Catastrophic events in protoplanetary

disks and their observational

manifestations

Tatiana Demidova

Crimean astrophysical observatory of RAS Vladimir Grinin

Central Astronomical Observatory of RAS

St Petersburg University

HD 135344B, Cazzoletti et al., 2018 HD 143006, Perez et al., 2018

RXJ 1615, Avenhaus et al., 2018 HD 163296, Huang et al., 2018

HD 169142 HD 97048 RU Lup

Elias 24 AS 209 GW Lup

Model

0.48 AU

10 µm, 100 µm, 1 mm

Mw = 4 · 1025 g, Ve = 50±50 m s-1

Jackson & Wyatt 2012; Genda et al. 2015

Protoplanetary disk

(Dutrey et al. 1994; Chiang & Goldreich 1997; Dullemond & Dominik 2004).

Main equations for gas and dust

g

Method SPH (Lucy,1977; Gingold & Monaghan, 1977)

Smoothed value Interpolation sum

Derivative

Kernel properties

h — smoothing lenght

Interpolation kernel

q = r/h Laibe & Price (2014)

Dust simulation

Gas simulation

GADGET-2 (Springel, 2010)

http://www.mpa-garching.mpg.de/gadget/

modified by Demidova (2016)

Results of simulation

Disk images at wavelength 1.3 mm (RADMC-3D http://www.ita.uni-heidelberg.de/~dullemond/software/radmc-3d/)

Collision of planetesimals is a natural process for protoplanetary disks (Meng et al., 2014;

Genda et al., 2015);

The planet may contribute to the ejection of planetesimals to the periphery of the disk

(Batygin & Morbidelli, 2013; Morrison & Malhotra, 2015);

The initial mass of the colliding bodies can be 10 times less than the mass of the clump;

Events in the Solar system: the formation of the Moon (Cameron & Ward, 1976),

formation of the Pluto-Charon system (Canup 2005, Stern et al., 2006), inclination of the

axis of Uranus (Slattery et al. 1992) could be the consequences of a catastrophic

collision;

Large emission of dust in the protoplanetary disk is possible with the destruction of the

planet (Nayakshin et al. 2020).

Justification of the model