Radiation pressure forces on circumstellar dust particles

Details Radiation pressure forces on circumstellar dust particles Radiation pressure forces on circumstellar dust particles

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998exdu.work..283m&link_type=abstract

Exozodiacal Dust Workshop, p. 283

Computer Science

1

Radiation Pressure, Cosmic Dust, Stellar Envelopes, Microparticles, Porosity, Carbon, Silicates, Black Body Radiation, Size Distribution

Scientific paper

We present model calculations of the radiation pressure forces acting on dust particles around stars based on the discrete dipole approximation method as well as the separation of variables method and the Maxwell-Garnett mixing rule. Carbon and silicates were chosen as material of the dust particles. The blackbody radiation of the stars with the effective temperatures in the range 2000-7000 K was considered. This interval covers late-type giants, solar type stars, and Herbig Ae/Be stars. The radiation pressure acting on submicrometer-sized particles around stars increases with the photospheric temperature of the star, indicating the growth of the scattering efficiency of particles with sizes larger than the wavelength of the scattered light. We show that porous, fluffy particles in the submicrometer size range can have longer lifetimes in circumstellar regions than compact (spherical) particles. Going to larger sizes of particles, the effect is reversed. The radiation pressure force for porous particles is only gradually reducing with decreasing size of the particles. As a consequence, the size range of particles that can stay in bound orbits around the star is much smaller for porous particles than for compact particles. We estimate the transverse component of the radiation pressure force on non-spherical particles. It can reach up to about 10% of the radial component in the surroundings of stars with photospheric temperatures beyond 6000 K. This effect is even stronger for compact dielectric grains and may influence their dynamics.

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