Chemical and Physical Picture of IRAS 16293-2422 Source B at a Sub-arcsecond Scale Studied with ALMA

Yoko Oya, Kana Moriwaki, Shusuke Onishi, Nami Sakai, Ana López-Sepulcre, Cécile Favre, Yoshimasa Watanabe, Cecilia Ceccarelli, Bertrand Lefloch, Satoshi Yamamoto

研究成果: Article査読

14 被引用数 (Scopus)

抄録

We have analyzed the OCS, H2CS, CH3OH, and HCOOCH3 data observed toward the low-mass protostar IRAS 16293-2422 Source B at a sub-arcsecond resolution with ALMA. A clear chemical differentiation is seen in their distributions; OCS and H2CS are extended with a slight rotation signature, while CH3OH and HCOOCH3 are concentrated near the protostar. Such a chemical change in the vicinity of the protostar is similar to the companion (Source A) case. The extended component is interpreted by the infalling-rotating envelope model with a nearly face-on configuration. The radius of the centrifugal barrier of the infalling-rotating envelope is roughly evaluated to be (30-50) au. The observed lines show the inverse P-Cygni profile, indicating the infall motion within a few 10 au from the protostar. The nearly pole-on geometry of the outflow lobes is inferred from the SiO distribution, and thus, the infalling and outflowing motions should coexist along the line of sight to the protostar. This implies that the infalling gas is localized near the protostar and the current launching points of the outflow have an offset from the protostar. A possible mechanism for this configuration is discussed.

本文言語English
論文番号96
ジャーナルAstrophysical Journal
854
2
DOI
出版ステータスPublished - 2018 2 20

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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