2009A&A...502L..17A


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.25CET14:31:09

2009A&A...502L..17A - Astronomy and Astrophysics, volume 502, L17-20 (2009/8-1)

On the interplay between flaring and shadowing in disks around Herbig Ae/Be stars.

ACKE B., MIN M., VAN DEN ANCKER M.E., BOUWMAN J., OCHSENDORF B., JUHASZ A. and WATERS L.B.F.M.

Abstract (from CDS):

Based on their spectral energy distribution, Herbig stars have been categorized into two observational groups, reflecting their overall disk structure: group I members have disks with a high degree of flaring as opposed to their group II counterparts. Literature results show that the structure of the disk is a strong function of the disk mass in µm-sized dust grains. We investigate the 5-35 µm Spitzer IRS spectra of a sample of 13 group I sources and 20 group II sources. We focus on the continuum emission to study the underlying disk geometry. We have determined the [30/13.5] and [13.5/7] continuum flux ratios. The 7-µm flux excess with respect to the stellar photosphere is measured, as a marker for the strength of the near-IR emission produced by the hot inner disk. We have compared our data to the spectra produced by self-consistent passive-disk models, for which the same quantities were derived. We confirm the results by Meijer et al. (2008A&A...492..451M) that the differences in continuum emission between group I and II sources can largely be explained by a difference in amount of small dust grains. However, we report a strong correlation between the [30/13.5] and [13.5/7] flux ratios for Meeus group II sources. Moreover, the [30/13.5] flux ratio decreases with increasing 7-µm excess for all targets in the sample. To explain these correlations with the models, we need to introduce an artificial scaling factor for the inner disk height. In roughly 50% of the Herbig Ae/Be stars in our sample, the inner disk must be inflated by a factor 2 to 3 beyond what hydrostatic calculations predict. The total disk mass in small dust grains determines the degree of flaring. We conclude, however, that for any given disk mass in small dust grains, the shadowing of the outer (tens of AU) disk is determined by the scale height of the inner disk (∼1AU). The inner disk partially obscures the outer disk, reducing the disk surface temperature. Here, for the first time, we prove these effects observationally.

Abstract Copyright:

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

Simbad objects: 33

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Number of rows : 33

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* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 951 2
2 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 411 0
3 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
4 HD 35187 Y*O 05 24 01.17261 +24 57 37.5791   8.79 8.71 8.72   A2e+A7 96 0
5 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 381 0
6 HD 244604 Or* 05 31 57.2512002483 +11 17 41.374206174   9.61 9.43     A0Vesh 61 0
7 HD 37258 Ae* 05 36 59.2489032761 -06 09 16.317559872   9.72 9.61 9.56   A3Ve 117 0
8 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
9 HD 37357 Ae* 05 37 47.0795535305 -06 42 30.203876953   8.96 8.85     A1V 98 0
10 HD 37411 Or* 05 38 14.5075249942 -05 25 13.317577897 10.03 9.91 9.79 9.60 9.45 hA3VakA0mA0(eb)_lB 84 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 HD 37806 Be* 05 41 02.2930276072 -02 43 00.729083804 7.67 7.93 7.90     B9/9.5II/III 143 0
13 HD 38120 Be* 05 43 11.8931815256 -04 59 49.881886291 9.08 9.10 9.1     B9Vnne 76 0
14 HD 250550 Ae* 06 01 59.9894900068 +16 30 56.724889160   9.60 9.593 9.64   B9e 234 1
15 HD 72106 ** 08 29 34.89852 -38 36 21.1321       9.32   A0IV 64 0
16 HD 85567 Be* 09 50 28.5375203189 -60 58 02.950579275 8.16 8.67 8.57     B5Vne 81 0
17 HD 95881 Em* 11 01 57.6212785173 -71 30 48.313329972   8.37 8.23     A0 90 0
18 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 467 0
19 HD 100453 Ae* 11 33 05.5765928993 -54 19 28.543792679   8.09 7.79     A9Ve 216 1
20 HD 101412 Be* 11 39 44.4562795603 -60 10 27.717502041   9.465 9.288     A3VaekA0mA0_lB 121 0
21 V* DX Cha Ae* 12 00 05.0870448690 -78 11 34.559255151   6.81 6.60     A0_sh 311 0
22 SS73 44 Ae* 15 03 23.7935361802 -63 22 58.878928904   13.88 12.75     Ae/B[e] 44 1
23 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 374 1
24 HD 139614 Ae? 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 167 0
25 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
26 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 503 1
27 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
28 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 244 1
29 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 352 2
30 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 231 0
31 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
32 HD 190073 Ae* 20 03 02.5098091524 +05 44 16.658081203 7.91 7.86 7.73   7.65 A2IVe 232 0
33 HD 203024 Y*O 21 16 03.0494926186 +68 54 52.100583837   9.02 8.86     A 47 1

    Equat.    Gal    SGal    Ecl

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2021.02.25-14:31:09

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