The Magnetic Field Structure in the Heliosheath

Details The Magnetic Field Structure in the Heliosheath The Magnetic Field Structure in the Heliosheath

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...631l.163j&link_type=abstract

The Astrophysical Journal, Volume 631, Issue 2, pp. L163-L165.

Astronomy and Astrophysics

Astronomy

20

Interplanetary Medium, Shock Waves

Scientific paper

The magnetic field observed in a fluctuating, dynamical heliosheath will differ considerably from that in a static heliosheath. In particular, the time between current-sheet crossings (sectors) is quite sensitive to the radial speed of the solar wind termination shock. If an inwardly moving termination shock moves past an observer on a slowly moving spacecraft, the time between current-sheet crossings in the heliosheath becomes larger, and can become very large, for reasonably expected inward shock speeds. This effect may help to explain recent observations of the magnetic field from the Voyager 1 spacecraft, where, in the heliosheath, the magnetic field has remained directed outward from the Sun for several months.

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