2002A&A...384..452W


Query : 2002A&A...384..452W

2002A&A...384..452W - Astronomy and Astrophysics, volume 384, 452-459 (2002/3-3)

An improved mass-loss description for dust-driven superwinds and tip-AGB evolution models.

WACHTER A., SCHROEDER K.-P., WINTERS J.M., ARNDT T.U. and SEDLMAYR E.

Abstract (from CDS):

We derive an improved description of dust-driven stellar mass-loss for the cool winds of carbon-rich tip-AGB stars. We use pulsating wind models in which the mass loss is driven by radiation pressure on dust grains, for C-rich chemistry. From a larger set of these models, selected for representative dynamical (pulsational velocity amplitude Δv, period P) and chemical (the εCO abundance ratio) input parameters, an improved approximative mass-loss formula has been derived which depends only on the stellar parameters (effective temperature Teff, luminosity L and mass M). Due to the detailed consideration of the chemistry and the physics of the dust nucleation and growth processes, there is a particularly strong dependence of the mass-loss rate {dot}(M) (in M/yr) on Teff: log{dot}(M)=8.86-1.95*logM/M-6.81*logT/K+2.47*logL/L. The dependence of the model mass-loss on the pulsational period has explicitly been accounted for in connection with the luminosity dependence, by applying an observed period-luminosity relation for C-rich Miras. We also apply the improved mass-loss description to our evolution models, and we revisit their tip-AGB mass-loss histories and the total masses lost, in comparison to our earlier work with a preliminary mass-loss description. While there is virtually no difference for the models in the lower mass range of consideration (Mi=1.0 to ≃1.3M), we now find more realistic, larger superwind mass-loss rates for larger stellar masses: i.e., {dot}(M) between ≃0.4 and 1.0x10–4M/yr for Mi between 1.85 and 2.65M, removing between 0.6 and 1.2M, respectively, during the final 30000yrs on the tip-AGB.

Abstract Copyright:

Journal keyword(s): stars: carbon - stars: circumstellar matter - stars: evolution - stars: interiors - stars: late-type - stars: mass loss

Simbad objects: 18

goto Full paper

goto View the references in ADS

Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* R Scl C* 01 26 58.0939182720 -32 32 35.439234828 17.26 9.59 5.72 3.69 2.30 C-N5+ 315 0
2 V* R For C* 02 29 15.3077617632 -26 05 55.646585700   12.94 7.50     C4,3e 188 0
3 V* R Lep C* 04 59 36.3486921120 -14 48 22.502479140 15.06 13.51 7.76 4.90 3.42 C7,6e 326 0
4 RAFGL 799 C* 05 40 36.9286934424 +13 48 22.396959792       12.24   C8,4J 41 0
5 RAFGL 865 C* 06 04 00.04728 +07 25 52.0104           C-rich 98 0
6 RAFGL 935 C* 06 25 27.2602239336 -09 32 06.248402592       15.52 13.09 C 42 0
7 RAFGL 971 C* 06 36 54.2452032888 +03 25 28.696182312       18.4   C5,9e 66 0
8 V* HV CMa C* 07 05 05.8274900568 -15 00 57.922888572       14.109   C-*6 29 0
9 RAFGL 1085 C* 07 12 04.0051268952 -20 17 23.124543108       14.43   C 57 0
10 [W71b] 021-06 C* 08 10 48.8849951112 -32 52 05.635358940       15.07 12.76 C 55 0
11 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2239 0
12 WOS 48 C* 15 23 05.0730770544 -51 25 58.762691652   17.85 16.66 14.51 10.18 C 125 1
13 Case 181 C* 19 03 18.4284440280 +07 30 45.340262352     14.22 14.77   C 69 0
14 IRC -10502 C* 19 20 18.1200757128 -08 02 12.063360120       13.22 10.59 C5,4e 69 0
15 V* V1421 Aql C* 19 27 14.7581047608 +07 04 12.671205564     14.30 14.69   C7,3e 47 0
16 V* TT Cyg C* 19 40 57.0158460384 +32 37 05.756696400   10.43 10.20     C-N5- 195 0
17 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 262 0
18 RAFGL 3099 C* 23 28 17.1145171968 +10 54 37.402209036           C-rich 89 0

To bookmark this query, right click on this link: simbad:objects in 2002A&A...384..452W and select 'bookmark this link' or equivalent in the popup menu


2022.05.22-03:36:03

© Université de Strasbourg/CNRS

    • Contact