The mass of a star is the most fundamental parameter for its structure , evolution , and final fate .
It is particularly important for any kind of stellar archaeology and characterization of exoplanets .
There exists a variety of methods in astronomy to estimate or determine it .
In this review we present a significant number of such methods , beginning with the most direct and model-independent approach using detached eclipsing binaries .
We then move to more indirect and model-dependent methods , such as the quite commonly used isochrone or stellar track fitting .
The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods .
We include methods for different evolutionary stages , from the pre-main sequence to evolved ( super ) giants and final remnants .
For all methods uncertainties and restrictions will be discussed .
We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between [ 0.3 , 2 ] \% for the covered mass range of M \in [ 0.1 , 16 ] { M _ { \odot } } , 75 \% of which are stars burning hydrogen in their core and the other 25 \% covering all other evolved stages .
We close with a recommendation how to combine various methods to arrive at a “ mass-ladder ” for stars .

\PACS 97.10.Nf , 97.10.Cv , 97.80.Hn , 97.82.-j , 98.35.Ln