NIEMCZURA, Ewa, Stefan HUEMMERICH, Fiorella CASTELLI, Ernst PAUNZEN, Klaus BERNHARD, Franz-Josef HAMBSCH and Krzysztof HELMINIAK. HD 66051, an eclipsing binary hosting a highly peculiar, HgMn-related star. Scientific reports. LONDON: NATURE PUBLISHING GROUP, 2017, vol. 7, July, p. nestránkováno, 11 pp. ISSN 2045-2322. Available from: https://dx.doi.org/10.1038/s41598-017-05987-6.
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Basic information
Original name HD 66051, an eclipsing binary hosting a highly peculiar, HgMn-related star
Authors NIEMCZURA, Ewa (616 Poland), Stefan HUEMMERICH (276 Germany), Fiorella CASTELLI (380 Italy), Ernst PAUNZEN (40 Austria, guarantor, belonging to the institution), Klaus BERNHARD (40 Austria), Franz-Josef HAMBSCH (56 Belgium) and Krzysztof HELMINIAK (616 Poland).
Edition Scientific reports, LONDON, NATURE PUBLISHING GROUP, 2017, 2045-2322.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
Impact factor Impact factor: 4.122
RIV identification code RIV/00216224:14310/17:00099899
Organization unit Faculty of Science
Doi http://dx.doi.org/10.1038/s41598-017-05987-6
UT WoS 000405895400003
Keywords in English UPPER MAIN-SEQUENCE; MAGNETIC-FIELD; A-STARS; ASTROPHYSICAL INTEREST; EFFECTIVE TEMPERATURE; BETA PHOTOMETRY; SURFACE GRAVITY; T-EFF; LOG-G; CALIBRATION
Tags NZ, rivok
Tags International impact, Reviewed
Changed by Changed by: Ing. Nicole Zrilić, učo 240776. Changed: 4/4/2018 13:57.
Abstract
HD 66051 is an eclipsing system with an orbital period of about 4.75 d that exhibits out-of-eclipse variability with the same period. New multicolour photometric observations confirm the longevity of the secondary variations, which we interpret as a signature of surface inhomogeneities on one of the components. Using archival and newly acquired high-resolution spectra, we have performed a detailed abundance analysis. The primary component is a slowly rotating late B-type star (T-eff = 12500 +/- 200 K; log g = 4.0, v sin i = 27 +/- 2 km s(-1)) with a highly peculiar composition reminiscent of the singular HgMn-related star HD 65949, which seems to be its closest analogue. Some light elements as He, C, Mg, Al are depleted, while Si and P are enhanced. Except for Ni, all the iron-group elements, as well as most of the heavy elements, and in particular the REE elements, are overabundant. The secondary component was estimated to be a slowly rotating A-type star (T-eff similar to 8000 K; log g = 4.0, v sin i similar to 18 km s(-1)). The unique configuration of HD 66051 opens up intriguing possibilities for future research, which might eventually and significantly contribute to the understanding of such diverse phenomena as atmospheric structure, mass transfer, magnetic fields, photometric variability and the origin of chemical anomalies observed in HgMn stars and related objects.
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