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Title: PLANETARY SYSTEM FORMATION IN THE PROTOPLANETARY DISK AROUND HL TAURI

Abstract

We reprocess the Atacama Large Millimeter/Submillimeter Array (ALMA) long-baseline science verification data taken toward HL Tauri. Assuming the observed gaps are opened up by currently forming, unseen bodies, we estimate the mass of such hypothetical bodies based on the following two approaches: the Hill radius analysis and a more elaborate approach developed from the angular momentum transfer analysis in gas disks. For the former, the measured gap widths are used for estimating the mass of the bodies, while for the latter, the measured gap depths are utilized. We show that their masses are comparable to or less than the mass of Jovian planets. By evaluating Toomre’s gravitational instability (GI) condition and cooling effect, we find that the GI might be a mechanism to form the bodies in the outer region of the disk. As the disk might be gravitationally unstable only in the outer region of the disk, inward planetary migration would be needed to construct the current architecture of the observed disk. We estimate the gap-opening mass and show that type II migration might be able to play such a role. Combining GIs with inward migration, we conjecture that all of the observed gaps may be a consequence of bodies that might havemore » originally formed at the outer part of the disk, and have subsequently migrated to the current locations. While ALMA’s unprecedented high spatial resolution observations can revolutionize our picture of planet formation, more dedicated observational and theoretical studies are needed to fully understand the HL Tauri images.« less

Authors:
; ; ;  [1]
  1. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
Publication Date:
OSTI Identifier:
22521524
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 818; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANGULAR MOMENTUM TRANSFER; COMPARATIVE EVALUATIONS; COOLING; GRAVITATIONAL INSTABILITY; IMAGES; MASS; PLANETS; PROTOPLANETS; SPATIAL RESOLUTION; T TAURI STARS

Citation Formats

Akiyama, Eiji, Hasegawa, Yasuhiro, Hayashi, Masahiko, and Iguchi, Satoru. PLANETARY SYSTEM FORMATION IN THE PROTOPLANETARY DISK AROUND HL TAURI. United States: N. p., 2016. Web. doi:10.3847/0004-637X/818/2/158.
Akiyama, Eiji, Hasegawa, Yasuhiro, Hayashi, Masahiko, & Iguchi, Satoru. PLANETARY SYSTEM FORMATION IN THE PROTOPLANETARY DISK AROUND HL TAURI. United States. https://doi.org/10.3847/0004-637X/818/2/158
Akiyama, Eiji, Hasegawa, Yasuhiro, Hayashi, Masahiko, and Iguchi, Satoru. 2016. "PLANETARY SYSTEM FORMATION IN THE PROTOPLANETARY DISK AROUND HL TAURI". United States. https://doi.org/10.3847/0004-637X/818/2/158.
@article{osti_22521524,
title = {PLANETARY SYSTEM FORMATION IN THE PROTOPLANETARY DISK AROUND HL TAURI},
author = {Akiyama, Eiji and Hasegawa, Yasuhiro and Hayashi, Masahiko and Iguchi, Satoru},
abstractNote = {We reprocess the Atacama Large Millimeter/Submillimeter Array (ALMA) long-baseline science verification data taken toward HL Tauri. Assuming the observed gaps are opened up by currently forming, unseen bodies, we estimate the mass of such hypothetical bodies based on the following two approaches: the Hill radius analysis and a more elaborate approach developed from the angular momentum transfer analysis in gas disks. For the former, the measured gap widths are used for estimating the mass of the bodies, while for the latter, the measured gap depths are utilized. We show that their masses are comparable to or less than the mass of Jovian planets. By evaluating Toomre’s gravitational instability (GI) condition and cooling effect, we find that the GI might be a mechanism to form the bodies in the outer region of the disk. As the disk might be gravitationally unstable only in the outer region of the disk, inward planetary migration would be needed to construct the current architecture of the observed disk. We estimate the gap-opening mass and show that type II migration might be able to play such a role. Combining GIs with inward migration, we conjecture that all of the observed gaps may be a consequence of bodies that might have originally formed at the outer part of the disk, and have subsequently migrated to the current locations. While ALMA’s unprecedented high spatial resolution observations can revolutionize our picture of planet formation, more dedicated observational and theoretical studies are needed to fully understand the HL Tauri images.},
doi = {10.3847/0004-637X/818/2/158},
url = {https://www.osti.gov/biblio/22521524}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 818,
place = {United States},
year = {Sat Feb 20 00:00:00 EST 2016},
month = {Sat Feb 20 00:00:00 EST 2016}
}