JpGU-AGU Joint Meeting 2017

Presentation information

[EJ] Oral

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS04] [EJ] New developments of planetary sciences with ALMA

Wed. May 24, 2017 9:00 AM - 10:30 AM A04 (Tokyo Bay Makuhari Hall)

convener:Munetake Momose(The College of Science, Ibaraki University), Hiroshi Kobayashi(Department of Physics, Nagoya University), Masumi Shimojo(National Astronomical Observatory of Japan), Hideko Nomura(Department of Earth and Planetary Sciences, Tokyo Institute of Technology), Chairperson:Munetake MOMOSE(The College of Science, Ibaraki University)

9:15 AM - 9:30 AM

[PPS04-02] millimeter-wave polarization as a tool of investigating the planet formation

★Invited papers

*Akimasa Kataoka1,3, Takashi Tsukagoshi2, Munetake Momose2, Hiroshi Nagai3, Takayuki Muto4, Cornelis Dullemond1, Adriana Pohl1,5, Misato Fukagawa6, Hiroshi Shibai7, Tomoyuki Hanawa8, Koji Murakawa9 (1.Heidelberg University, 2.Ibaraki Univerisity, 3.National Astronomical Observatory of Japan, 4.Kogakuin University, 5.Max-Planck Institute for Astronomy, 6.Nagoya University, 7.Osaka University, 8.Chiba University, 9.Osaka Sangyo University)

Keywords:protoplanetary disks, polarization, dust

Constraining the grain size in protoplanetary disks is a key to understand the first stage of planet formation. The grain size has been estimated by measuring the spectral index at millimeter wavelengths, while it has huge uncertainties. Here, we propose that millimeter-wave polarization is another method to constrain the grain size. We show that thermal dust emission is scattered off of other dust grains and the residual polarization is up to 2.5 %, which is detectable with ALMA. This self-scattering polarization is efficient only if the maximum grain size is comparable to the wavelengths. Therefore, we can constrain the grain size from millimeter-wave polarization of protoplanetary disks. Furthermore, we have observed the protoplanetary disk around HD 142527 with ALMA polarization mode, and found the evidence of the self-scattering plays a role in the protoplanetary disk. We will also discuss what is the essential observations to distinguish the mechanisms between the self-scattering and magnetic field alignment and what is needed for future observations.