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We describe, analyze and validate the recently developed Alfv\'en Wave SolarModel (AWSoM), a 3D global model starting from the top of the chromosphere andextending into interplanetary space (up to 1-2 AU). This model solves theextended two temperature magnetohydrodynamics equations coupled to a wavekinetic equation for low frequency Alfv\'en waves. In this picture, heating andacceleration of the plasma are due to wave dissipation and wave pressuregradients, respectively. The dissipation process is described by a fullydeveloped turbulent cascade of counter-propagating waves. We adopt a unifiedapproach for calculating the wave dissipation in both open and closed magneticfield lines, allowing for a self-consistent treatment of any magnetic topology.Wave dissipation is the only heating mechanism assumed in the model, and nogeometric heating functions are invoked. Electron heat conduction and radiativecooling 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\'enwaves, the perpendicular correlation length of the turbulence, and apseudo-reflection coefficient. We compare model results for Carrington Rotation2063 (November-December 2007) to remote observations in the EUV and X-rayranges from STEREO, SOHO and Hinode spacecraft, as well as to in-situmeasurements performed by Ulysses. The model results are in good agreement withobservations. This is the first global model capable of simultaneouslyreproducing the multi-wavelength observations of the lower corona and the windstructure beyond Earth's orbit.

A Global Wave-Driven MHD Solar Model with a Unified Treatment of Open and Closed Magnetic Field Topologies