| Name: Ribanda Marbaniang |
| Affiliation: Gauhati University |
| Conference ID: ASI2026_981 |
| Title: Disk Self-Gravity and the Global Response of Protoplanetary Disks Hosting Multiple Planets |
| Abstract Type: Poster |
| Abstract Category: Sun, Solar System, Exoplanets, and Astrobiology |
| Author(s) and Co-Author(s) with Affiliation: Ribanda Marbaniang(Gauhati University, Guwahati-781014, India), Dhritimaan Gogoi(Gauhati University, Guwahati-781014, India), Dhiraj Kumar Deka(Gauhati University, Guwahati-781014, India), Eeshankur Saikia(Gauhati University, Guwahati-781014, India) |
| Abstract: High resolution observations of protoplanetary disks reveal a wide variety of substructures, including gaps, rings, and non-axisymmetric features like vortices, which are commonly attributed to the presence of embedded planets. Although the interaction between a single planet and the surrounding disk is relatively well understood, recent numerical studies have shown that systems hosting multiple planets can produce wide and shallow gaps, long-lived vortices, and pronounced non-axisymmetric features. Despite this progress, the effects of disk self-gravity are often neglected in studies of multi-planet systems, even though young and massive disks are sufficiently self-gravitating for gravitational forces to influence wave propagation, torque exchange, and disk structure.
In this work, we investigate the role of disk self-gravity in shaping the substructures induced by multiple embedded planets in protoplanetary disks. Using two-dimensional hydrodynamical simulations, we explore the impact of disk self-gravity on the development of spiral density waves and the redistribution of material. We find that including self-gravity leads to a more pronounced global disk response, with stronger and more extended spiral features and enhanced radial perturbations in the azimuthally averaged surface density profiles compared to non-self-gravitating disks. These results suggest that disk self-gravity plays an important role in shaping the observable appearance of planet-hosting disks and contributes to the diversity of substructures seen in high-resolution observations. Accounting for self-gravity is therefore essential when interpreting disk morphologies and inferring planet properties from observed gaps and non-axisymmetric features.
Keywords: hydrodynamics — protoplanetary discs — planet–disc interactions — methods: numerical |
