Poster abstract details

We present a new method to compute the spatial sensitivity of helioseismic travel times to weak perturbations to a background solar model. This method uses numerical simulations of solar oscillations as input. Its advantages include simplicity, a wider range of applications (e.g., perturbations with respect to a 3D background model), and the possibility of modeling subtle observational effects (e.g., line-of-sight projection, foreshortening, known systematic errors). While we present example calculations for time-distance helioseismology, this method could be generalized to any other method of local helioseismology.