Solar Wind Flow Through the Comet p/ Halley Bow Shock

Details Solar Wind Flow Through the Comet p/ Halley Bow Shock Solar Wind Flow Through the Comet p/ Halley Bow Shock

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...187...55c&link_type=abstract

Astronomy and Astrophysics, Vol. 187, NO. 1&2/NOV(I), P. 55, 1987

Astronomy and Astrophysics

Astrophysics

29

Scientific paper

The bow shock of a comet is formed by the interaction of three different particle populations; solar wind ions, cometary ions and electrons. We follow the behaviour of the solar wind protons through the Giotto inbound shock crossing at comet P/Halley. A foreshock boundary is seen at ˜1.4 106 km where the level of solar wind fluctuations increases substantially. The shock itself is seen some 2.5 105 km closer. It is a complex structure with high-amplitude waves in the cometary ion foot of the shock preceding a permanent drop in the solar wind speed. The width of the shock structure is ˜40,000 km. There is evidence for a further excursion back into the cometary ion foot after the initial shock crossing. The cometary ion density is inferred from the solar wind speed changes and is compared with measurements.

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