# 2013A&A...555A..64M

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 Query : 2013A&A...555A..64M

2013A&A...555A..64M - Astronomy and Astrophysics, volume 555A, 64-64 (2013/7-1)

Identifying gaps in flaring Herbig Ae/Be disks using spatially resolved mid-infrared imaging. Are all group I disks transitional?

MAASKANT K.M., HONDA M., WATERS L.B.F.M., TIELENS A.G.G.M., DOMINIK C., MIN M., VERHOEFF A., MEEUS G. and VAN DEN ANCKER M.E.

Abstract (from CDS):

The evolution of young massive protoplanetary disks toward planetary systems is expected to correspond to structural changes in observational appearance, which includes the formation of gaps and the depletion of dust and gas. A special group of disks around Herbig Ae/Be stars do not show prominent silicate emission features, although they still bear signs of flaring disks, the presence of gas, and small grains. We focus our attention on four key Herbig Ae/Be stars to understand the structural properties responsible for the absence of silicate feature emission. We investigate Q- and N-band images taken with Subaru/COMICS, Gemini South/T-ReCS, and VLT/VISIR. We perform radiative transfer modeling to examine the radial distribution of dust and polycyclic aromatic hydrocarbons (PAHs). Our solutions require a separation of inner- and outer- disks by a large gap. From this, we characterize the radial density structure of dust and PAHs in the disk. The inner edge of the outer disk has a high surface brightness and a typical temperature between ∼100-150 K and therefore, dominates the emission in the Q-band. All four disks are characterized by large gaps. We derive radii of the inner edge of the outer disk of 34+4–4, 23+3–5, 30+5–3 and 63+4–4AU for HD97048, HD169142, HD135344B, and Oph IRS 48, respectively. For HD 97048 this is the first detection of a disk gap. The large gaps deplete the entire population of silicate particles with temperatures suitable for prominent mid-infrared feature emission, while small carbonaceous grains and PAHs can still show prominent emission at mid-infrared wavelengths. The continuum emission in the N-band is not due to emission in the wings of PAHs. This continuum emission can be due to very small grains or to thermal emission from the inner disk. We find that PAH emission is not always dominated by PAHs on the surface of the outer disk. The absence of silicate emission features is due to the presence of large gaps in the critical temperature regime. Many, if not all Herbig disks with spectral energy distribution classification group I'', are disks with large gaps and can be characterized as (pre-) transitional. An evolutionary path from the observed group I to the observed group II sources seems no longer likely. Instead, both might derive from a common ancestor.

Journal keyword(s): protoplanetary disks - circumstellar matter - planet-disk interactions - stars: variables: T Tauri, Herbig Ae/Be - stars: pre-main sequence

VizieR on-line data: <Available at CDS (J/A+A/555/A64): table1.dat tablea1.dat tablea2.dat tablea3.dat tablea4.dat refs.dat>

Full paper

 Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 996 2
2 HD 31648 Ae* 04 58 46.2655706952 +29 50 36.987625680 7.84 7.78 7.62 7.76 7.43 A5Vep 463 0
3 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 805 0
4 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 283 0
5 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 602 1
6 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 501 0
7 * gam Cru PM* 12 31 09.95961 -57 06 47.5684 5.01 3.23 1.64 -0.02 -1.44 M3.5III 269 0
8 * alf Cen ** 14 39 29.71993 -60 49 55.9990   0.4 -0.1     G2V+K1V 890 0
9 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 415 1
10 HD 135344 * 15 15 48.9462675744 -37 08 55.731368400   7.84 7.76     A0V 137 1
11 IRAS 16245-2423 TT* 16 27 37.1906433768 -24 30 35.025246828       16.66 14.67 B5-F2 265 0
12 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 391 2
13 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1185 3

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2022.08.12-08:43:34

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