2002A&A...382..241M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:52:57

2002A&A...382..241M - Astronomy and Astrophysics, volume 382, 241-255 (2002/1-4)

Crystalline silicate dust around evolved stars. III. A correlations study of crystalline silicate features.

MOLSTER F.J., WATERS L.B.F.M., TIELENS A.G.G.M., KOIKE C. and CHIHARA H.

Abstract (from CDS):

We have carried out a quantitative trend analysis of the crystalline silicates observed in the ISO spectra of a sample of 14 stars with different evolutionary backgrounds. We have modeled the spectra using a simple dust radiative transfer model and have correlated the results with other known parameters. We confirm the abundance difference of the crystalline silicates in disk and in outflow sources, as found by Molster et al. (1999Natur.401..563M). We found some evidence that the enstatite over forsterite abundance ratio differs, it is slightly higher in the outflow sources with respect to the disk sources. It is clear that more data is required to fully test this hypothesis. We show that the 69.0 micron feature, attributed to forsterite, may be a very suitable temperature indicator. We found that the enstatite is more abundant than forsterite in almost all sources. The temperature of the enstatite grains is about equal to that of the forsterite grains in the disk sources but slightly lower in the outflow sources. Crystalline silicates are on average colder than amorphous silicates. This may be due to the difference in Fe content of both materials. Finally we find an indication that the ratio of ortho to clino enstatite, which is about 1:1 in disk sources, shifts towards ortho enstatite in the high luminosity (outflow) sources.

Abstract Copyright:

Journal keyword(s): infrared: stars - stars: AGB and post-AGB - mass loss - planetary nebulae - dust

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 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 715 0
2 HD 45677 Be* 06 28 17.4219761127 -13 03 11.130589443 7.86 8.52 8.50 8.11 8.01 B2IV/V[e] 303 0
3 IRAS 09425-6040 C* 09 44 01.6685286753 -60 54 25.636690927     12.6     C 54 0
4 MR 22 PN 10 21 33.826 -58 05 48.26     12.7     A2Ie 101 0
5 HD 302821 sg* 10 23 19.4807452802 -59 32 04.680572222   10.59 9.17     A7Ie 75 1
6 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 756 1
7 HD 161796 pA* 17 44 55.4696 +50 02 39.484 8.00 7.68 7.21 6.77 6.51 F3Ib 310 0
8 * 89 Her pA* 17 55 25.1884459710 +26 02 59.970100296 5.36 5.70 5.36 5.06 4.94 F2Ibp 386 0
9 NGC 6537 PN 18 05 13.104 -19 50 34.88     13.58     ~ 410 1
10 EM* MWC 922 Be* 18 21 16.059408 -13 01 25.68432     13.80 13.65   B[e] 83 0
11 EM* MWC 300 Ae* 18 29 25.6915000349 -06 04 37.289920628 12.55 12.67 13.795     B1Ia+[e] 127 0
12 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 316 0
13 OH 26.5 +0.6 OH* 18 37 32.50920 -05 23 59.1936           ~ 284 0
14 HD 179821 pA* 19 13 58.6083165753 +00 07 31.934676028 10.81 9.694 8.19     G4_0-Ia 221 0
15 PN Vy 2-2 PN 19 24 22.2390166933 +09 53 56.259102426   14.02 12.65 13.38   ~ 248 0
16 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 452 0
17 NML Cyg s*r 20 46 25.5382179476 +40 06 59.396202678   18.64 16.60     M7/8 482 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-21:52:57

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