Type II solar radio events observed in the interplanetary medium

Cane, H. V.; Stone, R. G.; Fainberg, J.; Steinberg, J. L.; Hoang, S.

doi:10.1007/bf00151153

Cited by 99 publications

(51 citation statements)

References 10 publications

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“…It is generally accepted that type II bursts are caused by shock waves in the corona and CME-driven shocks in the solar wind. The energetic electron beams accelerated at the shock front excite Langmuir waves which through non-linear wave-wave interactions, couple into freely propagating radio emissions at the local electron plasma frequency (f pe ) or its harmonic (Cane et al, 1982;Kahler, Cliver, and Cane, 1989;Bale et al, 1999).…”

Section: Introductionmentioning

confidence: 99%

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

et al. 2014

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On 13 March 2010 an unusually long duration event was observed by radio spectrographs onboard the STEREO-B and Wind spacecraft. The event started at about 13:00 UT and ended at approximately 06:00 UT on 14 March. The event presents itself as slow drifting, quasi-continuous emission in a very narrow frequency interval, with an apparent frequency drift from about 625 kHz to approximately 425 kHz. Using the Leblanc, Dulk, and Bougeret (1998) interplanetary density model we determined that the drift velocities of the radio source are ≈33 km s −1 and ≈52 km s −1 for 0.2 and 0.5 times the densities of Leblanc model, respectively with a normalization density of 7.2 cm −3 at 1AU and assuming harmonic emission. A joint analysis of the radio direction finding data, coronograph white-light observations and modeling revealed that the radio sources appear to be localized in regions of interaction with relatively high density and slow solar wind speed.

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Section: Introductionmentioning

confidence: 99%

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

et al. 2014

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“…Bougeret 1985, and references therein; see also Lengyel-Frey & Stone 1989). Although the band-splitting was recognized in some events (Boischot et al 1980;Cane et al 1982) it was never considered as an important feature of UC/IP t-II bursts.…”

Section: Introductionmentioning

confidence: 99%

Band-splitting of coronal and interplanetary type II bursts

Vršnak¹,

Auraß²,

Magdalenić³

et al. 2001

A&A

141

113

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Abstract. Patterns analogous to the band-splitting of metric type II bursts are found in a number of type II bursts observed in the dekameter-kilometer wavelength range. A similarity of morphological and frequency-time characteristics of two emission components are indicative of a common source. Relative frequency splits span in the range ∆f/f = 0.05−0.6. At radial distances between 2 and 4 R only small splits around 0.1 can be found. In the interplanetary space the relative split on average increases with the radial distance, whereas the inferred shock velocity decreases. In three events extrapolations of the split components point to the base and the peak of the jump in the local plasma frequency caused by the associated shock passage at 1 AU. This is suggestive of the plasma radiation from the regions upstream and downstream of the shock. Adopting this interpretation, one finds that the drop of ∆f/f at 2-4 R is congruent with the Alfvén velocity maximum expected there. The split increase and the velocity decrease at larger distances can be explained as a consequence of declining Alfvén speed in the interplanetary space.

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“…A shock often forms ahead of the CME as it propagates outward and radio emission, at fpe and/or 2fpe, is thought to be generated by shock-accelerated electrons near this shock front [Cane et al, 1981] [Cane et al, 1982]. Reiner et al [1998b] suggested that some sporadic type II emissions correspond to emissions at various sites along the shock front.…”

Section: Introductionmentioning

confidence: 99%

The source region of an interplanetary type II radio burst

Bale¹,

Reiner²,

Bougeret³

et al. 1999

Geophysical Research Letters

205

203

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Abstract.We present the first observation of the source region of an interplanetary type II radio burst, using instruments on the Wind spacecraft. Type II radio emission tracks the motion of a CME-driven interplanetary (IF) shock which encounters the spacecraft. connection times to the shock, we infer the existence and characteristic size of large scale structure on the shock front. The type II radio emission seems to be generated in a small bay upstream of the shock, and this may account for some splitting structure observed in the frequency spectrum of many type II bursts.

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Type II solar radio events observed in the interplanetary medium

Cited by 99 publications

References 10 publications

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

Band-splitting of coronal and interplanetary type II bursts

The source region of an interplanetary type II radio burst

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