2010A&A...515A..27O


C.D.S. - SIMBAD4 rel 1.7 - 2020.03.31CEST16:35:42

2010A&A...515A..27O - Astronomy and Astrophysics, volume 515, A27-27 (2010/6-1)

High-resolution HST/ACS images of detached shells around carbon stars.

OLOFSSON H., MAERCKER M., ERIKSSON K., GUSTAFSSON B. and SCHOEIER F.

Abstract (from CDS):

Overall spherically symmetric, geometrically thin gas and dust shells have been found around a handful of asymptotic giant branch (AGB) carbon stars. Their dynamical ages lie in the range of 103 to 104 years. A tentative explanation for their existence is that they have formed as a consequence of mass-loss-rate modulations during a He-shell flash. The detached shells carry information on their formation process, as well as on the small-scale structure of the circumstellar medium around AGB stars due to the absence of significant line-of-sight confusion. The youngest detached shells, those around the carbon stars R Scl and U Cam, are studied here in great detail in scattered stellar light with the Advanced Survey Camera on the Hubble Space Telescope. Quantitative results are derived assuming optically thin dust scattering. The detached dust shells around R Scl and U Cam are found to be consistent with an overall spherical symmetry. They have radii of 19.2" (corresponding to a linear size of 8x1016cm) and 7.7" (5x1016cm), widths of 1.2" (5x1015cm) and 0.6" (4x1015cm), and dust masses of 3x10–6 and 3x10–7M, respectively. The dynamical ages of the R Scl and U Cam shells are estimated to be 1700 and 700yr, respectively, and the shell widths correspond to time scales of 100 and 50yr, respectively. Small-scale structure in the form of less than arcsec-sized clumps is clearly seen in the images of the R Scl shell. Average clump dust masses are estimated to be about 2x10–9M. Comparisons with CO line interferometer data show that the dust and gas shells coincide spatially, within the errors (≤1" for U Cam and ≃2" for R Scl). The results are consistent with the interpretation of geometrically thin gas and dust shells formed by a mass-loss eruption during a He-shell flash, and where interaction with a previous wind plays a role as well. The mass loss responsible for the shells must have been remarkably isotropic, and, if wind interaction plays a role, this also applies to the mass loss prior to the eruption. Clumpy structure is present in the R Scl shell, possibly as a consequence of the mass loss itself, but more likely as a consequence of instabilities in the expanding shell.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - stars: carbon - circumstellar matter - stars: mass-loss

Status at CDS:  

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* T Cet S* 00 21 46.2731778 -20 03 28.884826   7.32 5.74     M5-6Se 139 0
2 V* R Scl C* 01 26 58.0946233986 -32 32 35.437732667 17.26 9.59 5.72 3.69 2.30 C-N5+ 293 0
3 V* CQ Cam LP* 03 24 40.5563686966 +64 35 09.587610453 9.53 7.24 5.19 3.61 2.38 M0II 76 0
4 V* U Cam C* 03 41 48.1762532767 +62 38 54.397016016   11.5 11.00     C-N5 230 0
5 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2121 0
6 V* U Ant C* 10 35 12.8508908507 -39 33 45.320533564 15.32 8.22 5.38 3.18 1.86 C-N3 136 0
7 V* S Sct C* 18 50 20.0367524071 -07 54 27.430964220 13.93 9.89 6.80     C-N5 194 0
8 V* TT Cyg C* 19 40 57.0159854799 +32 37 05.755486755   10.43 10.20     C-N5- 185 0
9 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2312 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2010A&A...515A..27O and select 'bookmark this link' or equivalent in the popup menu


2020.03.31-16:35:42

© Université de Strasbourg/CNRS

    • Contact