  The spectral flux density of stars can indicate their atmospheric physical
properties. A detector can obtain any band flux density at the design stage.
However, the band flux density is confirmed and fixed in the process of
operation because of the restriction of filters. Other band flux densities
cannot be obtained through the same detector. In this study, a computational
model of stellar spectral flux density is established based on basic physical
parameters which are effective temperature and angular parameter. The
stochastic particle swarm optimization algorithm is adopted to address this
issue with appropriately chosen values of the algorithm parameters. Four star
catalogues are studied and consist of the Large Sky Area Multi-Object Fibre
Spectroscopic Telescope (LAMOST), Wide-field Infrared Survey Explorer (WISE),
Midcourse Space Experiment (MSX), and Two Micron All Sky Survey (2MASS). The
given flux densities from catalogues are input parameters. Stellar effective
temperatures and angular parameters are inversed using the given flux densities
according to SPSO algorithm. Then the flux density is calculated according to
Planck's law on the basis of stellar effective temperatures and angular
parameters. The calculated flux density is compared with the given value from
catalogues. It is found that the inversion results are in good agreement for
all bands of the MSX and 2MASS catalogues, whereas they do not agree well in
some bands of the LAMOST and WISE catalogues. Based on the results, data from
the MSX and 2MASS catalogues can be used to calculate the spectral flux density
at different wavelengths of given wavelength ranges. The stellar flux density
is obtained and can provide data support and an effective reference for
detection and recognition of stars.
