Computer Simulations of Spectrum of the Zodiacal Light

Type Conference Paper
Names Sergei I. Ipatov, A. S. Kutyrev, G. J. Madsen, J. C. Mather, H. Moseley, R. J. Reynolds
Conference Name Bulletin of the American Astronomical Society
Volume 38
Pages 558
Date September 1, 2006
URL http://adsabs.harvard.edu/abs/2006DPS....38.4102I
Library Catalog NASA ADS
Abstract Our studies of velocity and width of Mg I line were based on the distributions of positions and velocities of migrating dust particles. These distributions were obtained in our integrations of the orbital evolution of particles started from different small bodies (asteroids, comets, trans-Neptunian objects) [Annals of the New York Acad. of Sci., 2004, 1017, 66-80; Advances in Space Research, 2006, 37, 126-137]. Comparison of our models with the WHAM observations of velocities of zodiacal dust particles and the mean width of Mg I line made by Reynolds et al. (ApJ, 2004, 612, 1206-1213) shows that only asteroidal dust particles cannot explain these observations, and particles produced by comets, including high-eccentricity comets (such as Comet Encke and long-period comets), are needed for such explanation. The values of the exponent in the power law of the distribution of particles with the distance R from the Sun at R about 1 AU were smaller for asteroidal particles than those for the measurements of micrometeoroid flux made by Helios 1 and Pioneer 10. The fraction of particles started from Encke-type comets is not large (probably, less than 10-15\%) in order to fit the observational distributions of particles over their distances from the Sun. Greater velocity amplitudes of velocity - elongation curves at elongation between 90 and 270 deg usually correspond to greater mean eccentricities of particles at distance R about 1-3 AU. For the same mean eccentricities, velocity - elongation plots depend also on the distributions of particles over their eccentricities. The mean eccentricity of zodiacal dust particles that better fit the WHAM observations is estimated to be about 0.5. Results of our studies were presented in [LPSC, 2006, #1471], and a wider paper will be submitted to AJ this summer and will be put on astro-ph.
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