Polarization in Disks

Ian Stephens; Zhi-Yun Li; Haifeng Yang; Akimasa Kataoka; Leslie W. Looney; Charles L. H. Hull; Manuel Fernández-López; Sarah I. Sadavoy; Woojin Kwon; Satoshi Ohashi; Ryo Tazaki; Dan Li; Thiem Hoang; Gesa H. -M. Bertrang; Carlos Carrasco-González; William R. F. Dent; Satoko Takahashi; Francesca Bacciotti; Felipe O. Alves; Josep M. Girart; Qizhou Zhang; Ramprasad Rao; Adriana Pohl; Marco Padovani; Daniele Galli; Chin-Fei Lee; Dominique M. Segura-Cox

arXiv · 1903.05478

Polarization in Disks

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Abstract

Polarized dust emission outside of disks reveal the magnetic field morphology of molecular clouds. Within disks, however, polarized dust emission can arise from very different mechanisms (e.g., self-scattering), and each of them are useful for constraining physical properties in the disk. For example, these mechanisms allow us to constrain the disk grain size distributions and grain/disk geometries, independent from current methods of measuring these parameters. To accurately model these features and disentangle the various polarization mechanisms, multiwavelength observations at very high resolution and sensitivity are required. With significant upgrades to current interferometric facilities, we can understand how grains evolve in disks during the planet formation process.

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Ian Stephens, Zhi-Yun Li, Haifeng Yang, Akimasa Kataoka, Leslie W. Looney, Charles L. H. Hull, Manuel Fernández-López, Sarah I. Sadavoy, Woojin Kwon, Satoshi Ohashi, Ryo Tazaki, Dan Li, Thiem Hoang, Gesa H. -M. Bertrang, Carlos Carrasco-González, William R. F. Dent, Satoko Takahashi, Francesca Bacciotti, Felipe O. Alves, Josep M. Girart, Qizhou Zhang, Ramprasad Rao, Adriana Pohl, Marco Padovani, Daniele Galli, Chin-Fei Lee, Dominique M. Segura-Cox. 2019-03-13. Polarization in Disks. https://arxiv.org/abs/1903.05478

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