S. Kimeswenger, J. Koller, Institute of Astrophysics,
University of Innsbruck, Austria
We present steady-state models of the dust shell of Sakurai's Object using a variety of wide dust grain size distributions and dust grains not being in thermal equilibrium. The models are based on methods developed for modelling A58 (Nova Aql 1919, Koller & Kimeswenger, J., Modeling the IR Spectra of Dust Shells around [WC] Stars, AP&SS in press, preprint:
http://info.uibk.ac.at/c/c7/c706/koller/docs/ams99.html). We
show that non-equilibrium calculations are needed to get
real physical
values for the inner condensation edge of small particles, being the
seed for larger grains thereafter. We compare the results of those
models and their implication on the distance/luminosity problem of
Sakurai (and A58 as well). Using data from different epochs and
comparing the results give an estimate on the total mass of the dust
component and the mass loss rates.