2013ApJ...771...48T


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.07CET12:17:39

2013ApJ...771...48T - Astrophys. J., 771, 48 (2013/July-1)

Modeling the resolved disk around the class 0 protostar L1527.

TOBIN J.J., HARTMANN L., CHIANG H.-F., WILNER D.J., LOONEY L.W., LOINARD L., CALVET N. and D'ALESSIO P.

Abstract (from CDS):

We present high-resolution sub/millimeter interferometric imaging of the Class 0 protostar L1527 IRS (IRAS 04368+2557) at λ = 870 µm and 3.4 mm from the Submillimeter Array and Combined Array for Research in Millimeter Astronomy. We detect the signature of an edge-on disk surrounding the protostar with an observed diameter of 180 AU in the sub/millimeter images. The mass of the disk is estimated to be 0.007 M, assuming optically thin, isothermal dust emission. The millimeter spectral index is observed to be quite shallow at all the spatial scales probed: α ∼ 2, implying a dust opacity spectral index β ∼ 0. We model the emission from the disk and surrounding envelope using Monte Carlo radiative transfer codes, simultaneously fitting the sub/millimeter visibility amplitudes, sub/millimeter images, resolved L' image, spectral energy distribution, and mid-infrared spectrum. The best-fitting model has a disk radius of R = 125 AU, is highly flared (H∝R 1.3), has a radial density profile ρ∝R –2.5, and has a mass of 0.0075 M. The scale height at 100 AU is 48 AU, about a factor of two greater than vertical hydrostatic equilibrium. The resolved millimeter observations indicate that disks may grow rapidly throughout the Class 0 phase. The mass and radius of the young disk around L1527 are comparable to disks around pre-main-sequence stars; however, the disk is considerably more vertically extended, possibly due to a combination of lower protostellar mass, infall onto the disk upper layers, and little settling of ∼1 µm-sized dust grains.

Abstract Copyright:

Journal keyword(s): ISM: individual: L1527 - protoplanetary disks - stars: formation

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3467 3
2 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 373 3
3 IRAS 03407+3152 cor 03 43 56.52 +32 00 52.8           ~ 288 0
4 QSO B0400+258 QSO 04 03 05.58606763 +26 00 01.5028075     18 19.00   ~ 176 1
5 IRAS 04016+2610 Y*O 04 04 43.071 +26 18 56.39     20.45     ~ 229 0
6 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 841 1
7 V* HL Tau TT* 04 31 38.437 +18 13 57.65   16.02 15.10 14.21   K5 1135 0
8 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
9 IRAS 04302+2247 Y*O 04 33 16.501 +22 53 20.40           ~ 131 0
10 NAME Per B AGN 04 37 04.37510272 +29 40 13.8184969   21.7       ~ 458 2
11 IRAS 04368+2557 Y*O 04 39 53.86 +26 03 09.7           ~ 227 0
12 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3333 0
13 LDN 1439 DNe 05 00 09 +52 04.9           ~ 76 0
14 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2641 2
15 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 886 2
16 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 230 2
17 LDN 663 DNe 19 36 55 +07 34.4           ~ 538 0
18 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 463 0

    Equat.    Gal    SGal    Ecl

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2019.12.07-12:17:39

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