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On the radioactive shells in peculiar main sequence stars: the phenomenon of Przybylski's star.

Published online by Cambridge University Press:  02 March 2005

Vera F. Gopka ,
Alexander V. Yushchenko ,
Angelina V. Shavrina ,
David E. Mkrtichian ,
Artie P. Hatzes ,
Sergey M. Andrievsky  and
Larissa V. Chernysheva
Vera F. Gopka
Affiliation:
Astronomical observatory, Odessa national University, Park Shevchenko, Odessa, 65014, Ukraine email: gopkavera@mail.ru
Alexander V. Yushchenko
Affiliation:
Astronomical observatory, Odessa national University, Park Shevchenko, Odessa, 65014, Ukraine email: gopkavera@mail.ru Astrophysycal Research Center dor the Structure and Evolution of the Cosmos, Sejong University, Seoul, 143-747, (South) Korea email: yua@arcsec.sejong.ac.kr, david@arcsec.sejong.ac.kr
Angelina V. Shavrina
Affiliation:
Main Astronomical observatory of the Academy of Science of Ukraine, Kiev, 03680, Ukraine email: shavrina@mao.kiev.ua
David E. Mkrtichian
Affiliation:
Astrophysycal Research Center dor the Structure and Evolution of the Cosmos, Sejong University, Seoul, 143-747, (South) Korea email: yua@arcsec.sejong.ac.kr, david@arcsec.sejong.ac.kr Department of astronomy, Odessa National University, Odessa, 65014, Ukraine email: scan@deneb.odessa.ua
Artie P. Hatzes
Affiliation:
Thuringer Landessternwarte, Tautenburg, D-07778, Germany email: artie@tls-tautenburg.de
Sergey M. Andrievsky
Affiliation:
Department of astronomy, Odessa National University, Odessa, 65014, Ukraine email: scan@deneb.odessa.ua
Larissa V. Chernysheva
Affiliation:
A.F. Ioffe Physical-technical institute, Saint-Petrsburgh, 194021, Russia email: Larissa.Chernysheva@mail.ioffe.ru
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Abstract

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Using high-dispersion spectral observations of HD 101065 (Przybylski's star) we have identified the lines of heavy radioactive elements with atomic numbers from 84 to 99 in the spectrum of the star. We found the lines of all these elements except At (Z=85) and Fr (Z=87). We try to explain a presence of such heavy species in the atmosphere of this star as a result of radioactive decay of Th and U nuclei and neutron capture process producing some transuranium isotopes. The necessary conditions for these processes to work may appear due to atomic diffusion and favorable accumulation of the thorium and uranium nuclei in the upper of the PS atmosphere.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Atomic datanucleosynthesisstars: abundancesstars: chemically peculiarstars: individual (HD 101065)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 734 - 742
Copyright
© 2004 International Astronomical Union