Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26as..102..201n&link_type=abstract
Astronomy and Astrophysics Supplement, Vol.102, NO.1/NOVII, P. 201, 1993
Astronomy and Astrophysics
Astrophysics
20
Open Clusters: Individual: Ngc 2264, Stars: Sequence, Circumstellar Matter, Stars: Fundamental Parameters
Scientific paper
We present uvby-β and JHKLM photometry of about 50 stars reported as peculiar in the literature and associated with NGC 2264. In addition to stars with infrared and/or ultraviolet excesses and to objects with Hβ line in emission the sample includes "subluminous" as well as "IR flux deficient" stars. Quasi-simultaneous optical and near infrared observations were carried on in 44% of the cases. 70% of the sample stars are variable or possible variable stars. A distance and a mean reddening to NGC 2264 of d = 910±50 pc and E(b - y) = 0m.05±0m.01 are found here, respectively. The positions of the peculiar stars in the (V, b - y) diagram corroborate the "subluminous" star groups. The quasi-simultaneous optical and near infrared data do not confirm the existence of the "IR flux deficient" stars. Physical parameters (Teff and log g) of normal field stars are derived from their optical photometry, mainly from their positions in the (b - y)0, [m1] and [c1], [m1l diagrams, and then compared with those parameters given in the literature that were obtained by more direct methods. The two sets of parameters agree well for stars earlier than about spectral type A4, whereas for later type stars the photometric values differ systematically. We give correction equations for the latter in order to obtain from uvby photometry effective temperatures or spectral types and surface gravities for stars in general, and in particular, for most of the peculiar stars in the sample. Based on the photometric spectral types given here and those found in the literature for the program stars we suggest a final spectral type for each object, which should represent best the underlying photosphere of the PMS star.
Carlos Chavarria-K.
de Lara E.
Neri L. J.
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