Other
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.3408i&link_type=abstract
American Astronomical Society Meeting 206, #34.08; Bulletin of the American Astronomical Society, Vol. 37, p.791
Other
Scientific paper
Ipatov et al. (2005, LPSC, 1266) compared the observational plots of the zodiacal light spectrum near the solar Mg Iλ 5184 absorption line (Reynolds, Madsen and Moseley, ApJ, 2004, 612, 1206-1213) with the spectrum obtained by analyzing computer simulation results of the distribution of dust particles which migrated from different sources (Ipatov et al., Annals of New York Academy of Sciences, 2004, v. 1017, 66-80). Now we compare the rotation curves, i.e., plots of velocities of Mg I line (at zero inclination) versus elongations ǎrepsilon (measured eastward from the Sun). The comparison of the observed rotation curves with the models for dust particles of different sizes (hence for different values of the ratio between the radiation pressure force and gravitational force β ) started from asteroids, comets (2P/Encke, 10P/Tempel 2, 39P/Oterma), and trans-Neptunian objects allowed to make some conclusions about sources of zodiacal dust particles. The rotation curves obtained for different scattering functions were similar for 30<ǎrepsilon<330 deg. For asteroidal dust particles and particles originating from comets 39P and 10P, rotation curves are relatively close to each other at β <0.2. For 2P particles the difference between the rotation curves obtained at different β was considerable in case of the particles produced at aphelion. For asteroidal dust particles modeled rotation curves differed from the observed ones, and for ǎrepsilon<240o modeled velocities were smaller by several km/s; for 10P and 39P particles they were smaller than those for observations at ǎrepsilon<160o and 60<ǎrepsilon<150o, respectively, but for 39P particles the difference was smaller than that for asteroidal and 10P particles. For trans-Neptunian particles the rotation curves were in agreement with the observations at ǎrepsilon<180o, but modeled velocities were smaller than observational velocities at 200<ǎrepsilon<250o. The rotation curves corresponding to particles originating from comet 2P at perihelion were close to observations at ǎrepsilon>180o. Unlike the asteroidal dust, for 2P particles the modeled velocities of MgI line were a little higher than observed velocities at 60<ǎrepsilon<180o. For particles originating from comet 2P at aphelion, the difference between the rotation curves obtained at different β could exceed 10 km/s and the observational plot was inside the region covered by plots for different β . The main conclusion of the comparison is that asteroidal dust doesn't dominate the zodiacal light and a lot of zodiacal dust particles originated from high eccentricity comets (such as comet 2P Encke).
Ipatov Sergei I.
Kutyrev Alexander S.
Madsen Greg J.
Mather John C.
Moseley Samuel Harvey
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