Japan Geoscience Union Meeting 2015

Presentation information


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

[P-PS21] Planetary Sciences

Sun. May 24, 2015 2:15 PM - 4:00 PM A02 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Kosuke Kurosawa(Planetary Exploration Research Center, Chiba Institute of Technology), Keiko Hamano(Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo), Chair:Hiroshi Kobayashi(Department of Physics, Nagoya University), Sin-iti Sirono(Department of Earth and Planetary Sciences, Nagoya University)

3:00 PM - 3:15 PM

[PPS21-17] Gravitational instability by suppression of magnetic turbulence by electric-field heating

*Shoji MORI1, Satoshi OKUZUMI1 (1.Graduate School of Science, Tokyo Institute of Technology)

Keywords:protoplanetary disk, MHD, magnetorotaional instability, gravitational instability, accretion disk

Turbulence in protoplanetary disks is essential for disk evolution since the turbulence transport angular momentum outside and the gas falls into the central star. One of possible mechanism of generating the turbulence is magnetorotational instability (MRI; Balbus & Hawlley 1991). In a region far from the star where MRI fully develops, electric fields induced by MRI will heat up electrons (electric-field heating; Inutsuka & Sano, 2005). When the electric-field heating occurs, heated electrons tends to collide with and be captured by dust grains. Since number density of electrons decreases in the gas-phase, finally magnetic fields may disperse (Okuzumi & Inutsuka, 2015). For MRI, the dispersion of magnetic fields implies suppression of the magnetic turbulence. We have investigated where and how MRI turbulence is suppressed in protoplanetary disks so far. As a result, we have estimated the MRI turbulence is suppressed within approximately 100 AU on the mid-plane (electric-field heating region; the fall meeting of the Japanese Society for Planetary Sciences, 2014).

The purpose in this study is to investigate where the gas is accumulated in the disk considering electric-field heating.
In a vigorous turbulent region, the turbulence transports angular momentum of gas and the gas falls into the central star. On the other hand, in a weak turbulent region, accretion gas from outer disk is accumulated because of inefficiency of angular momentum transport. Therefore, the broad suppression of MRI turbulence will change the global disk structure of surface denaity(Mori & Okuzumi, in prep.). The fallen gas is accumulated in the inner region where MRI does not grow (dead zone; Gammie 1996), and the possibility is pointed out that gravitational instability occurs in the region. Considering the electric field heating of our study, the gas will be accumulated in broader region.

We calculated the relation between surface density and mass accretion rate at each place in disks. As our disk model, we set the disk containing 0.1 um-sized dust grain with dust-to-gas mass ratio of 0.01, and the gas pressure to the magnetic pressure on the mid-plane to be 104. As a result, with the mass accretion rate of 10-7M⦿ /yr, the surface density realizing the steady accretion does not exist within 70 AU from the central star. Comparing previous picture of dead zone that does not exist steady solution within 15 AU, we suggest that gas will be accumulated in considerably broad region. In such a region, the continuous gas accumulation increases surface density, and eventually the gravitational instability would occurs.