JEŘÁBKOVÁ, Tereza, Daniela KORČÁKOVÁ, A. MIROSHNICHENKO, S. DANFORD, S.V. ZHARIKOV, Radek KŘÍČEK, Petr ZASCHE, Viktor VOTRUBA, Miroslav ŠLECHTA, Petr ŠKODA and Jan JANÍK. Time-dependent spectral-feature variations of stars displaying the B[e] phenomenon III. HD 50138. Astronomy and Astrophysics. EDP Sciences, vol. 586, February, p. "nestrankovano", 29 pp. ISSN 0004-6361. doi:10.1051/0004-6361/201526290. 2016.
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Basic information
Original name Time-dependent spectral-feature variations of stars displaying the B[e] phenomenon III. HD 50138
Authors JEŘÁBKOVÁ, Tereza (203 Czech Republic), Daniela KORČÁKOVÁ (203 Czech Republic), A. MIROSHNICHENKO (643 Russian Federation), S. DANFORD (840 United States of America), S.V. ZHARIKOV (643 Russian Federation), Radek KŘÍČEK (203 Czech Republic), Petr ZASCHE (203 Czech Republic), Viktor VOTRUBA (203 Czech Republic, belonging to the institution), Miroslav ŠLECHTA (203 Czech Republic), Petr ŠKODA (203 Czech Republic) and Jan JANÍK (203 Czech Republic, guarantor, belonging to the institution).
Edition Astronomy and Astrophysics, EDP Sciences, 2016, 0004-6361.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher France
Confidentiality degree is not subject to a state or trade secret
Impact factor Impact factor: 4.378 in 2014
RIV identification code RIV/00216224:14310/16:00089235
Organization unit Faculty of Science
Doi http://dx.doi.org/10.1051/0004-6361/201526290
UT WoS 000369715900127
Keywords in English circumstellar matter; stars: emission line Be; stars: mass loss; binaries: spectroscopic; stars: individual: MWC 158
Tags AKR, rivok
Tags International impact, Reviewed
Changed by Changed by: RNDr. Jan Janík, Ph.D., učo 17241. Changed: 3/4/2019 14:13.
Abstract
We describe the spectral variability of HD 50138 over the last twenty years. Based on these data, we determine new restrictions for future modelling. We confirm the quasi-periodic behaviour of the object’s spectral variability, which probably reflects mass transfer in a binary system. This behaviour also supports a recently introduced explanation of the nature of FS CMa stars as post-merger systems.
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