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Learning about coronal heating from solar wind observationsa)
a)Paper RI2 4, Bull. Am. Phys. Soc. 49, 327 (2004).
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10.1063/1.1863192
/content/aip/journal/pop/12/5/10.1063/1.1863192
http://aip.metastore.ingenta.com/content/aip/journal/pop/12/5/10.1063/1.1863192
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Figures

Image of FIG. 1.
FIG. 1.

Linear theory results at : The (a) damping rates and (b) alpha resonance factors of Alfvén-cyclotron fluctuations in a homogeneous, collisionless electron-proton-alpha plasma as functions of the parallel wavenumber. The four curves of various dashes or dots correspond to successively increasing values of the alpha/proton relative speed; from left to right , 0, 0.10, and 0.50. The solid curve represents results for an electron-proton plasma with . Here , , , and .

Image of FIG. 2.
FIG. 2.

Second-order theory results at : The dimensionless scattering rates of the protons (solid line) and the alphas (dashed line). Here , , , and . These scattering rates are also functions of the choice of magnetic power spectrum and dissipation wavenumber chosen for the calculation; here corresponds to .

Image of FIG. 3.
FIG. 3.

ACE observations: ion anisotropies observed during January 2002 as functions of . The data have been reduced as described in the text. The dashed lines indicate least-squares best fits to the data which are: (a) and (b) .

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2005-04-07
2014-04-17
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Learning about coronal heating from solar wind observationsa)
http://aip.metastore.ingenta.com/content/aip/journal/pop/12/5/10.1063/1.1863192
10.1063/1.1863192
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