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Rings and filaments: The remarkable detached CO shell of U Antliae
Univ Vienna, Dept Astrophys.
Chalmers Univ Technol, Dept Earth & Space Sci, Onsala Space Observ.
Univ Vienna, Dept Astrophys.
Chalmers Univ Technol, Dept Earth & Space Sci, Onsala Space Observ.
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2017 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 605, A116Article in journal (Refereed) Published
Abstract [en]

Aims. Our goal is to characterize the intermediate age, detached shell carbon star U Antliae morphologically and physically in order to study the mass-loss evolution after a possible thermal pulse.

Methods. High spatial resolution ALMA observations of unprecedented quality in thermal CO lines allow us to derive first critical spatial and temporal scales and constrain modeling efforts to estimate mass-loss rates for both the present day as well as the ejection period of the detached shell.

Results. The detached shell is remarkably thin, overall spherically symmetric, and shows a barely resolved filamentary substructure possibly caused by instabilities in the interaction zone of winds with different outflow velocities. The expansion age of the detached shell is of the order of 2700 yr and its overall width indicates a high expansion-velocity and high mass-loss period of only a few hundred years at an average mass-loss rate of approximate to 10(-5) M-circle dot yr(-1). The post-high-mass-loss-rate-epoch evolution of U Ant shows a significant decline to a substantially lower gas expansion velocity and a mass-loss rate amounting to 4 x 10(-8) M-circle dot yr(-1), at present being consistent with evolutionary changes as predicted for the period between thermal pulses.

Place, publisher, year, edition, pages
2017. Vol. 605, A116
Keyword [en]
stars: AGB and post-AGB, stars: carbon, stars: evolution, stars: mass-loss
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-337756DOI: 10.1051/0004-6361/201730665ISI: 000412231200087OAI: oai:DiVA.org:uu-337756DiVA: diva2:1173328
Funder
Swedish Research Council
Note

Acknowledgements: F.K. and M.B. acknowledge funding by the Austrian Science Fund FWF under project number P23586. M.B. further acknowledges funding through the uni: docs fellowship of the University of Vienna. M.M., H.O., and W.V. acknowledge financial support from the Swedish Research Council. C.P. is supported by the Belgian Fund for Scientific Research F.R.S.-FNRS.

Available from: 2018-01-12 Created: 2018-01-12 Last updated: 2018-01-12Bibliographically approved

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