Three-lane and multilane signatures of planets in planetesimal discs

Abstract

In massive numerical experiments we show that a planet embedded in a planetesimal disk induces a characteristic multi-lane "planetosignature" representing a pattern of several stellar-centric rings. If the planet's mass is large enough, the multi-lane signature degenerates to a three-lane one: then it consists of three rings, one bright coorbital with the planet, and two dark gaps in the radial distribution of the particles. The gaps correspond to orbital resonances 2:1 and 1:2 with the planet. This theoretical prediction may explain recent ALMA observations of the disk of HL Tau.

Habitability Properties of Circumbinary Planets

“…The co-orbital material may include any rocky objects of suitable masses; a particular class of such objects was considered as "Trojan exomoons" in Quarles et al (2012). The dynamical stability of the material co-orbital with the planet sharply increases if the host star is bi-nary (Demidova & Shevchenko, 2016).…”

Dynamical environments of relativistic binaries: The phenomenon of resonance shifting

“…Generally, circumbinary material is now routinely observed in the form of planets and disks [32,33]. Near-resonant circumbinary planets (CBPs) were identified [34,29], as well as resonant features in circumbinary disks; see, e.g., [35]. On the other hand, planetary systems of compact stars are known to be an ordinary phenomenon [33].…”

Catastrophic Events in Protoplanetary Disks and Their Observational Manifestations

“…The rings usually have fuzzy (blurred) boundaries. The origin of such structures is most often associated with disturbances that arise when planets interact with a protoplanetary disk (e.g., Ruge et al, 2013;van der Marel et al, 2015;Dong et al, 2015Dong et al, , 2017Dong et al, , 2018Demidova and Shevchenko, 2016;Jin et al, 2016;Bae et al, 2017). However, since no direct observational signs of the existence of planets in these disks were found, alternative models have also been considered (e.g., Banzatti et al, 2015;Zhang et al, 2015;Birnstiel et al, 2015;Okuzumi et al, 2016).…”