The identification of the low-degree p modes in other stars is the challenge of future asteroseismology space missions such as Corot, MONS, Most or Eddington. The identification is based on a priori knowledge of the characteristics of the modes. We shall review the most common assumptions needed for the identification such as basic stellar structure, visibilities, rotational splittings or linewidths. We shall describe a few tools needed for facilitating the identification. As soon as modes are properly identified, the peakbagging of the mode characteristics can begin using Maximum Likelihood Estimation. We shall give examples of the whole process using solar data and hare-and-hounds excercises performed in the frame work of the Corot project.

 
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