2004A&A...426..151A


Query : 2004A&A...426..151A

2004A&A...426..151A - Astronomy and Astrophysics, volume 426, 151-170 (2004/10-4)

ISO spectroscopy of disks around Herbig Ae/Be stars.

ACKE B. and VAN DEN ANCKER M.E.

Abstract (from CDS):

We have investigated the infrared spectra of all 46 Herbig Ae/Be stars for which spectroscopic data are available in the ISO data archive. Our quantitative analysis of these spectra focuses on the emission bands at 3.3, 6.2, ``7.7'', 8.6 and 11.2 micron, linked to polycyclic aromatic hydrocarbons (PAHs), the nanodiamond-related features at 3.4 and 3.5 micron, the amorphous 10 micron silicate band and the crystalline silicate band at 11.3 micron. We have detected PAH emission in 57% of the Herbig stars in our sample. Although for most of these sources the PAH spectra are similar, there are clear examples of differences in the PAH spectra within our sample which can be explained by differences in PAH size, chemistry and/or ionization. Amorphous silicate emission was detected in the spectra of 52% of the sample stars, amorphous silicate absorption in 13%. We have detected crystalline silicate emission in 11 stars (24% of our sample), of which four (9%) also display strong PAH emission. We have classified the sample sources according to the strength of their mid-IR energy distribution. The systems with stronger mid-infared (20-100µm) excesses relative to their near-infrared (1-5µm) excess display significantly more PAH emission than those with weaker mid-infrared excesses. There are no pronounced differences in the behaviour of the silicate feature between the two groups. This provides strong observational support for the disk models by Dullemond et al. (2001ApJ...560..957D), in which systems with a flaring disk geometry display a strong mid-infrared excess, whereas those with disks that are strongly shadowed by the puffed-up inner rim of the disk only display modest amounts of mid-infrared emission. Since the silicates are expected to be produced mainly in the warm inner disk regions, no large differences in silicate behaviour are expected between the two groups. In contrast to this, the PAH emission is expected to be produced mainly in the part of the disk atmosphere that is directly exposed to radiation from the central star. In this model, self-shadowed disks should display weaker PAH emission than flared disks, consistent with our observations.

Abstract Copyright:

Journal keyword(s): stars: circumstellar matter - stars: pre-main sequence - stars: planetary systems: protoplanetary disks

