English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We have observed the Class 0 protostellar source IRAS 16293-2422 A in theC17O and H2CS lines as well as the 1.3 mm dust continuum with the Atacama LargeMillimeter/submillimeter Array at an angular resolution of ~0."1 (14 au). Thecontinuum emission of the binary component, Source A, reveals the substructureconsisting of 5 intensity peaks within 100 au from the protostar. The C17Oemission mainly traces the circummultiple structure on a 300 au scale centeredat the intensity centroid of the continuum, while it is very weak within theradius of 50 au from the centroid. The H2CS emission, in contrast, traces therotating disk structure around one of the continuum peaks (A1). Thus, it seemsthat the rotation centroid of the circummultiple structure is slightlydifferent from that of the disk around A1. We derive the rotation temperatureby using the multiple lines of H2CS. As approaching to the protostar A1, therotation temperature steeply rises up to 300 K or higher at the radius of 50 aufrom the protostar. It is likely due to a local accretion shock and/or thepreferential protostellar heating of the transition zone from thecircummultiple structure to the disk around A1. This position corresponds tothe place where the organic molecular lines are reported to be enhanced. Sincethe rise of the rotation temperature of H2CS most likely represents the rise ofthe gas and dust temperatures, it would be related to the chemicalcharacteristics of this prototypical hot corino.

Substructures in the Disk-Forming Region of the Class 0 Low-Mass Protostellar Source IRAS 16293-2422 Source A on a 10 au Scale