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Possible evidence for a magnetic dynamo in hot Algols

Published online by Cambridge University Press:  24 September 2020

R. E. Mennickent Open the ORCID record for R. E. Mennickent [Opens in a new window] ,
J. Garcés ,
G. Djurašević ,
G. Rojas ,
D. Schleicher  and
S. Otero
R. E. Mennickent
Affiliation:
Universidad de Concepción, Departamento de Astronoma, Casilla 160-C, Concepción, Chile emails: [email protected], [email protected], [email protected], [email protected]
J. Garcés
Affiliation:
Universidad de Concepción, Departamento de Astronoma, Casilla 160-C, Concepción, Chile emails: [email protected], [email protected], [email protected], [email protected]
G. Djurašević
Affiliation:
Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia email: [email protected] Issac Newton institute of Chile, Yugoslavia Branch, 11060, Belgrade, Serbia
G. Rojas
Affiliation:
Universidad de Concepción, Departamento de Astronoma, Casilla 160-C, Concepción, Chile emails: [email protected], [email protected], [email protected], [email protected]
D. Schleicher
Affiliation:
Universidad de Concepción, Departamento de Astronoma, Casilla 160-C, Concepción, Chile emails: [email protected], [email protected], [email protected], [email protected]
S. Otero
Affiliation:
American Association of Variable Star Observers, USA email: [email protected]
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Abstract

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We present the case of hot semi-detached Algols showing photometric cycles longer than the orbital period. The evidence indicating that this long cycle might be due to a magnetic dynamo operating in the rapidly rotating donor star is examined.

Keywords

binaries: spectroscopicclosestars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 207 - 210
Copyright
© International Astronomical Union 2020

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