Simbad objects: 48

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Number of rows : 48
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* V376 Cas Ae* 00 11 26.5410514344 +58 50 03.929517960           A3/F2e 96 1
2 V* VX Cas Ae* 00 31 30.6818495040 +61 58 50.984946300 11.83 11.59 10.50 11.19 10.94 A0Vep 132 0
3 V* V892 Tau Ae* 04 18 40.6157618376 +28 19 15.625058880   16.6 14.69 14.35   A0Ve 291 0
4 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1034 2
5 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 494 0
6 V* UX Ori Ae* 05 04 29.9878898040 -03 47 14.286732072 10.25 10.93 8.70 9.62 9.43 A4IVe 359 1
7 V* V1366 Ori Ae* 05 16 00.4765181328 -09 48 35.393784012 10.19 10.16 9.84 9.77 9.63 B9.5V 202 0
8 HD 34700 SB* 05 19 41.4089390784 +05 38 42.778590864 9.75 9.778 9.659 9.205 8.47 G0IVe 98 0
9 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 106 0
10 V* BF Ori Ae* 05 37 13.2623828280 -06 35 00.568242528 10.37 10.00 9.69 10.06 9.31 A7III 289 0
11 V* RR Tau Ae* 05 39 30.5115918672 +26 22 26.967444996 11.64 12.09 11.28 10.58 10.17 A0:IVe 223 0
12 V* Z CMa Ae* 07 03 43.1599411656 -11 33 06.209065836 10.51 9.99 8.80     B5/8eq+F5/7 565 3
13 HD 95881 Em* 11 01 57.6218887080 -71 30 48.316074624   8.37 8.23     A0 98 0
14 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 531 0
15 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 264 1
16 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 770 1
17 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A0_sh 338 0
18 V* DK Cha TT* 12 53 17.2111480272 -77 07 10.736046012           F0e 138 0
19 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 439 1
20 HD 135344 * 15 15 48.9462675744 -37 08 55.731368400   7.84 7.76     A0V 140 1
21 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 197 0
22 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 518 0
23 HD 142666 TT* 15 56 40.0221861696 -22 01 40.005872148 9.41 9.37 8.82 8.31 8.01 F0V_sh 258 0
24 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 601 1
25 HD 144432 Ae* 16 06 57.9533126832 -27 43 09.760564056 8.47 8.53 8.19 7.82 7.53 A9/F0V 238 1
26 V* V856 Sco Ae* 16 08 34.2870044544 -39 06 18.325711332 7.66 7.41 7.05 6.92   A7IIIne_sh 384 0
27 WRAY 15-1484 Em* 16 27 15.1097295456 -48 39 26.852709060   14.706 13.782 13.388   B[e] 55 0
28 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 313 0
29 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 266 1
30 CD-42 11721 Be* 16 59 06.7629322176 -42 42 08.404228224 12.16 12.28 11.00     B0IVe 164 0
31 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 1031 0
32 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 420 2
33 EM* MWC 297 Ae* 18 27 39.5265500160 -03 49 52.133050776 15.57 14.34 12.31 11.34   B1.5Ve 289 0
34 V* VV Ser Ae* 18 28 47.8620017808 +00 08 39.923474964 12.99 12.63 11.80 11.01 10.24 A5Ve 246 0
35 V* R CrA Ae* 19 01 53.6764322232 -36 57 08.299341828 12.781 12.651 11.917 11.242 10.412 B5IIIpe 474 1
36 2MASS J19015545-3657231 Y*O 19 01 55.460 -36 57 23.13           ~ 93 2
37 V* T CrA Ae* 19 01 58.7902764120 -36 57 50.339720880     11.67     F0 164 0
38 HD 179218 Ae* 19 11 11.2538919456 +15 47 15.636008472 7.55 7.476 7.39 7.25 7.21 A0Ve 247 0
39 V* WW Vul Ae* 19 25 58.7494120560 +21 12 31.333658616 11.46 10.99 10.25 10.38 10.12 A2IVe 223 0
40 BD+40 4124 Ae* 20 20 28.2413946720 +41 21 51.529070088 11.11 11.36 10.62 10.510   B2Ve 289 1
41 EM* LkHA 224 Ae* 20 20 29.3503944888 +41 21 28.410038964 14.82 14.08 12.93 12.05 11.08 A4:Ve 100 0
42 EM* LkHA 225 Ae* 20 20 30.5955531672 +41 21 26.370826704   18.2 19.17     A4:Ve 82 0
43 V* PV Cep Or* 20 45 53.9540390184 +67 57 38.679941304   19.27 17.46 15.98 14.60 A5 266 3
44 HD 200775 Ae* 21 01 36.9205762896 +68 09 47.789578836 7.34 7.754 7.427 8.13   B2Ve 545 0
45 V* V645 Cyg Ae* 21 39 58.2745507632 +50 14 21.042184668   14.23 13.10 13.82   O6/9eq 264 0
46 BD+46 3471 Ae* 21 52 34.0992801288 +47 13 43.605617340 10.72 10.56 10.15     A0.5IIIer 210 1
47 V* SV Cep Ae* 22 21 33.2166238512 +73 40 27.097678812 11.40 11.25 10.35 10.28 10.08 A2IVe 129 0
48 EM* MWC 1080 Ae* 23 17 25.5895018656 +60 50 43.444557384   13.24 11.542     B0eq 320 0

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2023.06.03-15:45:54

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