Glasgow Callisto and CMEless type II bursts

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(e-Callisto and Glasgow Callisto)
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[[File:oct21_wb.png|600px|thumb|center|alt=Light curves| Figure 2:
[[File:oct21_wb.png|600px|thumb|center|alt=Light curves| Figure 2:
CALLISTO light curve at 55MHz, and time derivative of GOES soft X-ray light curve]]
CALLISTO light curve at 55MHz, and time derivative of GOES soft X-ray light curve]]
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[[File:oct21_stretched.png|600px|thumb|center|alt=Light curves| Figure 3:
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CALLISTO spectrograph, stretched to bring out Type II emission, including cute harmonic. ]]
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== Type II bursts without CMEs? ==
== Type II bursts without CMEs? ==

Revision as of 16:31, 13 February 2015

Link title

Nugget
Number: 246
1st Author: Peter Wakeford
2nd Author: Hugh Hudson
Published: February 16, 2015
Next Nugget: TBD
Previous Nugget: [1]
List all



Contents

Introduction

In the conventional picture, a [CME] drives a coronal shock wave that produces a [type II ("slow drift")] radio burst, which then accelerates solar energetic particles [SEPs]. In an earlier Nugget we noted the development of [NOAA] active region 2192, in October 2014; this region produced a remarkable series of major flares but few CMEs and no SEPs. We were thus quite surprised to find that our Glasgow Callisto radio observatory had actually detected type II bursts from some of these flares.

e-Callisto and Glasgow Callisto

The e-Callisto project is a global development of solar radio spectrometers scattered widely around the world, organized brilliantly from Switzerland by Christian Monstein. By providing an inexpensive and easily maintained receiver, this project rather brilliantly provides full-time broad-band monitoring of solar radio bursts.

[more text and a couple of figures]

Glasgow Callisto
Figure 1: A type II solar radio burst, SOL2014-10-21T12, observed at the Glasgow Callisto site. This is a spectrogram showing the solar flux density as a function of frequency and time. The near-vertical features are type III bursts, produced by streams of fast electrons; the faint diagonal line drifting slowly to lower frequency is the type II burst. Standard interpretation would associate this with a global MHD wave driven by a CME; in this case it's probably a [blast wave] instead.
Light curves
Figure 2: CALLISTO light curve at 55MHz, and time derivative of GOES soft X-ray light curve
Light curves
Figure 3: CALLISTO spectrograph, stretched to bring out Type II emission, including cute harmonic.

Type II bursts without CMEs?

[some solar physics. Just checking I can edit the wiki]

Conclusions

Live data from the Glasgow CALLISO can be seen here, and back data can be downloaded by following the links. CALLISTO data can be analysed using IDL routines, or using the nice new Python package SunPy. [some text. Virtues of e-callisto; failure of Irish site to confirm. ]

References

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