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


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.20CEST02:31:58

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 - 2021
#notes
1 V* V376 Cas Ae* 00 11 26.5610557523 +58 50 03.750169804           A3/F2e 95 1
2 V* VX Cas Ae* 00 31 30.6816836826 +61 58 50.982831889 11.83 11.59 10.50 11.19 10.94 A0Vep 128 0
3 V* V892 Tau Ae* 04 18 40.6120892867 +28 19 15.641672501   16.6 14.69 14.35   A0Ve 271 0
4 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 953 2
5 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 413 0
6 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 339 1
7 V* V1366 Ori Ae* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 168 0
8 HD 34700 TT* 05 19 41.4088548858 +05 38 42.777125431 9.75 9.788 9.15 8.80 8.47 G0IVe 75 0
9 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 97 0
10 V* BF Ori Ae* 05 37 13.2623698298 -06 35 00.565420577 10.37 10.00 9.69 10.06 9.31 A7III 272 0
11 V* RR Tau Ae* 05 39 30.5114685049 +26 22 26.961204895 11.64 12.09 11.28 10.58 10.17 A0:IVe 217 0
12 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 537 3
13 HD 95881 Em* 11 01 57.6212785173 -71 30 48.313329972   8.37 8.23     A0 90 0
14 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 470 0
15 HD 100453 Ae* 11 33 05.5765928993 -54 19 28.543792679   8.09 7.79     A9Ve 218 1
16 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 673 1
17 V* DX Cha Ae* 12 00 05.0870448690 -78 11 34.559255151   6.81 6.60     A0_sh 312 0
18 V* DK Cha Or* 12 53 17.2028372976 -77 07 10.727661977           F0 132 0
19 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 375 1
20 HD 135344 * 15 15 48.9457954324 -37 08 55.727525343   7.84 7.76     A0V 130 1
21 HD 139614 Ae? 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 168 0
22 HD 141569 Y*O 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 480 0
23 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 225 0
24 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 510 1
25 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 218 1
26 V* V856 Sco Ae* 16 08 34.2868591379 -39 06 18.326059778 7.66 7.41 7.05 6.92   A7IIIne_sh 359 0
27 WRAY 15-1484 Em* 16 27 15.1095981539 -48 39 26.849684049   14.6 13.7     B[e] 52 0
28 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 296 0
29 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 244 1
30 CD-42 11721 Be* 16 59 06.7622892572 -42 42 08.404916931 12.16 12.28 11.00     B0IVe 156 1
31 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 851 0
32 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 353 2
33 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 271 0
34 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 232 0
35 V* R CrA Ae* 19 01 53.6850227874 -36 57 08.145519972 12.781 12.651 11.917 11.242 10.412 B5IIIpe 456 1
36 2MASS J19015545-3657231 Y*O 19 01 55.460 -36 57 23.13           ~ 91 2
37 V* T CrA Ae* 19 01 58.7901571143 -36 57 50.329832417     11.67     F0 157 0
38 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 225 0
39 V* WW Vul Ae* 19 25 58.7494596284 +21 12 31.333220807 11.46 10.99 10.25 10.38 10.12 A2IVe 216 0
40 BD+40 4124 Ae* 20 20 28.2415737117 +41 21 51.527810947 11.11 11.36 10.62 10.510   B2Ve 279 1
41 EM* LkHA 224 Ae* 20 20 29.3500765489 +41 21 28.448014439 14.82 14.08 12.93 12.05 11.08 A4:Ve 92 0
42 EM* LkHA 225 Ae* 20 20 30.5937486026 +41 21 26.337058307   18.2 19.17     A4:Ve 73 0
43 V* PV Cep Or* 20 45 53.9537161790 +67 57 38.678052612   19.27 17.46 15.98 14.60 A5 255 3
44 HD 200775 Ae* 21 01 36.9184805541 +68 09 47.770037306 7.34 7.754 7.427 8.13   B2Ve 519 0
45 V* V645 Cyg Ae* 21 39 58.2775729406 +50 14 21.002745087   14.23 13.10 13.82   O6/9eq 256 0
46 BD+46 3471 Ae* 21 52 34.0992388111 +47 13 43.600551484 10.72 10.56 10.15     A0.5IIIer 198 1
47 V* SV Cep Ae* 22 21 33.2175224577 +73 40 27.096415978 11.40 11.25 10.35 10.28 10.08 A2IVe 124 0
48 EM* MWC 1080 Ae* 23 17 25.5890248379 +60 50 43.452566559   13.24 11.542     B0eq 310 0

    Equat.    Gal    SGal    Ecl

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2021.04.20-02:31:58

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