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tokens: for a different simulation in Schwadron et al. 2014 ). Other intended applications have been mentioned throughout the text. We encourage interested researchers to contact us if they would like to use our simulation data for complementary investigations. Appendix A The MAS Thermodynamic MHD Model The numerical code MAS employed in this article integrates the standard viscous and resistive one-fluid MHD equations in 3D spherical coordinates. For the coronal simulation described in Sections 3.1 – 3.3 and 4 , the so-called “thermodynamic MHD model” was used, in which the standard equations are extended to include parallel electron thermal conduction, radiative losses, and parameterized coronal heating. The MAS thermodynamic MHD model has been used extensively for simulating the global corona and solar wind (e.g., Mikić et al. 1999 , 2007 ; Lionello et al. 2001 , 2009 ; Downs et al. 2013 ; Linker et al. 2017 ; Titov et al. 2017 ) and eruptive phenomena such as soft X-ray jets (Lionello et al. 2016 ; Török et al. 2016 ) and CMEs (e.g., Linker et al. 2001 , 2003 ; Mikić et al. 2013b ). In this article, we use a version of the model in which the solar wind is accelerated with Alfvén waves using a Wentzel–Kramers–Brillouin (WKB) approximation (Jacques 1977 ). A more sophisticated wave-acceleration model is under development (Lionello et al. 2014 ; Downs et al. 2016 ). In the version used here, the governing equations take the following form: where A is the magnetic vector potential, is the magnetic field, is the current density, ρ is the plasma density, T is the temperature, is the plasma pressure, v is the plasma velocity, is the direction of the magnetic field, c is the speed of light, γ = 5/3 is the adiabatic index, m p is the proton mass, k is Boltzmann’s constant, κ 0 is the coefficient of the classical Spitzer thermal conductivity, is a profile that limits the radial extent within which collisional (Spitzer’s law) thermal conduction is active, is the equivalent profile for collisionless thermal conduction, Q ( T ) is the radiative loss function, H is the coronal heating term that typically consists of a sum of empirical heating functions (Lionello et al. 2009 ), is the Alfvén-wave speed, and is the gravitational force. Note that joule heating, , is not included in Equation ( 3 ). While it is implemented in MAS, we switch it off in our simulation, otherwise the insertion of the current-carrying flux rope into the background corona (Section 3.2 ) would lead to an instantaneous, unphysical temperature increase of the rope. The last expression in Equation ( 4 ) is a semi-implicit term that is added to the equations to stabilize the algorithm for time steps larger than the fast magnetosonic wave limit (Lionello et al. 1999 ; Caplan et al. 2017 ). Equations ( 5 ) and ( 6 ) are the WKB approximation for Alfvén-wave pressure advance (Mikić et al. 1999 ), where + and − are the forward and backward Alfvén-wave energy densities. The electron density