The Microwave Thermal Emission from the Zodiacal Dust Cloud Predicted
  with Contemporary Meteoroid Models
  Predictions of the microwave thermal emission from the interplanetary dust
cloud are made using several contemporary meteoroid models to construct the
distributions of cross-section area of dust in space, and applying the Mie
light-scattering theory to estimate the temperatures and emissivities of dust
particles in broad size and heliocentric distance ranges. In particular, the
model of the interplanetary dust cloud by Kelsall et al. (1998, ApJ 508:
44-73), the five populations of interplanetary meteoroids of Divine (1993, JGR
98(E9): 17,029-17,048) and the Interplanetary Meteoroid Engineering Model
(IMEM) by Dikarev et al. (2004, EMP 95: 109-122) are used in combination with
the optical properties of olivine, carbonaceous and iron spherical particles.
The Kelsall model has been widely accepted by the Cosmic Microwave Background
(CMB) community. We show, however, that it predicts the microwave emission from
interplanetary dust remarkably different from the results of application of the
meteoroid engineering models. We make maps and spectra of the microwave
emission predicted by the three models assuming variant composition of dust
particles. Predictions can be used to look for the emission from interplanetary
dust in CMB experiments as well as to plan new observations.
