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A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass ProtostarsModel Calculation

A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass Protostars: Model... [In this thesis, five low-mass protostellar sources are investigated with high angular-resolution observations with ALMA. The observational results are discussed in Chapters 4−8. The physical structure of the gas of each source are characterized with the aid of physical models. For the envelope components around the protostar, an infalling-rotating envelope model is prepared. The Keplerian disk model is employed for the disk components. The three dimensional velocity field in a disk/envelope system is calculated and projected onto the plane of the sky, and then compared with the observed kinematic structures of the gas. The model results are convolved with the intrinsic line width and the Gaussian beam for fair comparison with the observations. As for the outflow components, a parabolic model is employed. The details of these models are described in this chapter. Moreover, some representative examples of the model results are presented to demonstrate their dependences of the kinematic structure on the physical parameters.] http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png

A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass ProtostarsModel Calculation

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Publisher
Springer Nature Singapore
Copyright
© Springer Nature Singapore Pte Ltd. 2022
ISBN
978-981-19-1707-3
Pages
31 –50
DOI
10.1007/978-981-19-1708-0_3
Publisher site
See Chapter on Publisher Site

Abstract

[In this thesis, five low-mass protostellar sources are investigated with high angular-resolution observations with ALMA. The observational results are discussed in Chapters 4−8. The physical structure of the gas of each source are characterized with the aid of physical models. For the envelope components around the protostar, an infalling-rotating envelope model is prepared. The Keplerian disk model is employed for the disk components. The three dimensional velocity field in a disk/envelope system is calculated and projected onto the plane of the sky, and then compared with the observed kinematic structures of the gas. The model results are convolved with the intrinsic line width and the Gaussian beam for fair comparison with the observations. As for the outflow components, a parabolic model is employed. The details of these models are described in this chapter. Moreover, some representative examples of the model results are presented to demonstrate their dependences of the kinematic structure on the physical parameters.]

Published: Nov 9, 2022

Keywords: Protostellar disks; Jets and Outflows; Kinematics; Individual sources (L1527; TMC−1A)

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