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