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Signs of rotating equatorial density enhancements around SRb pulsators

Published online by Cambridge University Press:  30 December 2019

W. Homan Open the ORCID record for W. Homan [Opens in a new window] ,
L. Decin ,
A. Richards  and
P. Kervella Open the ORCID record for P. Kervella [Opens in a new window]
W. Homan
Affiliation:
IvS, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: [email protected]
L. Decin
Affiliation:
IvS, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: [email protected] University of Leeds, School of Chemistry, Leeds LS2 9JT, United Kingdom
A. Richards
Affiliation:
JBCA, Dept. Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK
P. Kervella
Affiliation:
LESIA (CNRS UMR 8109), Obs. de Paris, PSL, CNRS, UPMC, Univ. Paris-Diderot, France
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Abstract

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We observed the circumstellar environments (CSEs) of the semiregular AGB stars L2 Puppis, R Doradus and EP Aquarii with ALMA. (1) The molecular emission in the L2 Pup nebula reveals an edge-on rotating disk. (2) PV diagrams of the 28SiO emission in the inner CSE of R Dor expose a pattern pointing to an inclined rotating disk. (3) The CO emission in the CSE of EP Aqr reveals a nearly face-on equatorial density enhancement (EDE). The inner EDE strongly resembles theoretical wind-Roche-lobe-overflow models. The SiO emission points to a potential companion. The combination of (1), (2) and (3) suggests that a link may exist between the type of AGB pulsations and the morphological nature of the CSE.

Keywords

stars: AGB and post-AGB starscircumstellar materialstars: mass lossstars: imagingsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 421 - 422
Copyright
© International Astronomical Union 2019 

References

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