Document Type

Article

Publication Date

5-31-2019

Publication Title

Astrophysical Journal

Publisher

American Astronomical Society

Volume

877

Issue

2

First page number:

1

Last page number:

8

Abstract

We use two-dimensional Fourier transformation to measure the pitch angle () of the dominant spiral Fourier mode of well-defined spiral arms in 13 protoplanetary disks, making use of near-infrared scattered-light images of AB Aur, SAO 206462, MWC 758, V1247 Ori, HD 142527, DZ Cha, LkHα 330, and HD 100453, and ALMA millimeter continuum images of Elias 2-27, IM Lup, AS 205, and HT Lup. We find that the measured pitch angle correlates strongly with disk mass (M D ), such that more massive protoplanetary disks have smaller pitch angles, following . Interestingly, four disks with a known companion (HD 142527, HD 100453, AS 205, and HT Lup) share the same trend. Such a strong dependence of spiral arm pitch angle on disk mass suggests that the disk mass, independent of the formation mechanism, plays a fundamental role in determining the arm tightness of the observed spiral structure. The physical origin of the relation is still not clear. The pitch angle of spiral arms in protoplanetary disks provides an independent constraint on the disk mass.

Keywords

Circumstellar matter; Protoplanetary disk; Stars: protostars

Disciplines

Astrophysics and Astronomy | Cosmology, Relativity, and Gravity | Physical Processes

File Format

pdf

File Size

2.888 KB

Language

English

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