Radio-Frequency Energy from the Sun

Pawsey, J. L.; Payne-Scott, Ruby; McCready, L. L.

doi:10.1038/157158a0

Cited by 91 publications

(40 citation statements)

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“…Since the Dover Heights sea-cliff interferometer observations of Pawsey, Payne-Scott & McCready (1946) and Mc-Cready, Pawsey & Payne-Scott (1947), it has been known that the most intense solar radio emission comes from sunspots, and subsequent investigations have shown that this is also the case for other main-sequence dwarf stars. These radio emissions can be non-thermal, arising from gyrosynchrotron emission, or thermal.…”

Section: Introductionmentioning

confidence: 99%

Exoplanet transits with next-generation radio telescopes

Pope

Withers

Callingham

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Nearly everything we know about extrasolar planets to date comes from optical astronomy. While exoplanetary aurorae are predicted to be bright at low radio frequencies (< 1 GHz), we consider the effect of an exoplanet transit on radio emission from the host star. As radio emission from solar-like stars is concentrated in active regions, a planet occulting a starspot can cause a disproportionately deep transit which should be detectable with major radio arrays currently under development, such as the Square Kilometre Array (SKA). We calculate the radiometric sensitivity of the SKA stages and components, finding that SKA2-Mid can expect to detect transits around the very nearest solar-like stars and many cool dwarfs. The shape of this radiometric light curve will be affected by scintillation and lensing from the planet's magnetosphere and thereby encode magnetospheric parameters. Furthermore, these transits will also probe the distribution of stellar activity across a star's surface, and will help scrub out contamination from stellar activity on exoplanet transmission spectra and radial velocity spectra. This radio window on exoplanets and their host stars is therefore a valuable complement to existing optical tools.1 In the remainder of this paper, for simplicity, we will refer to a planet's extended plasma environment as its magnetosphere, even if it might properly be referred to as its exosphere or thermosphere. The distinctions in a stratified atmosphere are not important in the simplified models we will be using.

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Section: Introductionmentioning

confidence: 99%

Exoplanet transits with next-generation radio telescopes

Pope

Withers

Callingham

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Around the same time, Pawsey, Bolton and Stanley in Australia placed a radio antenna on top of a cliff and measured the interference pattern between the direct beam from a rising source and the beam reflected by the ocean surfacethis is essentially a Lloyd's mirror arrangement [36] (Table 1). This work was largely motivated by the desire to study the radio emission from the Sun, but it also resulted in the identification of the strong sources Tau A, Vir A, and Cen A with the Crab Nebula, M 87, and NGC 5128, respectively.…”

Section: Radio Interferometry In the 1950smentioning

confidence: 99%

The development of astronomical interferometry

Quirrenbach¹

2009

Exp Astron

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Astronomical interferometry was pioneered by Fizeau and Michelson in the 19 th century. In the 1920s, the first stellar diameters were measured. The development of radio interferometry began in the 1950s, and led to the construction of powerful synthesis arrays operating at cm, mm, and sub-mm wavelengths. Modern computer and control technology has enabled the interferometric combination of light from separate telescopes also in the visible and infrared regimes. Imaging with milliarcsecond resolution and astrometry with microarcsecond precision have thus become reality.

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“…Pioneering research led by Pawsey and Ruby Payne-Scott showed that strong variable solar radiation bursts originated near sunspots, causing disruptions to radio communications on Earth (Pawsey et al 1946). At this time and in the foreseeable future, Australia became an international leader in this completely new field.…”

Section: The Beginning Of Radio Astronomymentioning

confidence: 99%