Institute of Astronomy

Finding the water trail of the star and planet formation

SpeakerTalk DateTalk Series
Daniel Harsono (Leiden)29 August 2018Institute of Astronomy Seminars


Water is abundant in the solid phase prior to star formation as revealed
by ice absorption studies of embedded protostars. In contrast, water
toward Class II disks is significantly depleted. Since planets are
formed in those disks, it is crucial to understand how it is being
transported there from the large-scale envelope around protostars. Class
I protostellar systems have been shown to host well-defined Keplerian
disks on similar scales to that of Class II systems. Disks around Class
I sources thereby provide an interesting link to trace the water
evolution. We here present non-detections of spatially resolved warm
water lines toward four Class I protostars from the IRAM NOEMA and ALMA.
The stringent upper limits suggest that the chemical processing of
water due to grain growth and photodissociation are known to take place
in Class II disks, already start during the earlier embedded phases.
Deeper water line observations are required to further constrain the
dependence of the water vapor abundance on the physical structure of the
Class I disks.


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