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@article{1406900,
author = {Niemczura, Ewa and Huemmerich, Stefan and Castelli, Fiorella and Paunzen, Ernst and Bernhard, Klaus and Hambsch, FranzandJosef and Helminiak, Krzysztof},
article_location = {LONDON},
article_number = {July},
doi = {http://dx.doi.org/10.1038/s41598-017-05987-6},
keywords = {UPPER MAIN-SEQUENCE; MAGNETIC-FIELD; A-STARS; ASTROPHYSICAL INTEREST; EFFECTIVE TEMPERATURE; BETA PHOTOMETRY; SURFACE GRAVITY; T-EFF; LOG-G; CALIBRATION},
language = {eng},
issn = {2045-2322},
journal = {Scientific reports},
title = {HD 66051, an eclipsing binary hosting a highly peculiar, HgMn-related star},
volume = {7},
year = {2017}
}
TY - JOUR
ID - 1406900
AU - Niemczura, Ewa - Huemmerich, Stefan - Castelli, Fiorella - Paunzen, Ernst - Bernhard, Klaus - Hambsch, Franz-Josef - Helminiak, Krzysztof
PY - 2017
TI - HD 66051, an eclipsing binary hosting a highly peculiar, HgMn-related star
JF - Scientific reports
VL - 7
IS - July
SP - nestránkováno
EP - nestránkováno
PB - NATURE PUBLISHING GROUP
SN - 20452322
KW - UPPER MAIN-SEQUENCE
KW - MAGNETIC-FIELD
KW - A-STARS
KW - ASTROPHYSICAL INTEREST
KW - EFFECTIVE TEMPERATURE
KW - BETA PHOTOMETRY
KW - SURFACE GRAVITY
KW - T-EFF
KW - LOG-G
KW - CALIBRATION
N2 - 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.
ER -
NIEMCZURA, Ewa, Stefan HUEMMERICH, Fiorella CASTELLI, Ernst PAUNZEN, Klaus BERNHARD, Franz-Josef HAMBSCH a Krzysztof HELMINIAK. HD 66051, an eclipsing binary hosting a highly peculiar, HgMn-related star. \textit{Scientific reports}. LONDON: NATURE PUBLISHING GROUP, 2017, roč.~7, July, s.~nestránkováno, 11 s. ISSN~2045-2322. Dostupné z: https://dx.doi.org/10.1038/s41598-017-05987-6.
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