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8. 8 Boundary Layer Structure and Detached Plasma 305 8. 8. 1
Background 305 8. 8. 2 Structure inside the boundary layer 306 8.
8. 3 Observation of detached plasma 308 8. 8. 4 Summary 309 8. 9
Summary and Conclusions 310 References 312 9. CLUSTER AT THE
MAGNETOSPHERIC CUSPS 321 9. 1 Introduction 321 9. 1. 1 Previous
work 323 9. 1. 2 How Cluster investigates the cusp 325 9. 2 The
High-Altitude Cusp 326 9. 2. 1 March 17, 2001 328 9. 2. 2 February
4, 2001 332 9. 2. 3 February 13, 2001 337 9. 2. 4 Statistical
survey 340 9. 2. 5 Waves and turbulence 343 9. 3 The Mid-Altitude
Cusp 352 9. 3. 1 Structure: Case study 352 9. 3. 2 Structure:
Statistical survey 354 9. 3. 3 Ionospheric ions 354 9. 3. 4
Mid-altitude signatures of the LLBL 357 9. 4 Discussion 359
References 360 10. MAGNETOPAUSE PROCESSES 367 10. 1 Magnetopause
Reconnection 368 10. 1. 1 Intermittent vs. quasi-steady
reconnection 368 10. 1. 2 Component vs. anti-parallel reconnection
382 10. 1. 3 Tailward-of-the-cusp reconnection 385 10. 1. 4
Quantitative tests of reconnection occurrence 388 10. 1. 5 Summary
391 10. 2 Kelvin-Helmholtz Instability at the Flank Magnetopause
391 10. 3 Microphysics of Magnetopause Processes 396 10. 3. 1
Collisionless generalised Ohm's law 397 10. 3. 2 Ion di?usion
region observations 398 10. 3. 3 High-frequency waves 402 10. 3. 4
Lower-hybrid waves 405 10. 3.
When the stream of plasma emitted from the Sun (the solar wind)
encounters Earth's magnetic field, it slows down and flows around
it, leaving behind a cavity, the magnetosphere. The magnetopause is
the surface that separates the solar wind on the outside from the
Earth's magnetic field on the inside. Because the solar wind moves
at supersonic speed, a bow shock must form ahead of the
magnetopause that acts to slow the solar wind to subsonic speeds.
Magnetopause, bow shock and their environs are rich in exciting
processes in collisionless plasmas, such as shock formation,
magnetic reconnection, particle acceleration and wave-particle
interactions. They are interesting in their own right, as part of
Earth's environment, but also because they are prototypes of
similar structures and phenomena that are ubiquitous in the
universe, having the unique advantage that they are accessible to
in situ measurements. The boundaries of the magnetosphere have been
the target of direct in-situ measurements since the beginning of
the space age. But because they are constantly moving, changing
their orientation, and undergoing evolution, the interpretation of
single-spacecraft measurements has been plagued by the fundamental
inability of a single observer to unambiguously distinguish spatial
from temporal changes. The boundaries are thus a prime target for
the study by a closely spaced fleet of spacecraft. Thus the Cluster
mission, with its four spacecraft in a three-dimensional
configuration at variable separation distances, represents a giant
step forward. This 20th volume of the ISSI Space Science Series
represents the first synthesis of the exciting new results obtained
in the first few years of the Cluster mission.
Dawn-Dusk Asymmetries in Planetary Plasma Environments Dawn-dusk
asymmetries are ubiquitous features of the plasma environment of
many of the planets in our solar system. They occur when a
particular process or feature is more pronounced at one side of a
planet than the other. For example, recent observations indicate
that Earth's magnetopause is thicker at dawn than at dusk.
Likewise, auroral breakups at Earth are more likely to occur in the
pre-midnight than post-midnight sectors. Increasing availability of
remotely sensed and in situ measurements of planetary ionospheres,
magnetospheres and their interfaces to the solar wind have revealed
significant and persistent dawn-dusk asymmetries. As yet there is
no consensus regarding the source of many of these asymmetries, nor
the physical mechanisms by which they are produced and maintained.
Volume highlights include: * A comprehensive and updated overview
of current knowledge about dawn-dusk asymmetries in the plasma
environments of planets in our solar system and the mechanisms
behind them * Valuable contributions from internationally
recognized experts, covering both observations, simulations and
theories discussing all important aspects of dawn-dusk asymmetries
* Space weather effects are caused by processes in space, mainly
the magnetotail, and can be highly localized on ground. Knowing
where the source, i.e., where dawn-dusk location is will allow for
a better prediction of where the effects on ground will be most
pronounced Covering both observational and theoretical aspects of
dawn dusk asymmetries, Dawn--Dusk Asymmetries in Planetary Plasma
Environments will be a valuable resource for academic researchers
in space physics, planetary science, astrophysics, physics,
geophysics and earth science.
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