Editing Inverse problem (section)

===== {{anchor|Doppler tomography}}Doppler tomography (astrophysics) =====

If we consider a rotating stellar object, the spectral lines we can observe on a spectral profile will be shifted due to Doppler effect. Doppler tomography aims at converting the information contained in spectral monitoring of the object into a 2D image of the emission (as a function of the radial velocity and of the phase in the periodic rotation movement) of the stellar atmosphere. As explained by [[Tom Marsh (astronomer)|Tom Marsh]]<ref>{{cite journal |last1=Marsh |first1=Tom |title=Doppler tomography |journal=Astrophysics and Space Science |volume=296 |date=2005 |issue=1–4 |pages=403–415 |doi=10.1007/s10509-005-4859-3 |arxiv=astro-ph/0011020 |bibcode=2005Ap&SS.296..403M |s2cid=15334110 }}</ref> this linear inverse problem is tomography like: we have to recover a distributed parameter which has been integrated along lines to produce its effects in the recordings.