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Figure 4. Initial orbital elements (i.e., referred to time of nodal passage during perihelion passage of ejection), of particles integrated in Figure 3. For particles ejected after nodal passage of comet, elements are projected (integrated) back to their ecliptic crossing.

Aao relates more closely to the ejection velocity distribution, and to to the physical existence of a trail in space at later times. Near the disrupted section, a large range in all three quantities tp, r^, fl is present and so the latter two are plotted as functions of to in Figure 5. This shows the close 1833 encounter to remove particles that by the time of the next return would span about a month along the trail (i.e., there is a very clear gap of this length in the trail), and to scatter these particles over orbital periods that span ~1000 days, by the time of the next return. However, although tp spans such a large

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H-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-h

■i-1-1-1-i-1-1-1-1-1-i-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-1-t-

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