Polarization in Disks
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.
Cite
@article{arxiv.1903.05478,
title = {Polarization in Disks},
author = {Ian Stephens and Zhi-Yun Li and Haifeng Yang and Akimasa Kataoka and Leslie W. Looney and Charles L. H. Hull and Manuel Fernández-López and Sarah I. Sadavoy and Woojin Kwon and Satoshi Ohashi and Ryo Tazaki and Dan Li and Thiem Hoang and Gesa H. -M. Bertrang and Carlos Carrasco-González and William R. F. Dent and Satoko Takahashi and Francesca Bacciotti and Felipe O. Alves and Josep M. Girart and Qizhou Zhang and Ramprasad Rao and Adriana Pohl and Marco Padovani and Daniele Galli and Chin-Fei Lee and Dominique M. Segura-Cox},
journal= {arXiv preprint arXiv:1903.05478},
year = {2019}
}
Comments
Science white paper submitted to the Astro2020 Decadal Survey