Titlebook

巧思

übersichtsuntersuchung des K?rperstammes those sampled by Vega and Sakigake, it is important to compare observations from the three missions that carried dedicated wave instruments. Here we summarize ICE plasma wave measurements associated with both comet encounters and relate the very high sensitivity ICE observations to corresponding measurements from the other Halley spacecraft.

SAGE

New information on comet P/Halley as depicted by Giotto di Bondone and other Western artistsley (Olson, 1979), a great deal of new information has come to light. We present a synopsis of the textual, visual, and astronomical evidence to support the theory that when Giotto painted his comet in the Scrovegni Chapel he was reflecting his viewing of Comet Halley in 1301.

土坯

Waves in the magnetic field and solar wind flow outside the bow shock at comet P/Halleypropagation for these waves to be separated. The magnetic component is predominantly transverse to the magnetic field and linearly polarised. The flow vector also has a substantial amount of power parallel to the magnetic field. A examination of the pressure variations shows that slow magnetosonic waves are more common than the fast mode.

Provenance

Plasma flow in the cometosheath of P/Halley during the encounter of Suiseiby the cooling effect accompanying with the charge exchange process as well as with the mass addition of cold pickup ions. On the contrary, the observed temperature of alpha particles stayed almost constant throughout the cometosheath. This is because that there is no effective cooling process for alpha particles within the cometosheath.

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ciliary-body

The pick-up of cometary protons by the solar windoidal trajectories such that they were nonuniformly distributed over a spherical shell in velocity space. The shell radius (relative to its expected radius) and thickness increased as the bow shock was approached. Down-stream of the shock, the cometary protons could not be distinguished from the heated solar wind protons.