# 2009A&A...501..609H

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 Query : 2009A&A...501..609H

2009A&A...501..609H - Astronomy and Astrophysics, volume 501, 609-617 (2009/7-2)

An ISO/SWS study of the dust composition around S stars. A novel view of S-star dust.

HONY S., HERAS A.M., MOLSTER F.J. and SMOLDERS K.

Abstract (from CDS):

We investigate the composition of the solid-state materials in the winds around S-type AGB stars. The S stars produce dust in their wind that bears a resemblance to the dust produced in some O-rich AGB stars. However, the reported resemblance is mostly based on IRAS/LRS spectra with limited spectral resolution, sensitivity, and wavelength coverage. We investigate the dust composition around S stars using ISO/SWS data that surpass the previous studies in terms of spectral resolution and wavelength coverage. We selected the dust producing S stars in the ISO/SWS archive with enough signal to perform a detailed dust analysis, and then compare the dust spectra from the 9 sources with the O-rich AGB spectra and a subset of M super-giants. We constructed average dust emission spectra of the different categories. We report the discovery of several previously unreported dust emission features in the S star spectra. The long wavelength spectra of W Aql and π1 Gru exhibit the 30'' µm feature attributed to MgS. Two sources exhibit a series of emission bands between 20 and 40µm that we tentatively ascribe to Diopside. We show that the 10-20µm spectra of the S stars are significantly different from the O-rich AGB stars. The O-rich stars exhibit a structured emission feature that is believed to arise from amorphous silicate and aluminium-oxide. The S stars lack the substructure found in the O-rich stars. Instead they show a smooth peak with a varying peak-position from source to source. We suggest that this feature is caused by a family of related materials, whose exact composition determines the peak position. The observed trend mimics the laboratory trend of non-stoichiometric silicates. In this scenario the degree of non-stoichiometry is related to the Mg to SiO4 ratio, in other words, to the amount of free O available during the dust grain growth.

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

Full paper

 Number of rows : 37
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* W Cet S* 00 02 07.3899783984 -14 40 33.032623080 16.64 16.09 14.46 9.14 5.38 S5.5-7/1.5-3e 83 0
2 V* T Cet S* 00 21 46.2731778 -20 03 28.884826   7.32 5.74     M5-6Se 144 0
3 V* R And S* 00 24 01.9457463096 +38 34 37.370144352 10.61 9.36 7.39 4.45 2.30 S5-7/4-5e 346 0
4 V* RW And S* 00 47 18.9203868696 +32 41 08.247572160   12.78 11.79 10.66   S6/2e 84 0
5 V* S Cas S* 01 19 41.9796588720 +72 36 40.850697240           S3-54-8 120 1
6 V* KK Per s*r 02 10 15.7846748496 +56 33 32.663347416 12.32 9.96 7.74 5.86 4.29 M2Iab-Ib 104 0
7 NGC 869 OpC 02 18 58 +57 08.0           ~ 463 0
8 V* V605 Cas s*r 02 20 22.4632763112 +59 40 16.904099784 13.41 10.80 8.36 6.42 4.85 M2Iab 67 0
9 V* AD Per s*r 02 20 29.0035384536 +56 59 35.239755912 12.70 10.16 7.8490   7.1111 M3Iab 125 1
10 NGC 884 OpC 02 22 20 +57 08.9           ~ 477 0
11 V* RR Per Mi* 02 28 29.4075457320 +51 16 17.281798176       13.09   M6.5e: 76 0
12 LEE 259 C* 03 26 29.5037418864 +47 31 48.551540844       10.70   N 173 0
13 V* WX Cam S* 03 49 03.7421392032 +53 10 59.132001396   12.67 10.18     S5/5.5 35 0
14 V* NO Aur s*r 05 40 42.0497751264 +31 55 14.197536156 10.52 8.30 6.21 4.43 3.02 M2Iab 141 1
15 V* R Hya Mi* 13 29 42.7801586466 -23 16 52.751628992 7.26 6.58 4.97 2.27 -0.15 M6-9e 475 0
16 V* LY Mus Sy* 13 41 13.5903837744 -71 52 05.761119720   8.73 6.97     S6,2 35 0
17 WOS 48 C* 15 23 05.0730770544 -51 25 58.762691652   17.85 16.66 14.51 10.18 C 129 1
18 V* ST Her S* 15 50 46.6232210160 +48 28 58.850853780   9.09 7.75     M6S-M7SIII: 160 0
19 V* TY Dra LP* 17 37 00.1116207432 +57 44 25.309145436   10.61 9.30     M8 52 0
20 V* OP Her S* 17 56 48.5269765296 +45 21 03.060662328 9.45 7.93 6.32 4.15 2.25 M6S 148 0
21 HD 165774 S* 18 09 17.1822535392 -36 57 57.598152480   9.86 8.17     S4,6 25 0
22 V* R Aql OH* 19 06 22.2510922392 +08 13 48.012661776 8.06 7.69 6.09     M6.5-9e 552 2
23 V* S Lyr S* 19 13 11.8046954880 +26 00 27.853438788       11.35   SC 73 0
24 V* W Aql S* 19 15 23.3572741560 -07 02 50.333886492   12.72 10.14 10.21   S6/6e 224 0
25 V* R Cyg S* 19 36 49.3579856496 +50 11 59.727536988   9.96 6.10 8.96 6.447 S4-8/6e 270 1
26 * chi Cyg S* 19 50 33.9213430345 +32 54 50.575531294 7.02 6.06 4.24 1.81 -0.01 S6-9/1-2e 683 0
27 V* AA Cyg S* 20 04 27.6062351064 +36 49 00.458592240   10.93 8.79     S6/3 90 0
28 V* RZ Sgr S* 20 15 28.4023889376 -44 24 37.478466072   11.21 10.40     S4,4ep 72 0
29 BD+35 4077 s?r 20 21 14.0683222872 +35 37 16.559940720 14.72 12.65 9.72 6.83 4.65 M3Iab: 48 0
30 IRC +40427 s*r 20 31 28.6960739064 +40 38 43.423540872     11.4     M0/2I 27 0
31 CIT 11 s*r 20 39 36.5223205248 +39 12 09.688510872     13.8 13.24   M2/4I 35 1
32 * pi.01 Gru S* 22 22 44.2083897000 -45 56 52.791160956 10.52 8.62 6.55 3.19 0.52 S5,7: 181 0
33 V* V354 Cep LP* 22 33 34.6356348888 +58 53 47.124005640   13.71 10.90     M3.5Ib 27 1
34 V* RX Lac S* 22 49 56.8993161696 +41 03 04.307827176   10.11 8.62     S7.5/1e 51 0
35 V* HR Peg S* 22 54 35.6272159944 +16 56 30.606025560 9.970 8.160 6.360     S4+/1+ 129 0
36 * 57 Peg S* 23 09 31.4573825 +08 40 37.763634   6.48 5.14     M4S 126 0
37 V* V582 Cas Mi* 23 30 11.2241389920 +60 16 45.407772264     11.81 10.84   M4I 32 0

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2023.02.09-09:36:24