  We describe, analyze and validate the recently developed Alfv\'en Wave Solar
Model (AWSoM), a 3D global model starting from the top of the chromosphere and
extending into interplanetary space (up to 1-2 AU). This model solves the
extended two temperature magnetohydrodynamics equations coupled to a wave
kinetic equation for low frequency Alfv\'en waves. In this picture, heating and
acceleration of the plasma are due to wave dissipation and wave pressure
gradients, respectively. The dissipation process is described by a fully
developed turbulent cascade of counter-propagating waves. We adopt a unified
approach for calculating the wave dissipation in both open and closed magnetic
field lines, allowing for a self-consistent treatment of any magnetic topology.
Wave dissipation is the only heating mechanism assumed in the model, and no
geometric heating functions are invoked. Electron heat conduction and radiative
cooling are also included. We demonstrate that the large-scale, steady-state
(in the co-rotating frame) properties of the solar environment are reproduced,
using three adjustable parameters: the Poynting flux of chromospheric Alfv\'en
waves, the perpendicular correlation length of the turbulence, and a
pseudo-reflection coefficient. We compare model results for Carrington Rotation
2063 (November-December 2007) to remote observations in the EUV and X-ray
ranges from STEREO, SOHO and Hinode spacecraft, as well as to in-situ
measurements performed by Ulysses. The model results are in good agreement with
observations. This is the first global model capable of simultaneously
reproducing the multi-wavelength observations of the lower corona and the wind
structure beyond Earth's orbit.
