Radio array of portable interferometric detectors (RAPID)

Lind, Frank D.; Lonsdale, Colin J.; Faulkner, A. J.; Alexander, Paul; Mattmann, Chris A.

doi:10.1109/array.2013.6731911

Cited by 5 publications

(2 citation statements)

References 20 publications

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“…Any co-located instruments capable of measuring ionospheric scintillation, such as SKA-low prototype stations, could also be used without any requirement that they be interferometrically correlated with the MWA. As well as the tiles that make up the MWA Phase II compact configuration, a Radio Array of Portable Interferometric Detectors (RAPID Lind et al 2013) or the SKA-low in a mode where each station is treated as a separate interferometer could be used in this way to measure scintillation pattern on the ground. Since this would be an independent and direct measurement of the Fresnel scale, it could be combined with the amplitude scintillation index to determine the height of the irregularities.…”

Section: Discussionmentioning

confidence: 99%

A measurement of small-scale features using ionospheric scintillation. Comparison with refractive shift measurements

Waszewski

Morgan

Jordan

2022

Publ. Astron. Soc. Aust.

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We present a study of scintillation induced by the mid-latitude ionosphere. By implementing methods currently used in Interplanetary Scintillation studies to measure amplitude scintillation at low frequencies, we have proven it is possible to use the Murchison Widefield Array to study ionospheric scintillation in the weak regime, which is sensitive to structures on scales ${\sim}300$ m at our observing frequency of 154 MHz, where the phase variance on this scale was $0.06\, \textrm{rad}^{2}$ in the most extreme case observed. Analysing over 1000 individual 2-min observations, we compared the ionospheric phase variance with that inferred with previous measurements of refractive shifts, which are most sensitive to scales almost an order of magnitude larger. The two measurements were found to be highly correlated (Pearson correlation coefficient 0.71). We observed that for an active ionosphere, the relationship between these two metrics is in line with what would be expected if the ionosphere’s structure is described by Kolmogorov turbulence between the relevant scales of 300 and 2000 m. In the most extreme ionospheric conditions, the refractive shifts were sometimes found to underestimate the small-scale variance by a factor of four or more, and it is these ionospheric conditions that could have significant effects on radio astronomy observations.

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Section: Discussionmentioning

confidence: 99%

A measurement of small-scale features using ionospheric scintillation. Comparison with refractive shift measurements

Waszewski

Morgan

Jordan

2022

Publ. Astron. Soc. Aust.

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“…As of March 2017, the project was entering the production prototype phase for many key elements of the system. Figure 3 illustrates several aspects of the RAPID system, and a full description can be found in Lind et al [2013;.…”

Section: The Instrumentmentioning

confidence: 99%

Solar imaging using low frequency arrays

2018

Planetary Radio Emissions Viii

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Low frequency imaging radio arrays such as MWA, LWA and LOFAR have been recently commissioned, and significantly more advanced and flexible arrays are planned for the near term. These powerful instruments offer new opportunities for direct solar imaging at high time and frequency resolution. They can also probe large volumes of the heliosphere simultaneously, by virtue of very large fields of view. They allow highly detailed, spatially resolved study of solar and heliospheric radio bursts, which are complemented by heliospheric propagation studies using both background astronomical radio emissions as well as the bursts themselves. In this paper, the state of the art in such wide field solar and heliospheric radio studies is summarized, including recent results from the Murchison Widefield Array (MWA). The prospects for major advances in observational capabilities in the near future are reviewed, with particular emphasis on the RAPID system developed at Haystack Observatory.

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