Abstract
In this final chapter we focus on binary populations amongst pre-main-sequence stars, namely the evolutionary phase between protostars and the main-sequence which includes both classical and weak-lined T Tauri stars. Our discussion begins by looking at the frequency of pre-main-sequence binaries as a function of environment as well as orbital period. There are brief discussions on higher-order multiple pre-main-sequence binaries, in addition to protostellar binaries, before we move onto the effects of young binary objects with regard to the evolution of circumstellar (and circumbinary) discs.
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Speckle imaging takes advantage of very short exposures in an attempt to freeze the seeing of large telescopes so that potentially diffraction-limited images are less sensitive to atmospheric turbulence. The image centroids of bright point sources in the field of view are registered and the individual exposures are co-added to search for fainter nearby sources. Because in such short exposures one can be limited by the noise of the detector rather than the background sky emission, the sensitivity is much lower than modern adaptive optics assisted imaging.
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Mathieu, R.D. (2015). Pre-main-sequence Binaries. In: Meyer, M., Eyer, L., Bell, C. (eds) Dynamics of Young Star Clusters and Associations. Saas-Fee Advanced Course, vol 42. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-47290-3_14
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