American Astronomical Society
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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.
Circumstellar matter; Protoplanetary disk; Stars: protostars
Astrophysics and Astronomy | Cosmology, Relativity, and Gravity | Physical Processes
Ho, L. C.,
A Tight Relation between Spiral Arm Pitch Angle and Protplanetary Disk Mass.
Astrophysical Journal, 877(2),
American Astronomical Society.