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- W2017804781 abstract "The young cluster NGC 2264 contains early type and non-emission stars, as well as T Tauri-like variables which populate the elevated main sequence (Walker 1956). The astrometric study of Vasilevskis et al . (1965) indicates a high probability of these variable stars being cluster members. The generally accepted view is that the stars which lie above the zero-age main sequence are still undergoing contraction. They exhibit infra-red, blue and ultra-violet excesses (Mendoza 1968, Smak 1964), and they are characterized by H α emission, the intensity of which is correlated with ultra-violet excess (Kuhi 1966). In the (U–B, B–V) diagram these stars occupy the same region as would the heavily reddened OB stars. It is necessary to distinguish between them and this can be achieved by the application of multi-colour (UBVRI) photometry. In the present paper UBV photometry of the stars of NGC 2264 has been extended to R and I magnitudes in Johnson's (1966) system, and the infra-red and ultra-violet excesses of the T Tauri-like stars have been studied. The UBV data have been taken from Walker (1956)." @default.
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- W2017804781 date "1971-09-01" @default.
- W2017804781 modified "2023-10-16" @default.
- W2017804781 title "Multicolour Photometry of the Stars in NGC 2264*" @default.
- W2017804781 doi "https://doi.org/10.1093/mnras/153.4.521" @default.
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