slide1 ==> 7.1: Comet Hyakutake showed a bright coma (lower left) and long gas tail (upwards from coma) in March 1996 (D. Dierick).
slide2 ==> 7.2: Changing line of sight towards a stationary comet as the Earth turns, not seen by Brahe.
slide3 ==> 7.3: Relative to the ecliptic, Comet P/Halley orbits not far out of the plane but retrograde.
slide4 ==> 7.4: Spectrum of the coma of Comet P/Tuttle (1980 XIII). Bright wavelengths are colours scattered by coma molecules.
slide5 ==> 7.5: Rocket effect felt by a comet nucleus from outgassing for non-rotating (top) and rotating nuclei.
slide6 ==> 7.6: Comet Hale-Bopp showed both a gas tail (left) and a dust tail (right) in 1996 (D. Dierick).
slide7 ==> 7.7: Dust grains ejected from a comet nucleus follow less curved orbits (light lines) because of radiation.
slide8 ==> 7.8: Cartoon of the interaction between outflowing cometary gas and the solar wind.
slide9 ==> 7.9: Nucleus of Comet P/Halley (dark blob) from about 600 km away; bright region is due to gas outflow (ESA).
slide10 ==> 7.10: Distribution of initial orbit sizes for long-period comets; most have a around 10 000 km.
slide11 ==> 7.11: The 20 pieces of Comet Shoemaker-Levy approaching Jupiter before impact (NASA).
slide12 ==> 7.12: Dust clouds on Jupiter produced by impacts of pieces of Comet Shoemaker-Levy 9 (NASA).
slide13 ==> 7.13: Gas sublimation rate from various ices as a function of distance from the Sun.