Dust Resurgence in Protoplanetary Disks Due to Planetesimal–Planet Interactions

Abstract Observational data on the dust content of circumstellar disks show that the median dust content in disks around pre-main-sequence stars in nearby star-forming regions seems to increase from ∼1 to ∼2 Myr and then decline with time. This behavior challenges the models where the small dust gra...

Full description

Saved in:
Bibliographic Details
Published inAstrophysical journal. Letters Vol. 927; no. 2; p. L22
Main Authors Bernabò, Lia Marta, Turrini, Diego, Testi, Leonardo, Marzari, Francesco, Polychroni, Danai
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.03.2022
IOP Publishing
Subjects
Accretion disks
Circumstellar disks
Collision processes
Cosmic dust
Dust
Dust content
Planet formation
Planetary migration
Planetary system formation
Planetary-disk interactions
Planetesimals
Planets
Pre-main sequence stars
Protoplanetary disk
Protoplanetary disks
Star formation
Online AccessGet full text

Cover

More Information
Summary:Abstract Observational data on the dust content of circumstellar disks show that the median dust content in disks around pre-main-sequence stars in nearby star-forming regions seems to increase from ∼1 to ∼2 Myr and then decline with time. This behavior challenges the models where the small dust grains steadily decline by accumulating into larger bodies and drifting inwards on a short timescale (≤1 Myr). In this Letter we explore the possibility to reconcile this discrepancy in the framework of a model where the early formation of planets dynamically stirs the nearby planetesimals and causes high-energy impacts between them, resulting in the production of second-generation dust. We show that the observed dust evolution can be naturally explained by this process within a suite of representative disk-planet architectures.
Bibliography:AAS36364
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ac574e