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Tracing the physical conditions of planet formation with molecular excitation

Published online by Cambridge University Press:  12 October 2020

Richard Teague Open the ORCID record for Richard Teague [Opens in a new window]
Richard Teague*
Affiliation:
Department of Astronomy, University of Michigan, 1085 S. University Ave., Ann Arbor, MI48109, USA email: [email protected]
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Abstract

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Understanding the physical structure of the planet formation environment, the protoplanetary disk, is essential for the interpretation of high resolution observations of the dust and future observations of the magnetic field structure. Observations of multiple transitions of molecular species offers a unique view of the underlying physical structure through excitation analyses. Here we describe a new method to extract high-resolution spectra from low-resolution observations, then provide two case studies of how molecular excitation analyses were used to constrain the physical structure in TW Hya, the closest protoplanetary disk to Earth.

Keywords

astrochemistrytechniques: radar astronomyplanets and satellites: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 181 - 186
Copyright
© International Astronomical Union 2020

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