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The temperature of nonspherical circumstellar dust grains

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Abstract

The temperatures of prolate and oblate spheroidal dust grains in the envelopes of stars of various spectral types are calculated. Homogeneous particles with aspect ratios a/b≤10 composed of amorphous carbon, iron, dirty ice, various silicates, and other materials are considered. The temperatures of spherical and spheroidal particles were found to vary similarly with particle size, distance to the star, and stellar temperature. The temperature ratio T d(spheroid)/T d(sphere) depends most strongly on the grain chemical composition and shape. Spheroidal grains are generally colder than spherical particles of the same volume; only iron spheroids can be slightly hotter than iron spheres. At a/b≈2, the temperature differences do not exceed 10%. If a/b≥4, the temperatures can differ by 30–40%. For a fixed dust mass in the medium, the fluxes at wavelengths λ≥100 are higher if the grains are nonspherical, which gives overestimated dust masses from millimeter observations. The effect of grain shape should also be taken into account when modeling Galactic-dust emission properties, which are calculated when searching for fluctuations of the cosmic microwave background radiation in its Wien wing.

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Authors and Affiliations

  1. Sobolev Astronomical Institute, St. Petersburg State University, Bibliotechnaya pl. 2, St. Petersburg-Peterhof, 198904, Russia

    N. V. Voshchinnikov & D. A. Semenov

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  1. N. V. Voshchinnikov
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  2. D. A. Semenov
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To the memory of Gennadii Borisovich Sholomitski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \), an enthusiast for research in the field of infrared and submillimeter astronomy.

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Translated from Pis'ma v Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \) Zhurnal, Vol. 26, No. 10, 2000, pp. 787–800.

Original Russian Text Copyright © 2000 by Voshchinnikov, Semenov.

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Voshchinnikov, N.V., Semenov, D.A. The temperature of nonspherical circumstellar dust grains. Astron. Lett. 26, 679–690 (2000). https://doi.org/10.1134/1.1316114

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