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Unveiling the mid-plane temperature and mass distribution in the giant-planet formation zone

Published online by Cambridge University Press:  04 September 2018

Ke Zhang Open the ORCID record for Ke Zhang [Opens in a new window] ,
Edwin A. Bergin ,
Geoffrey A. Blake ,
L. Ilsedore Cleeves Open the ORCID record for L. Ilsedore Cleeves [Opens in a new window]  and
Kamber R. Schwarz
Ke Zhang
Affiliation:
Department of Astronomy, University of Michigan, 311 West Hall, 1085 S University Ave., Ann Arbor, MI 48109, USA email: [email protected]
Edwin A. Bergin
Affiliation:
Department of Astronomy, University of Michigan, 311 West Hall, 1085 S University Ave., Ann Arbor, MI 48109, USA email: [email protected]
Geoffrey A. Blake
Affiliation:
Division of Geological & Planetary Sciences, California Institute of Technology, MC 150-21, Pasadena, CA 91125, USA
L. Ilsedore Cleeves
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Kamber R. Schwarz
Affiliation:
Department of Astronomy, University of Michigan, 311 West Hall, 1085 S University Ave., Ann Arbor, MI 48109, USA email: [email protected]
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Abstract

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Core-accretion theory predicts that the formation of giant planets predominantly occurs at the dense mid-plane of the inner ∼50 AU of protoplanetary disks. However, due to observational limitation, this critical region remains to be the least charted area in protoplanetary disks. With its great sensitivity, ALMA recently started to image optically thin line emissions arisen from the mid-plane of the inner 50AU in nearby disks, which unlocks an exciting new path to directly constrain the physical properties of the giant planet formation zone through gas tracers. Here we present the first spatially resolved observations of the 13C18O J=3-2 line emission in the TW Hya disk. We show that this emission is optically thin even inside the CO mid-plane snowline. Combining it with the C18O J=3-2 images and the previously detected HD J=1-0 flux, we directly constrain the mid-plane temperature and optical depths of the CO gas and dust. We report a mid-plane CO snowline at 20.5 ± 1.3 AU, a mid-plane temperature distribution of 27+4−3×(R/20.5AU)-0.47+0.06−0.07 K, and a gas mass distribution of 13+8−5×(R/20.5AU)-0.9+0.4−0.3 g cm−2 between 5-20.5 AU in the TW Hya protoplanetary disk. We find a total gas/mm-sized dust mass ratio of 140 ± 40 in this region, suggesting that ∼2.4 earth mass of dust aggregates have grown to > cm sizes (and perhaps much larger).

Keywords

planet formationprotoplanetary disksastrochemistry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 103 - 108
Copyright
Copyright © International Astronomical Union 2018 

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