ISBN-10: 0875904300
ISBN-13: 9780875904306
ISBN-10: 1118666208
ISBN-13: 9781118666203
Published through the yank Geophysical Union as a part of the Geophysical Monograph Series.
Coronal mass ejections (CMEs) are the main full of life occasions within the heliosphere. in the course of sunlight cycle 23, the shut connection among CMEs and sun full of life debris (SEPs) used to be studied in a lot higher element than was once formerly attainable, together with results on area climate.
This booklet reports large observations of sun eruptions and SEPs from orbiting and ground-based structures. From SOHO and ACE to RHESSI and hint, we have now measurements of unparalleled sensitivity in which to check assumptions and refine models.
Discussion and research of:
- Coronal mass ejections and lively debris over one sunlight cycle
- Implications of sun eruptions for house climate and human house exploration
- The elemental, isotopic, and ionic cost kingdom composition of speeded up particles
- Complex interconnections between CMEs, flares, shocks, and vigorous debris will make this ebook an critical source for scientists engaged on the Sun-Earth connection, together with area physicists, magnetospheric physicists, atmospheric physicists, astrophysicists, and aeronomists.
Content:
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Additional resources for Solar Eruptions and Energetic Particles
Example text
In the simple 2-dimensional view disconnection leads to interplanetary magnetic fields completely unattached to the corona, for which solar wind signatures are rarely, if ever, seen. Crooker et al. [2002] have proposed that an interchange reconnection between open coronal fields and closed CME fields, shown in Figure 10, will prevent the addition of new magnetic flux to the interplanetary medium from CMEs. 29 The product will be small closed coronal loops and large open CME fields. , 1999], but eventually the flux rope itself must reconnect to prevent an interplanetary magnetic-flux buildup.
M. Wang, Coronal inflows and sector magnetism, Astrophys. , 562, L107, 2001. -M. Wang, Characteristics of coronal inflows, Astrophys. , 579, 874, 2002. , Evidence of magnetic reconnection in solar flares and a unified model of flares, Astrophys. , 264, 129, 1999. , and K. Shibata, Physical parameters of solar X-ray jets, Astrophys. , 542, 1100, 2000. , The relationship between prominence eruptions and coronal mass ejections, J. Atmos. Terr. , 62, 1479, 2000. , Evidence for magnetic reconnection in the high corona, Astron.
Those features were also interpreted in terms of reconnecting current sheets. Several considerations complicate the above picture of field-line disconnection in a large-scale current sheet. In the simple 2-dimensional view disconnection leads to interplanetary magnetic fields completely unattached to the corona, for which solar wind signatures are rarely, if ever, seen. Crooker et al. [2002] have proposed that an interchange reconnection between open coronal fields and closed CME fields, shown in Figure 10, will prevent the addition of new magnetic flux to the interplanetary medium from CMEs.
Solar Eruptions and Energetic Particles
by John
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