Synthetic line profiles of rotationally distorted hot-star winds

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On the formation of Hα line emission around classical T Tauri stars (2006, methodology): “3 T H E R A D I AT I V E T R A N S F E R M O D E L We have extended the TORUS radiative transfer code (Harries 2000; Kurosawa et al. 2004; Symington et al. 2005a) to include the multiple circumstellar components described above.”
Mass loss from hot massive stars (2008, methodology): “Monte Carlo models for scattering off wind clumps were developed by Code and Whitney (1995), Rodrigues and Magalhaes (2000), Harries (2000), whilst analy tical models to produce the variability of the linear polarization were pre sented by Davies et al (2007).”
EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, methodology): “With that established, we have created a 2D azimuthally symmetric model of a disk with the radiation transfer capabilities of the TORUS code (Harries 2000; Harries et al. 2004; Kurosawa et al. 2004; Pinte et al. 2009).”