High-Resolution Studies of Ten Solar Active Regions at Wavelengths of 3-21 cm.

Swarup, G.; Kakinuma, Takakiyo; Covington, A. E.; Harvey, Gladys A.; Mullaly, R. F.; Rome, JM

doi:10.1086/147601

Cited by 54 publications

(11 citation statements)

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“…From the reported associated flare area a solid angle could be found of the order of 10-s ster subtended by the burst source, resulting in a A T b ~ 8 x 105 K. If we assume p~0.5 for a typical burst-associated S-component (Kakinuma and Swarup, 1962;, disregarding the polarization sense in (2), one finds Tb~ 3 x 106K for the S-component -in fairly good agreement with some interferometric and eclipse measurements of microwave S-components (Swarup et al, 1963;Maxwell, 1965;. It is also possible that more than one of the suggested physical conditions could be invoked at the same time, or they could be different for each specific event.…”

Section: Frequency (Ghz)supporting

confidence: 82%

Unpolarized impulsive solar bursts observed at 7 GHz

Kaufmann

1969

Sol Phys

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Section: Frequency (Ghz)supporting

confidence: 82%

Unpolarized impulsive solar bursts observed at 7 GHz

Kaufmann

1969

Sol Phys

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“…From high-resolution observation of 8 sources Swarup et al (1963) found that the average altitude of radio emission is 15 000 km above the photosphere. But Kundu (1965) mentioned emission altitudes two or three times higher for some active regions observed by Swarup.…”

Section: Datamentioning

confidence: 99%

Solar activity cycle and rotation of the corona

Mouradian

Bocchia

Botton

2002

A&A

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Abstract. In this paper we consider the dependence of the coronal rotation period on solar activity. We analyzed the 10.7 cm radio emission flux covering cycles 19 to 22. We have established a new method for studying the rotation rate: by identifying the flux pulses with the recurrence of active longitudes. We first determined the frequency domain of the rotation and then analyzed each cycle separately. The entire domain of 51.7 years was divided into 480-day sections, which were analyzed independently and then grouped into frames for each cycle in order to study the time variation of prominent frequencies (Fig. 4). Power spectra were obtained with the Maximum Entropy Method. The 10.7 cm emission rotation varies accordingly to the activity level, i.e. at the activity maxima the synodic period of rotation is about 25.4 days and at the minima it is around 30 days; it is 32 days for the quiet Sun (Table 1). Empirical relations give the ratio of maximum and minimum sidereal rotation rate with respect to sunspot number (Fig. 6). During the cycle increase phase, the average acceleration of the rotation period is 0.8• /d per year, in decreasing phase that average is only −0.5.

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“…These processes were used to explain the intensity and polarization spectrum of the slowly varying component in two-component, "core-halo" models incorporating gyroresonance absorption above sunspots and thermal bremsstrahlung in other regions (Zheleznyakov, 1962;Kakinuma and Swarup, 1962;Swarup et al, 1963;Lantos, 1968;Zlotnik, 19 6 8a, b). Although the complete expression for gyroresonant absorption is somewhat complicated (Ginzburg 1961(Ginzburg , 1967Kakinuma and Swarup, 1962;Kriiger, 1979), its basic properties can be inferred from the simplified optical depth formula which holds for quasi-longitudinal propagation with an index of refraction near unity (Zheleznyakov, 1970) 2 2n-2 T vP L H (Vth n +22 n (I + cos_) 2 sin2n-2 ,…”

Section: -3mentioning

confidence: 99%