CMEless Flares: Difference between revisions
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In this Nugget we tackle this question as regards the X-ray properties, basing our study on recent lists of powerful (hence easy-to-study) major | In this Nugget we tackle this question as regards the X-ray properties, basing our study on recent lists of powerful (hence easy-to-study) major | ||
flares without CMEs. | flares without CMEs. | ||
These "confined" flares comprise about 10% of all of the X-class flares and have recognizable magnetic properties that point to the flare's <i>magnetic environment</i> as a key factor (reference [1]). | |||
== Hard X-rays == | |||
== Soft X-rays == | |||
== Conclusion == | |||
[1] [http://adsabs.harvard.edu/abs/2007ApJ...665.1428W Wang & Zhang, 2007] | |||
Revision as of 18:57, 10 August 2009
| CMEless Flares | |
|---|---|
| Number: | 107 |
| 1st Author: | Hugh Hudson |
| 2nd Author: | Säm Krucker |
| Published: | 10 August 2009 |
| Next Nugget: | NUGGET 108 |
| Previous Nugget: | Where are the flares |
Introduction
Solar flares are much more common than coronal mass ejections (CMEs). Nevertheless the standard model for a solar flare essentially requires the prior or simultaneous occurrence of a CME. How do we reconcile this discrepancy? A comparison of flare properties, for flares with and without CMEs, would seem like an obvious place to start. In this Nugget we tackle this question as regards the X-ray properties, basing our study on recent lists of powerful (hence easy-to-study) major flares without CMEs. These "confined" flares comprise about 10% of all of the X-class flares and have recognizable magnetic properties that point to the flare's magnetic environment as a key factor (reference [1]).