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Massive stars play an important role in the mechanical and chemical evolutionof galaxies. Understanding the internal processes of these stars is vital toour understanding of their evolution and eventual end products. Deformationsfrom spherical geometry are common for massive stars; however, the tools thatare currently available for the study of these systems are almost exclusivelyone-dimensional. We present a new spectroscopic analysis tool tailored formassive stars that deviate from spherical symmetry. This code (entitled SPAMMS)is a spectroscopic patch model that takes the three-dimensional surfacegeometry of the system into account to produce spectral profiles at givenphases and orientations. In using the Wilson-Devinney-like code PHOEBE incombination with the non local thermodynamic equilibrium (NLTE) radiativetransfer code FASTWIND, we created a three-dimensional mesh that represents thesurface geometry of our system and we assigned FASTWIND emergent intensity lineprofiles to each mesh triangle, which take the local parameters such astemperature, surface gravity, and radius into account. These line profiles werethen integrated across the visible surface, where their flux contribution andradial velocity are taken into account, thus returning a final line profile forthe visible surface of the system at a given phase. We demonstrate that SPAMMScan accurately reproduce the morphology of observed spectral line profiles forovercontact systems. Additionally, we show how line profiles ofrapidly-rotating single stars differ when taking rotational distortion intoaccount, and the effects that these can have on the determined parameters.Finally, we demonstrate the code's ability to reproduce the Rossiter-Mclaughlinand Struve-Sahade effects.

Spectroscopic patch model for massive stars using PHOEBE II and FASTWIND