2006A&A...456..535S


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.27CET03:22:29

2006A&A...456..535S - Astronomy and Astrophysics, volume 456, 535-548 (2006/9-3)

Analysis of the dust evolution in the circumstellar disks of T Tauri stars.

SCHEGERER A., WOLF S., VOSHCHINNIKOV N.V., PRZYGODDA F. and KESSLER-SILACCI J.E.

Abstract (from CDS):

We present a compositional analysis of 8-13µm spectra of 32 young stellar objects (YSOs). Our sample consists of 5 intermediate-mass stars and 27 low-mass stars. Although some previous studies give reasons for the similarity between the dust in circumstellar disks of TTauri stars and Herbig Ae/Be stars, a quantitative comparison has been lacking so far. Therefore, we include a discussion of the results of the 10µm spectroscopic survey of van Boekel et al. (2005A&A...437..189V), who focus on Herbig Ae/Be stars, the higher mass counterparts of TTauri stars, and draw comparisons to this and other studies. While the spectra of our 32 objects and first scientific results have already been published elsewhere we perform a more detailed analysis of the ∼10µm silicate feature. In our analysis we assume that this emission feature can be represented by a linear superposition of the wavelength-dependent opacity κabs(λ) describing the optical properties of silicate grains with different chemical composition, structure, and grain size. Determining an adequate fitting equation is another goal of this study. Using a restricted number of fitting parameters, we investigate which silicate species are necessary for the compositional fitting. Particles, with radii of 0.1µm- and 1.5µm and consisting of amorphous olivine and pyroxene, forsterite, enstatite, and quartz are considered. Only compact, homogeneous dust grains are used in the presented fitting procedures. In this context we show that acceptable fitting results can also be achieved if emission properties of porous silicate grains are considered instead. Our analysis shows - in terms of the properties of the circumstellar dust-like crystallinity - TTauri systems are a continuation of HAeBe systems at their lower mass end. However, a weak correlation between grain growth and stellar luminosity could be found, in contrast to HAeBe systems.

Abstract Copyright:

Journal keyword(s): astrochemistry - stars: pre-main sequence - infrared: stars - lines: profiles

Simbad objects: 35

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Number of rows : 35

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 ACO S 205 ClG 01 55 11 -58 32.3           ~ 6 0
2 V* RY Tau TT* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 639 1
3 V* GG Tau TT* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 634 1
4 V* AA Tau TT* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 609 0
5 EM* LkCa 15 TT* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 534 1
6 V* DQ Tau TT* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 283 0
7 V* DR Tau TT* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 464 0
8 V* GM Aur TT* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 540 0
9 V* SU Aur TT* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 527 0
10 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 383 0
11 V* GW Ori TT* 05 29 08.3925564419 +11 52 12.653756566   10.83 10.10 9.52   G5/8Ve 294 0
12 * tet01 Ori D Y*O 05 35 17.2574309230 -05 23 16.567215876 6.08 6.79 6.70 6.40 6.20 B1.5Vp 304 0
13 V* FU Ori FU* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 693 1
14 V* V646 Pup FU* 07 50 35.5923632458 -33 06 23.904713538           ~ 61 0
15 Hen 3-545 TT* 10 59 06.9712894449 -77 01 40.309036535   12.91 11.136   9.596 K4Ve 185 0
16 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1476 1
17 V* VW Cha TT* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 166 0
18 V* HP Cha Y*O 11 08 15.099 -77 33 53.16     13.3     K7V 97 0
19 PDS 47a Y*O 11 08 15.71 -77 33 53.1           K3.5 80 1
20 V* VZ Cha Or* 11 09 23.7736314968 -76 23 20.855918834   13.82 12.94   12.14 K7e 122 0
21 V* WW Cha Or* 11 10 00.0791962314 -76 34 57.971855660   14.74 14.10   10.95 K5 127 0
22 TWA 3 ** 11 10 27.894072 -37 31 51.96612   13.53 12.05 11.61 9.29 M4Ve+M4Ve 200 0
23 TWA 3A TT* 11 10 27.9117558304 -37 31 51.529219753   14.04 12.57   9.10 M4Ve 185 0
24 V* V1032 Cen TT* 14 08 10.1545137760 -41 23 52.576649494     12.199   10.506 K7IVe 83 0
25 THA 15-12 TT* 15 56 09.2067120748 -37 56 06.126159332   13.12 11.93 11.45   M0e 224 0
26 V* RU Lup TT* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 372 0
27 EM* AS 205 TT* 16 11 31.343 -18 38 26.00   13.98 12.63 12.81   K0e+K5e 236 0
28 GSS 31 TT* 16 26 23.3694945462 -24 20 59.580653864   15.9 14.70 14.33 11.53 K0e 132 1
29 Haro 1-16 TT* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 166 0
30 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 228 1
31 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 753 0
32 V* S CrA TT* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 258 0
33 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 216 0
34 V* WW Vul Ae* 19 25 58.7494596284 +21 12 31.333220807 11.46 10.99 10.25 10.38 10.12 A2IVe 214 0
35 HD 184761 PM* 19 34 58.9696800358 +27 13 31.222607898   7.00 6.73     A3 20 0

    Equat.    Gal    SGal    Ecl

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2020.01.27-03:22:29

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