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The carbon abundance in the atmospheres of single and binary stars
The carbon abundance in the atmospheres of single stars and the brightercomponents of binary stars are determined on the basis ofhigh-dispersion W(lambda) data, using the LTE atmospheric model for C IIlines and the non-LTE model for C III lines. The mean value of lg N (C)for 38 single stars was found to be 8.5 + or - 0.3. For 48 binary stars,the mean value was 8.3 + or - 0.3. The lesser carbon abundance in theatmospheres of binary stars may be explained by a more intense transferof matter from hydrogen burning regions to the atmosphere in theCNO-cycle compared to normal single stars.
| Optical and radio study of BL Lacertae.
Abstract image available at:http://adsabs.harvard.edu/abs/1969A&A.....3..436B
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Member of following groups:
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Observation and Astrometry data
| Constellation: | Lacerta |
| Right ascension: | 22h38m39.74s |
| Declination: | +52°52'25.7" |
| Apparent magnitude: | 8.035 |
| Distance: | 332.226 parsecs |
| Proper motion RA: | -5.3 |
| Proper motion Dec: | -7.1 |
| B-T magnitude: | 10.066 |
| V-T magnitude: | 8.203 |
Catalogs and designations:
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