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In the radio regime the mass-loss rate of AGB stars is best probed usingmolecular (and atomic) line emission arising in the CSE formed by the stellarwind. The numerical modelling of the circumstellar emission where intricateinterplays between physical and chemical processes take place, is a challenge.The derived mass-loss rates depend crucially on the assumptions in thecircumstellar model, of which some can be constrained if enough observationaldata exist. Therefore, a reliable mass-loss-rate determination for anindividual star requires, in addition to a detailed radiative transferanalysis, good observational constraints in the form of multi-line observationsand radial brightness distributions. Of the methods used to estimate mass-lossrates from galactic AGB stars those based on radiative transfer modelling of COline emission are most commonly used and possibly also the most accurate.Typically, CO multi-transitional observations can constrain the mass-loss rateto better than 50%, within the adopted circumstellar model. Comparison withcomplementary methods, such as estimates based on dust radiative transfermodelling coupled with a dynamical model, are consistent within a factor ofthree.

Methods for determining AGB mass loss rates based on radio data