2017A&A...597A.132K

Query : 2017A&A...597A.132K

2017A&A...597A.132K - Astronomy and Astrophysics, volume 597A132-132 (2017/1-1)

Radial decoupling of small and large dust grains in the transitional disk RX J1615.3-3255.

KOOISTRA R., KAMP I., FUKAGAWA M., MENARD F., MOMOSE M., TSUKAGOSHI T., KUDO T., KUSAKABE N., HASHIMOTO J., ABE L., BRANDNER W., BRANDT T.D., CARSON J.C., EGNER S.E., FELDT M., GOTO M., GRADY C.A., GUYON O., HAYANO Y., HAYASHI M., HAYASHI S.S., HENNING T., HODAPP K.W., ISHII M., IYE M., JANSON M., KANDORI R., KNAPP G.R., KUZUHARA M., KWON J., MATSUO T., McELWAIN M.W., MIYAMA S., MORINO J.-I., MORO-MARTIN A., NISHIMURA T., PYO T.-S., SERABYN E., SUENAGA T., SUTO H., SUZUKI R., TAKAHASHI Y.H., TAKAMI M., TAKATO N., TERADA H., THALMANN C., TOMONO D., TURNER E.L., WATANABE M., WISNIEWSKI J., YAMADA T., TAKAMI H., USUDA T., TAMURA M., CURRIE T., AKIYAMA E., MAYAMA S., FOLLETTE K.B. and NAKAGAWA T.

Abstract (from CDS):

We present H-band (1.6µm) scattered light observations of the transitional disk RX J1615.3-3255, located in the ∼1Myr old Lupus association. From a polarized intensity image, taken with the HiCIAO instrument of the Subaru Telescope, we deduce the position angle and the inclination angle of the disk. The disk is found to extend out to 68±12AU in scattered light and no clear structure is observed. Our inner working angle of 24AU does not allow us to detect a central decrease in intensity similar to that seen at 30AU in the 880µm continuum observations. We compare the observations with multiple disk models based on the spectral energy distribution (SED) and submm interferometry and find that an inner rim of the outer disk at 30AU containing small silicate grains produces a polarized intensity signal which is an order of magnitude larger than observed. We show that a model in which the small dust grains extend smoothly into the cavity found for large grains is closer to the actual H-band observations. A comparison of models with different dust size distributions suggests that the dust in the disk might have undergone significant processing compared to the interstellar medium.

Abstract Copyright: © ESO, 2017

Journal keyword(s): circumstellar matter - planet-disk interactions - planets and satellites: formation - protoplanetary disks

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 792 1
2 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 551 0
3 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 894 1
4 HD 135344B Or* 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 548 0
5 WRAY 15-1443 TT* 16 15 20.2341630672 -32 55 05.097631872 13.88 13.22 12.00 11.658 10.50 K5 120 0
6 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 293 1
7 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 535 0
8 HD 203856 * 21 23 35.5297279464 +40 01 07.023676800   7.33 7.21     A0V 85 0

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