-001 can be treated as a nearly ideal point source at 327 MHz, with almost all of its flux contained in a compact scintillating component with very little flux outside this compact component (Swarup 1977;Venugopal et al 1985).…”

Section: Discussionmentioning

confidence: 99%

A Study of Density Modulation Index in the Inner Heliospheric Solar Wind During Solar Cycle 23

Janardhan

Ingale

Subramanian

et al. 2014

ApJ

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The ratio of the rms electron density fluctuations to the background density in the solar wind (density modulation index, N ≡ ΔN/N) is of vital importance for understanding several problems in heliospheric physics related to solar wind turbulence. In this paper, we have investigated the behavior of N in the inner heliosphere from 0.26 to 0.82 AU. The density fluctuations ΔN have been deduced using extensive ground-based observations of interplanetary scintillation at 327 MHz, which probe spatial scales of a few hundred kilometers. The background densities (N) have been derived using near-Earth observations from the Advanced Composition Explorer. Our analysis reveals that 0.001 N 0.02 and does not vary appreciably with heliocentric distance. We also find that N declines by 8% from 1998 to 2008. We discuss the impact of these findings on problems ranging from our understanding of Forbush decreases to the behavior of the solar wind dynamic pressure over the recent peculiar solar minimum at the end of cycle 23.

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“…The early VLBI observations confirmed the small angular dimensions of quasars and AGN predicted from their radio spectra and time variability and revealed their complex multi-component structure (Broten et al 1969, Clarke et al 1969. In particular, the 3.8-cm (7.8 GHz) observations of 3C 279 by Knight et al (1971) showed a particularly well-defined double source with a component separation of 0.00155 ± 00005 arcsec.…”

Section: Early Vlbi Systemsmentioning

confidence: 52%

The Development of High-Resolution Imaging in Radio Astronomy

Kellermann

Moran

2001

Annu. Rev. Astron. Astrophys.

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Since the first radio astronomy observations in the 1930s, the angular resolution of radio telescopes has improved from tens of degrees to better than one thousandth of a second of arc. This advancement has been the result of technological innovations such as stable, sensitive, short-wavelength radio receivers, digital correlators, atomic clocks, and high-speed tape recorders, as well as the development of sophisticated image processing algorithms implemented on inexpensive, fast, digital computers.

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Long Baseline Interferometer Observations at 408 and 448 MHz--II: The Interpretation of the Observations

Cited by 32 publications

References 0 publications

A new wideband, fully steerable, decametric array at Clark Lake

A new wideband, fully steerable, decametric array at Clark Lake

A Study of Density Modulation Index in the Inner Heliospheric Solar Wind During Solar Cycle 23

The Development of High-Resolution Imaging in Radio Astronomy

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