2011A&A...532A..54S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST23:12:54

2011A&A...532A..54S - Astronomy and Astrophysics, volume 532A, 54-54 (2011/8-1)

The mass-loss return from evolved stars to the Large Magellanic Cloud. V. The GRAMS carbon-star model grid.

SRINIVASAN S., SARGENT B.A. and MEIXNER M.

Abstract (from CDS):

Outflows from asymptotic giant branch (AGB) and red supergiant (RSG) stars inject dust into the interstellar medium. The total rate of dust return provides an important constraint to galactic chemical evolution models. However, this requires detailed radiative transfer (RT) modeling of individual stars, which becomes impractical for large data sets. An alternative approach is to select the best-fit spectral energy distribution (SED) from a grid of dust shell models, allowing for a faster determination of the luminosities and mass-loss rates for entire samples. We have developed the Grid of RSG and AGB ModelS (GRAMS) to measure the mass-loss return from evolved stars. The models span the range of stellar, dust shell and grain properties relevant to evolved stars. The GRAMS model database will be made available to the scientific community. In this paper we present the carbon-rich AGB model grid and compare our results with photometry and spectra of Large Magellanic Cloud (LMC) carbon stars from the SAGE (Surveying the Agents of Galaxy Evolution) and SAGE-Spec programs. We generate models for spherically symmetric dust shells using the 2Dust code, with hydrostatic models for the central stars. The model photospheres have effective temperatures between 2600 and 4000K and luminosities from ∼2000L to ∼40000L. Assuming a constant expansion velocity, we explore five values of the inner radius Rin of the dust shell (1.5, 3, 4.5, 7 and 12Rstar). We fix the outer radius at 1000 Rin. Based on the results from our previous study, we use amorphous carbon dust mixed with 10% silicon carbide by mass. The grain size distribution follows a power-law and an exponential falloff at large sizes. The models span twenty-six values of 11.3µm optical depth, ranging from 0.001 to 4. For each model, 2Dust calculates the output SED from 0.2 to 200µm. Over 12000 models have dust temperatures below 1800K. For these, we derive synthetic photometry in optical, near-infrared and mid-infrared filters for comparison with available data. We find good agreement with magnitudes and colors observed for LMC carbon-rich and extreme AGB star candidates from the SAGE survey, as well as spectroscopically confirmed carbon stars from the SAGE-Spec study. Our models reproduce the IRAC colors of most of the extreme AGB star candidates, consistent with the expectation that a majority of these enshrouded stars have carbon-rich dust. Finally, we fit the SEDs of some well-studied carbon stars and compare the resulting luminosities and mass-loss rates with those from previous studies.

Abstract Copyright:

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

VizieR on-line data: <Available at CDS (J/A+A/532/A54): grid.dat grid.fit>

Simbad objects: 17

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Number of rows : 17

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 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
2 IRAS 04496-6958 C* 04 49 18.486 -69 53 14.52 20.060 20.027 18.791 15.087 15.060 C 45 0
3 IRAS 04535-6616 C* 04 53 44.241 -66 11 46.14           C-rich 11 0
4 [KDM2001] 1656 C* 05 03 16.6102381687 -65 49 45.081630152 19.681 18.771 16.275 13.660 13.423 C 10 0
5 2MASS J05050322-6924266 LP* 05 05 03.227 -69 24 26.62     16.770   14.040 C-rich 9 0
6 NGC 1835 Cl* 05 05 09.210 -69 24 20.96   11.314 10.596     ~ 155 0
7 IRAS 05103-6959 Mi* 05 10 00.0021953859 -69 56 09.519909604     21.017 17.249 16.758 C-rich 11 0
8 OGLE LMC-LPV-28579 C* 05 13 06.42 -69 09 46.2       17.716 17.586 C 15 0
9 MSX LMC 310 C* 05 20 19.3880413662 -66 35 47.798268030       17.567 14.825 C 22 0
10 [KDM2001] 3409 C* 05 20 21.6162214800 -66 36 04.200036630   16.21 16.07 14.72   C 19 0
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
12 TRM 45 * 05 28 16.3 -67 20 55     16.87     ~ 9 0
13 Cl* NGC 1978 IR 1 C* 05 28 40.2 -66 13 54           C-rich 15 0
14 NGC 1978 GlC 05 28 45.330 -66 14 12.04   10.7 10.70     ~ 273 0
15 IRAS 05289-6617 C* 05 29 02.412 -66 15 27.77   22.276 21.353     C 22 0
16 MSX LMC 1384 Mi* 05 43 36.03 -70 10 35.1         19.445 C-rich 12 0
17 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2133 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-23:12:54

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