Models of the Ejection of Material from Comet Tempel 1 Caused by the Deep Impact Experiment

Details Models of the Ejection of Material from Comet Tempel 1 Caused by the Deep Impact Experiment Models of the Ejection of Material from Comet Tempel 1 Caused by the Deep Impact Experiment

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.2006i&link_type=abstract

American Astronomical Society, DPS meeting #41, #20.06

Astronomy and Astrophysics

Astronomy

Scientific paper

Ejection of material from Comet Tempel 1 was studied based on analysis of the images made by the Deep Impact cameras. Our studies presented in [1-2] were based on very simple calculations. Then we started to complicate our model of ejection. In the current model, the velocity of ejection is considered to be proportional to the time te of ejection in the power of parameter α. For each interval of te corresponding to successive images, based on the distances from the place of ejection to the levels of brightness (the same brightness for different images) close to the place of ejection, we find the relative amount dm of ejected material. Using also the distances to the levels of smaller brightness, we find the value of α that better fits the observations. As a result, we obtain the dependences of dm and α on te. The results are mainly in accordance with the studies presented in [1-2]. The contribution of the triggered outburst to the brightness of the cloud could be considerable, but its contribution to the ejected mass could be relatively small. At the time te 10 s corresponding to a local maximum of ejection rate, the direction from the place of ejection to the brightest pixel quickly changed by 50 deg, a considerable excessive ejection (rays of ejected material) to a few directions began, and typical projections of velocities onto the plane perpendicular to the line of sight were 100-200 m/s. At this time, ejection of more icy material could begin. Evaporation and sublimation of this ice could increase velocities of dust. The work was supported by NASA DDAP grant NNX08AG25G.
[1] LPSC XL, 2009, 1022. [2] http://arxiv.org/abs/0810.1294.

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