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 exist 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.

恒星的质量是其结构、演化和最终命运的最基本参数。这对于任何类型的恒星考古学和系外行星的表征都特别重要。天文学中有多种方法来估计或确定它。在这篇综述中，我们提出了大量此类方法，首先是使用分离食双星的最直接且与模型无关的方法。然后，我们转向更间接和模型相关的方法，例如非常常用的等时线或恒星轨迹拟合。定量星震学的出现开辟了一种全新的方法来确定恒星质量并补充和提高其他方法的准确性。我们包括不同进化阶段的方法，从前主序列到进化的（超级）巨人和最终的遗迹。对于所有方法的不确定性和限制都将被讨论。我们提供了总共 200 多个基准恒星的列表，其相对质量精度在\([0.3,2]\%\)之间，涵盖的质量范围为\(M\in [0.1,16]\,M_\odot\)，其中\(75\%\)是在其核心燃烧氢的恒星，其他\(25\%\)涵盖了所有其他演化阶段。最后，我们建议如何结合各种方法来达到恒星的“质量阶梯”。