Planetary System Formation in Protoplanetary Disk around HL Tauri
Eiji Akiyama, Yasuhiro Hasegawa, Masahiko Hayashi, Satoru Iguchi

TL;DR
This study re-analyzes high-resolution ALMA data of HL Tauri, confirming multiple disk gaps and exploring their possible origins, including gravitational instability and planetary migration, to understand early planet formation processes.
Contribution
It introduces new mass estimation methods for potential forming bodies in the disk and discusses their possible formation via gravitational instability and inward migration.
Findings
Gaps are likely caused by bodies with masses comparable to Jovian planets.
Gravitational instability may form bodies in the outer disk region.
Inward planetary migration could explain current gap locations.
Abstract
We re-process the Atacama Large Millimeter/Submillimeter Array (ALMA) long-baseline science verification data taken toward HL Tauri. As shown by the previous work, we confirm that the high spatial resolution (~ 0."019, corresponding to ~ 2.7 AU) dust continuum images at \lambda = 0.87, 1.3, and 2.9 mm exhibit a multiple ring-like gap structure in the circumstellar disk. Assuming that the observed gaps are opened up by currently forming, unseen bodies, we estimate the mass of such hypothetical bodies based on following two approaches; the Hill radius analysis and a more elaborated approach developed from the angular momentum transfer analysis in gas disks. For the former, the measured gap widths are used for calibrating the mass of the bodies, while for the latter, the measured gap depths are utilized. We show that their masses are likely comparable to or less than the mass of Jovian…
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