3 years ago

SMA and ALMA Studies of Disk- and Planet Formation around Low-mass Protostars.

Naomi Hirano, Hauyu Baobab Liu, Pin-Gao Gu, Nagayoshi Ohashi, Shigehisa Takakuwa, Chin-Fei Lee, Masao Saito, Yuri Aikawa, Yusuke Aso, Ruben Krasnopolsky, Kengo Tomida, Ti-Lin Chou, Patrick M. Koch, Kohji Tomisaka, Evaria Puspitaningrum, Kazuya Saigo, Hsi-Wei Yen, Masahiro N. Machida, Paul T. P. Ho

We report our current SMA and ALMA studies of disk and planet formation around protostars. We have revealed that $r \gtrsim$100 AU scale disks in Keplerian rotation are ubiquitous around Class I sources. These Class I Keplerian disks are often embedded in rotating and infalling protostellar envelopes. The infalling speeds of the protostellar envelopes are typically $\sim$ 3-times smaller than the free-fall velocities, and the rotational profiles follow the $r^{-1}$ profile, that is, rotation with the conserved specific angular momentum. Our latest high-resolution ($\sim$0$\farcs$5) ALMA studies, as well as the other studies in the literature, have unveiled that $r \sim$100-AU scale Keplerian disks are also present in several Class 0 protostars, while in the other Class 0 sources the inferred upper limits of the Keplerian disks are very small ($r \lessim$20 AU). Our recent data analyses of the ALMA long baseline data of the Class I-II source HL Tau have revealed gaps in molecular gas as well as in dust in the surrounding disk, suggesting the presence of sub-Jovian planets in the disk. These results imply that disk and planet formation should be completed in the protostellar stage.

Publisher URL: http://arxiv.org/abs/1711.00447

DOI: arXiv:1711.00447v1

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