Search: onr:"swepub:oai:DiVA.org:uu-281832" >
A detailed view of ...
A detailed view of the gas shell around R Sculptoris with ALMA
-
- Maercker, Matthias, 1979 (author)
- Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.,Chalmers tekniska högskola,Chalmers University of Technology,Universität Wien,University of Vienna,European Southern Observatory (ESO)
-
- Vlemmings, Wouter, 1974 (author)
- Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.,Chalmers tekniska högskola,Chalmers University of Technology
-
- Brunner, M. (author)
- Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
-
show more...
-
- De Beck, Elvire, 1985 (author)
- Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.,Chalmers tekniska högskola,Chalmers University of Technology
-
- Humphreys, E. M. (author)
- European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
-
- Kerschbaum, F. (author)
- Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.,Universität Wien,University of Vienna
-
- Lindqvist, Michael, 1960 (author)
- Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.,Chalmers tekniska högskola,Chalmers University of Technology
-
- Olofsson, Hans, 1952 (author)
- Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.,Chalmers tekniska högskola,Chalmers University of Technology
-
- Ramstedt, Sofia (author)
- Uppsala universitet,Observationell astrofysik,Uppsala University
-
show less...
-
Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden Chalmers tekniska högskola (creator_code:org_t)
- 2016-01-19
- 2016
- English.
-
In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 586
- Related links:
-
https://www.aanda.or...
-
show more...
-
http://publications.... (primary) (free)
-
https://urn.kb.se/re...
-
https://doi.org/10.1...
-
https://research.cha...
-
show less...
Abstract
Subject headings
Close
- Context. During the asymptotic giant branch (AGB) phase, stars undergo thermal pulses - short-lived phases of explosive helium burning in a shell around the stellar core. Thermal pulses lead to the formation and mixing-up of new elements to the stellar surface. They are hence fundamental to the chemical evolution of the star and its circumstellar envelope. A further consequence of thermal pulses is the formation of detached shells of gas and dust around the star, several of which have been observed around carbon-rich AGB stars. Aims. We aim to determine the physical properties of the detached gas shell around R Sculptoris, in particular the shell mass and temperature, and to constrain the evolution of the mass-loss rate during and after a thermal pulse. Methods. We analyse (CO)-C-12(1-0), (CO)-C-12(2-1), and (CO)-C-12(3-2) emission, observed with the Atacama Large Millimeter/submillimeter Array (ALMA) during Cycle 0 and complemented by single-dish observations. The spatial resolution of the ALMA data allows us to separate the detached shell emission from the extended emission inside the shell. We perform radiative transfer modelling of both components to determine the shell properties and the post-pulse mass-loss properties. Results. The ALMA data show a gas shell with a radius of 19.'' 5 expanding at 14.3 km s(-1). The different scales probed by the ALMA Cycle 0 array show that the shell must be entirely filled with gas, contrary to the idea of a detached shell. The comparison to single-dish spectra and radiative transfer modelling confirms this. We derive a shell mass of 4.5 x 10(-3) M-circle dot with a temperature of 50 K. Typical timescales for thermal pulses imply a pulse mass-loss rate of 2.3 x 10(-5) M-circle dot yr(-1). For the post-pulse mass-loss rate, we find evidence for a gradual decline of the mass-loss rate, with an average value of 1.6 x 10(-5) M-circle dot yr(-1). The total amount of mass lost since the last thermal pulse is 0.03 M-circle dot, a factor four higher compared to classical models, with a sharp decline in mass-loss rate immediately after the pulse. Conclusions. We find that the mass-loss rate after a thermal pulse has to decline more slowly than generally expected from models of thermal pulses. This may cause the star to lose significantly more mass during a thermal pulse cycle, which affects the lifetime on the AGB and the chemical evolution of the star, its circumstellar envelope, and the interstellar medium.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- stars: AGB and post-AGB
- binaries: general
- stars: carbon
- stars: evolution
- stars: mass-loss
Publication and Content Type
- ref (subject category)
- art (subject category)
Find in a library
To the university's database
- By the author/editor
-
Maercker, Matthi ...
-
Vlemmings, Woute ...
-
Brunner, M.
-
De Beck, Elvire, ...
-
Humphreys, E. M.
-
Kerschbaum, F.
-
show more...
-
Lindqvist, Micha ...
-
Olofsson, Hans, ...
-
Ramstedt, Sofia
-
show less...
- About the subject
-
- NATURAL SCIENCES
-
NATURAL SCIENCES
-
and Physical Science ...
-
and Astronomy Astrop ...
- Articles in the publication
-
Astronomy and As ...
- By the university
-
Uppsala University
-
Chalmers University of Technology