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Observational techniques to measure solar and stellar oscillations
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As said by Sir A. Eddington in 1925: Our telescopes may probe farther and farther into the depths of space. At first sight it would seem that the deep interior of the sun and stars is less accessible to scientific investigation than any other region of the universe. What appliance can pierce through the outer layers of a star and test the conditions within? Eddington (1926). Nowadays, asteroseismology has proven its ability to pierce below stellar pho- tospheres and allow us to see inside the interior of thousands of stars down to the stellar cores, answering the question asked by Eddington ninety years ago. In this chapter we review the general properties of the spectral analysis which is the base of any asteroseismic investigation. After describing the stellar power spectrum, we will describe in details the characterization of the modal spec- trum. This chapter will end by a brief description of the instrumentation in both helio and asteroseismology.
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The subgiant HR 7322 as an asteroseismic benchmark star
HR 7322's precise interferometric radius agrees with asteroseismic scaling relations, while standard stellar models underpredict the radius unless a sub-solar mixing length is adopted.
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