Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh44b..06r&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH44B-06
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles
Scientific paper
A constellation of spacecraft located between 0.4 and 1AU currently provides in-situ measurements of the solar wind (STEREO, ACE, Wind, Venus Express, Messenger). These measurements are complemented with unprecedented remote-sensing observations of the Sun and the solar wind from the photosphere to 1AU (SDO, STEREO, SMEI). They permit accurate and comprehensive monitoring of the evolution of Coronal Mass Ejections (CMEs) and the background solar wind from the Sun to 1AU. We can now track the formation and longitudinal/latitudinal structure of Corotating Interaction Regions (CIRs) as high-speed streams from coronal holes sweep up the small (blobs) and large (CMEs) disturbances that are continually released in the slow solar wind. These combined white-light and in-situ observations have provided clues on the nature and likely origin of one source of variability of the slow solar wind. We can now also observe the formation of coronal and heliospheric shocks in extreme ultraviolet light and in white-light images, track their evolution in the interplanetary medium and, by combining these observations with numerical models and in-situ measurements, derive the expected shock properties (geometry, compression ratio,...) in the lower and upper corona. We can now compare/interpret the timing and spectral properties of solar energetic particle events in terms of (inferred) basic shock parameters with more confidence. Despite all these major advances, many puzzles still remain unanswered. Are the small-scale transients released in the slow solar wind signatures of the acceleration mechanism of that wind? Or are their origins independent of the acceleration process of the slow solar wind? What are the seed populations for shock-accelerated particles and the injection mechanism? To answer these fundamental questions, a new constellation of missions armed with exceptional instrumentation will be launched over the next decade. They will return to the inner heliosphere and enter yet unexplored regions of the solar atmosphere well inside 20 solar radii. We will argue that, based on the instrumental design and orbital characteristics of these future missions and especially the synergy between these missions, they will provide the critical information necessary to discriminate between the various theories of solar wind acceleration and energetic particle acceleration.
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