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An indication of the existence of a solar wind strahl at 10AU

Research output: Contribution to Journal/Magazine › Journal article › peer-review

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An indication of the existence of a solar wind strahl at 10AU. / Walsh, A. P.; Arridge, C. S.; Masters, A. et al.
In: Geophysical Research Letters, Vol. 40, No. 11, 16.06.2013, p. 2495-2499.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Walsh, AP, Arridge, CS, Masters, A, Lewis, GR, Fazakerley, AN, Jones, GH, Owen, CJ & Coates, AJ 2013, 'An indication of the existence of a solar wind strahl at 10AU', Geophysical Research Letters, vol. 40, no. 11, pp. 2495-2499. https://doi.org/10.1002/grl.50529

APA

Walsh, A. P., Arridge, C. S., Masters, A., Lewis, G. R., Fazakerley, A. N., Jones, G. H., Owen, C. J., & Coates, A. J. (2013). An indication of the existence of a solar wind strahl at 10AU. Geophysical Research Letters, 40(11), 2495-2499. https://doi.org/10.1002/grl.50529

Vancouver

Walsh AP, Arridge CS, Masters A, Lewis GR, Fazakerley AN, Jones GH et al. An indication of the existence of a solar wind strahl at 10AU. Geophysical Research Letters. 2013 Jun 16;40(11):2495-2499. doi: 10.1002/grl.50529

Author

Walsh, A. P. ; Arridge, C. S. ; Masters, A. et al. / An indication of the existence of a solar wind strahl at 10AU. In: Geophysical Research Letters. 2013 ; Vol. 40, No. 11. pp. 2495-2499.

Bibtex

@article{d0cd8710309c45f1a8fa7568dba33a01,
title = "An indication of the existence of a solar wind strahl at 10AU",
abstract = "The solar wind electron distribution is observed near and within 1AU to consist of three components: a thermal core, a suprathermal halo, and a suprathermal strahl. The former two components are isotropic, while the strahl is field aligned and flows outward along the interplanetary magnetic field. The evolution of solar wind electrons with heliocentric distance is poorly understood; although the halo is thought to be formed through pitch angle (PA) scattering of the strahl, the responsible physical process has not been conclusively identified. Measurements of solar wind electrons throughout the heliosphere are required to solve this problem. We present the first observations of the suprathermal components of the solar wind electron distribution made outside 5AU. We find indications of a strahl component narrower than that predicted by extrapolating observations and models of electrons in the inner heliosphere, suggesting the rate of electron pitch angle scattering in the solar wind can decrease with increasing heliocentric distance.",
keywords = "solar wind, electrons, strahl, heliosphere, VELOCITY DISTRIBUTION-FUNCTIONS, HELIOS PLASMA-EXPERIMENT, ELECTRONS, HALO, SPECTROMETER, WAVES, AU",
author = "Walsh, {A. P.} and Arridge, {C. S.} and A. Masters and Lewis, {Gethyn. R.} and Fazakerley, {A. N.} and Jones, {Geraint. H.} and Owen, {C. J.} and Coates, {A. J.}",
note = "{\textcopyright}2013. American Geophysical Union",
year = "2013",
month = jun,
day = "16",
doi = "10.1002/grl.50529",
language = "English",
volume = "40",
pages = "2495--2499",
journal = "Geophysical Research Letters",
issn = "0094-8276",
publisher = "John Wiley & Sons, Ltd",
number = "11",

}

RIS

TY - JOUR

T1 - An indication of the existence of a solar wind strahl at 10AU

AU - Walsh, A. P.

AU - Arridge, C. S.

AU - Masters, A.

AU - Lewis, Gethyn. R.

AU - Fazakerley, A. N.

AU - Jones, Geraint. H.

AU - Owen, C. J.

AU - Coates, A. J.

N1 - ©2013. American Geophysical Union

PY - 2013/6/16

Y1 - 2013/6/16

N2 - The solar wind electron distribution is observed near and within 1AU to consist of three components: a thermal core, a suprathermal halo, and a suprathermal strahl. The former two components are isotropic, while the strahl is field aligned and flows outward along the interplanetary magnetic field. The evolution of solar wind electrons with heliocentric distance is poorly understood; although the halo is thought to be formed through pitch angle (PA) scattering of the strahl, the responsible physical process has not been conclusively identified. Measurements of solar wind electrons throughout the heliosphere are required to solve this problem. We present the first observations of the suprathermal components of the solar wind electron distribution made outside 5AU. We find indications of a strahl component narrower than that predicted by extrapolating observations and models of electrons in the inner heliosphere, suggesting the rate of electron pitch angle scattering in the solar wind can decrease with increasing heliocentric distance.

AB - The solar wind electron distribution is observed near and within 1AU to consist of three components: a thermal core, a suprathermal halo, and a suprathermal strahl. The former two components are isotropic, while the strahl is field aligned and flows outward along the interplanetary magnetic field. The evolution of solar wind electrons with heliocentric distance is poorly understood; although the halo is thought to be formed through pitch angle (PA) scattering of the strahl, the responsible physical process has not been conclusively identified. Measurements of solar wind electrons throughout the heliosphere are required to solve this problem. We present the first observations of the suprathermal components of the solar wind electron distribution made outside 5AU. We find indications of a strahl component narrower than that predicted by extrapolating observations and models of electrons in the inner heliosphere, suggesting the rate of electron pitch angle scattering in the solar wind can decrease with increasing heliocentric distance.

KW - solar wind

KW - electrons

KW - strahl

KW - heliosphere

KW - VELOCITY DISTRIBUTION-FUNCTIONS

KW - HELIOS PLASMA-EXPERIMENT

KW - ELECTRONS

KW - HALO

KW - SPECTROMETER

KW - WAVES

KW - AU

U2 - 10.1002/grl.50529

DO - 10.1002/grl.50529

M3 - Journal article

VL - 40

SP - 2495

EP - 2499

JO - Geophysical Research Letters

JF - Geophysical Research Letters

SN - 0094-8276

IS - 11

ER -