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Solar and Heliospheric Physics
Magnetic field fluctuations observed in the heliosheath by Voyager 1 at 114 ± 2 AU during 2010
Article first published online: 27 OCT 2012
DOI: 10.1029/2012JA017894
©2012. American Geophysical Union. All Rights Reserved.
2169-9402/asset/cover.gif?v=1&s=c95aab738f9359df0f217c15befc7ccc95c58657 "Journal of Geophysical Research: Space Physics (1978–2012)")
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How to Cite
, and (2012), Magnetic field fluctuations observed in the heliosheath by Voyager 1 at 114 ± 2 AU during 2010, J. Geophys. Res., 117, A10107, doi:10.1029/2012JA017894.
Publication History
- Issue published online: 27 OCT 2012
- Article first published online: 27 OCT 2012
- Manuscript Accepted: 16 SEP 2012
- Manuscript Revised: 27 JUL 2012
- Manuscript Received: 4 MAY 2012
- Abstract
- Article
- References
- Cited By
Keywords:
- fluctuations;
- heliosheath
[1] The radial component of the flow speed VR in the heliosheath was decreasing between 2009.0 (108.5 AU) and 2010.3, at which time it reached the “stagnation region” where VR ≈ 0 km/s from 2010.3 to at least to 2011.0 (115.7 AU). The fluctuations of the hour averages of the magnetic field B observed by Voyager 1 (V1) each day throughout 2010 were primarily compressive (longitudinal) fluctuations, along the T (average B) direction in HG coordinates. The yearly average of the daily standard deviations (SD) of the compressive component of B was 〈SDc〉 = 〈SD(BT)〉 ≈ 〈SD(B)〉 ≈ 0.015 nT. The corresponding standard deviations of the transverse components 〈SDt〉 = SD(BR) > ≈ 〈SD(BN)〉 ≈ 0.006 nT. During 2010, 〈SDc〉/〈SDt〉 > 2.6 and 〈SDc〉/〈B〉 = 0.15. The counting rate of cosmic rays >70 MeV/nuc tends to increase with increasing B and SDc, contrary to expectations.