Abstract
The subclass of Near-Contact Binary stars (NCB) was defined by Shaw (1990). They are eclipsing binaries which 1) have periods of less than one day, 2) exhibit strong tidal actions, 3) are less than 0.1 orbital radius apart at their facing surfaces, but they are not in contact. They also have an A- or F- type primary component and a much cooler (by one or two spectral types) secondary, and most have at least one component filling its Roche lobe. There is evidence that they are evolutionary precursors to A-type UMa sources and that they are in the early stages of mass transfer.
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Shaw, J.S., Smith, E. (2000). Coronal Activity of Near-Contact Binaries. In: Cheng, K.S., Chau, H.F., Chan, K.L., Leung, K.C. (eds) Stellar Astrophysics. Astrophysics and Space Science Library, vol 254. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0878-5_23
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DOI: https://doi.org/10.1007/978-94-010-0878-5_23
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