Thickness of the Heliosheath, Return of the Pick-up Ions, and Voyager 1's Crossing the Heliopause

Details Thickness of the Heliosheath, Return of the Pick-up Ions, and Voyager 1's Crossing the Heliopause Thickness of the Heliosheath, Return of the Pick-up Ions, and Voyager 1's Crossing the Heliopause

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...718l.185h&link_type=abstract

The Astrophysical Journal Letters, Volume 718, Issue 2, pp. L185-L188 (2010).

Astronomy and Astrophysics

Astronomy

2

Acceleration Of Particles, Methods: Data Analysis, Plasmas, Shock Waves, Space Vehicles: Instruments, Sun: Heliosphere

Scientific paper

Using results of remote sensing by energetic neutral atoms from IBEX, SOHO/HSTOF, and Cassini/INCA, in situ measurements of ~40-4000 keV protons in the heliosheath (HS) from Low Energy Charged Particle on Voyager 1 and Voyager 2, and outputs from numerical modeling of the termination shock, we estimate L, the characteristic thickness of the HS in the "upwind" direction (±45° in ecliptic longitude of the Nose at λ = 255°). A simple steady-state, internally consistent model gives L = 21 ± 6 AU for Voyager 1, L = 28 ± 8 AU for Voyager 2, and L = 25 ± 8 AU assuming that the same L value is valid for both spacecraft. We recognize that this is a very coarse cut at a very dynamic region of the heliosphere; but if the lower value L = 21 AU applies, one could expect Voyager 1 to cross the heliopause as early as late 2010.

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