The Variable Solar Radio Spectrum

Maxwell, A.

doi:10.1007/978-94-010-3587-3_19

Cited by 5 publications

(3 citation statements)

References 65 publications

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“…Solar radio emission is related to hot plasma and magnetic activities in the solar atmosphere (Jursa 1985). With a brightness temperature of 10 6 -10 12 K (Maxwell 1965), the Sun is one of the strongest and closest radio sources in the sky.…”

Section: Introductionmentioning

confidence: 99%

Estimation of Solar Observations with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST)

Qian¹,

Pan²,

Liu³

et al. 2022

Res. Astron. Astrophys.

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We present the estimation of the solar observation with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). For both the quite Sun and the Sun with radio bursts, when pointing directly to the Sun, the total power received by FAST would be out of the safe operational range of the signal chain, even resulting in the damage to the receiver. As a conclusion, the Sun should be kept at least 2 degrees away from the main beam during the observing at $\sim 1.25 {\ \rm GHz}$. The separation for lower frequency should be larger. For simplicity, the angular separation between the FAST beam and the Sun is suggested to be 5 degrees for observations on 200 MHz or higher bands.

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Section: Introductionmentioning

confidence: 99%

Estimation of Solar Observations with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST)

Qian¹,

Pan²,

Liu³

et al. 2022

Res. Astron. Astrophys.

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“…For observational background, a comprehensive text-book (KUNDU, 1965) and many good reviews have been available so far (KtJNDU, t963;FOKKZR, 1963;WILD, 1964;MAXWELL, 1965) and a theoretical (and observational) review on the solar bursts has been given by WILD, SMERD, and WEISS (1963). Recently, a review on the implications of solar bursts for the study of the corona was given by TAI~AKt; RA (1966).…”

Section: Introductionmentioning

confidence: 99%

Theory of solar bursts

Takakura

1967

Sol Phys

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“…The type III radio emission, which is characterized by a fast frequency drift in time from high to low frequencies (Wild, 1950), is also an impulsive phenomenon usually associated with the flash phase (Malville, 1962). The characteristics of the type III radiation have been discussed by Wild et al ), Maxwell (1965), Kundu (1965), Smith (1970a, and others. Following the initial suggestion by Wild et al (1959) andby de Jager (1960), the type III radio bursts are generally believed to be excited by streams of energetic electrons moving outwards through the solar corona (Alvarez et al, 1972).…”

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confidence: 99%

Evidence for a common origin of the electrons responsible for the impulsive X-ray and type III radio bursts

Kane

1972

Sol Phys

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Observations of impulsive solar flare X-rays > 10 keV made with the OGO-5 satellite are compared with ground based measurements of type III solar radio bursts in 10-580 MHz range. It is shown that the times of maxima of these two emissions, when detectable, agree within ~ 18 s. This maximum time difference is comparable to that between the maxima of the impulsive X-ray and impulsive microwave bursts. In view of the various observational uncertainties, it is argued that the observations are consistent with the impulsive X-ray, impulsive microwave, and type Ill radio bursts being essentially simultaneous. The observations are also consistent with 10--100 keV electron streams being responsible for the type III emission. It is estimated that the total number of electrons > 22 keV required to produce a type III burst is < 1034. The observations indicate that the non-thermal electron groups responsible for the impulsive X-ray, impulsive microwave, and type III radio bursts are accelerated simultaneously in essentially the same region of the solar atmosphere.The most characteristic non-thermal emissions during a solar flare are the impulsive hard X-ray, impulsive microwave, and type III radio bursts. In general the X-ray emission > 10 keV consists of two components, viz. impulsive and slow, the impulsive emission being the bremsstrahlung radiation from non-thermal electrons >~ 10 keV accelerated during the flash phase (Kane, 1969;Kane and Anderson, 1970). The type III radio emission, which is characterized by a fast frequency drift in time from high to low frequencies (Wild, 1950), is also an impulsive phenomenon usually associated with the flash phase (Malville, 1962). The characteristics of the type III radiation have been discussed by Wild et al. ), Maxwell (1965), Kundu (1965), Smith (1970a, and others. Following the initial suggestion by Wild et al. (1959) andby de Jager (1960), the type III radio bursts are generally believed to be excited by streams of energetic electrons moving outwards through the solar corona (Alvarez et al., 1972). De Jager (1960, 1962 noted that the kinetic energy of the electrons generating type III radio emission is similar to that of the electrons responsible for the hard X-ray emission. Moreover, the duration of a hard X-ray burst and a group of type III bursts at meter wavelengths is nearly the same. Therefore, he pointed out that a good correlation should exist between the hard X-ray and type III radio bursts. Winckler et al. (1961) and Anderson and Winckler (1962) indeed found a good correlation between the hard X-ray and type III radio bursts (two events). On the other hand, from a study of seven flares events, Kundu (1961) concluded that the correlation between these two types of emissions is weak. This led de Jager and Kundu (1963) to suggest that (i) hard X-rays and type III radio bursts are due to different jets of electrons accelerated (above the chromosphere) in different directions and (ii) simultaneous hard X-ray and Solar Physics 27 (1972) 174--181.

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The Variable Solar Radio Spectrum

Cited by 5 publications

References 65 publications

Estimation of Solar Observations with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST)

Estimation of Solar Observations with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST)

Theory of solar bursts

Evidence for a common origin of the electrons responsible for the impulsive X-ray and type III radio bursts

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