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We summarize the main results of a modeling aimed to reproduce the
observed properties of the earliest phases of massive star formation. The
models calculate the spectral energy distribution (SED) as well as the
molecular emission of massive protostars under the hyphotesis that they
form via an accrecion process. We take into account a wide base set
of observational data paying special attention to reproduce the highangular
resolution observations (< 100) of the dust continuun emission
and molecular line of high excitation levels. Firstly, we present a model
of a spherically symmetric infalling envelope that reproduce simultaneouslly
the SED and VLA subarcsecond observations of ammonia (4,4)
hyperfine line emission. In this case, we are able to determine temperature,
density, velocity, velocity dipersion, abundance variations along
the core. Secondly, we present a model of a flattened envelope to reproduce
the SED obtained with Gemini observations at the mid-infrared
wavelengths. In this case, we are able to constrain parameters such as
the degree of elongation, rotation of the envelope, inclination of the system,
etc. With these two approachs we have been able to apply to the
formation of the massive stars models with a degree of detail similar to
those applied to the low-mass protostars.
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