2015A&A...582L...7C


Query : 2015A&A...582L...7C

2015A&A...582L...7C - Astronomy and Astrophysics, volume 582, L7-7 (2015/10-1)

Nonazimuthal linear polarization in protoplanetary disks.

CANOVAS H., MENARD F., DE BOER J., PINTE C., AVENHAUS H. and SCHREIBER M.R.

Abstract (from CDS):

Several studies discussing imaging polarimetry observations of protoplanetary disks use the so-called radial Stokes parameters Qφ and Uφ to discuss the results. This approach has the advantage of providing a direct measure of the noise in the polarized images under the assumption that the polarization is only azimuthal, i.e., perpendicular to the direction toward the illuminating source. However, a detailed study of the validity of this assumption is currently missing. We aim to test whether departures from azimuthal polarization can naturally be produced by scattering processes in optically thick protoplanetary disks at near infrared wavelengths. We use the radiative transfer code MCFOST to create a generic model of a transition disk using different grain size distributions and dust masses. From these models we generate synthetic polarized images at 2.2µm. We find that even for moderate inclinations (e.g., i=40°), multiple scattering alone can produce significant (up to ∼4.5% of the Qφ image, peak-to-peak) nonazimuthal polarization reflected in the Uφ images. We also find that different grain populations can naturally produce radial polarization (i.e., negative values in the Qφ images). Despite the simplifications of the models, our results suggest that caution is recommended when interpreting polarized images by only analyzing the Qφ and Uφ images. We find that there can be astrophysical signal in the Uφ images and negative values in the Qφ images, which indicate departures from azimuthal polarization. If significant signal is detected in the Uφ images, we recommend checking the standard Q and U images to look for departures from azimuthal polarization. On the positive side, signal in the Uφ images once all instrumental and data-reduction artifacts have been corrected for means that there is more information to be extracted regarding the dust population and particle density.

Abstract Copyright:

Journal keyword(s): scattering - techniques: polarimetric - circumstellar matter - stars: variables: T Tauri, Herbig Ae/Be

Simbad objects: 6

goto Full paper

goto View the references in ADS

Number of rows : 6
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 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3747 0
2 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 961 2
3 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 569 1
4 THA 15-20 TT* 16 07 11.5876160594 -39 03 47.490881982   16.25 14.58 14.11 12.92 M0.5 83 0
5 2MASS J16335560-2442049 Y*O 16 33 55.6149601032 -24 42 05.006785530           K7 44 0
6 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 241 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2015A&A...582L...7C and select 'bookmark this link' or equivalent in the popup menu


2021.07.30-00:53:19

© Université de Strasbourg/CNRS

    • Contact