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arXiv · 1801.04174

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
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Abstract

We have analyzed the OCS, H$_2$CS, CH$_3$OH, and HCOOCH$_3$ 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 H$_2$CS are extended with a slight rotation signature, while CH$_3$OH and HCOOCH$_3$ 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 with in 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.

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Yoko Oya, Kana Moriwaki, Shusuke Onishi, Nami Sakai, Ana López-Sepulcre, Cécile Favre, Yoshimasa Watanabe, Cecilia Ceccarelli, Bertrand Lefloch, Satoshi Yamamoto. 2018-01-12. Chemical and Physical Picture of IRAS 16293-2422 Source B at a Sub-arcsecond Scale Studied with ALMA. https://doi.org/10.3847/1538-4357%2Faaa6c7

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