# Linear Analysis of the Nonaxisymmetric Secular Gravitational Instability

## TL;DR

This paper conducts a linear analysis of nonaxisymmetric secular gravitational instability in protoplanetary disks, revealing transient growth of perturbations that can influence planet formation, especially under certain dust-gas coupling conditions.

## Contribution

It provides the first linear perturbation analysis of nonaxisymmetric SGI in protoplanetary disks using a two-fluid model, highlighting transient amplification effects.

## Key findings

- Nonaxisymmetric perturbations grow significantly over finite times.
- Dust amplification occurs even when gas remains stable.
- Amplification depends on dust-gas coupling and azimuthal wavelength.

## Abstract

In protoplanetary discs (PPDs) consisting of gas and dust particles, fluid instabilities induced by the drag force, including secular gravitational instability (SGI) can facilitate planet formation. Although SGI subject to the axisymmetric perturbations was originally studied in the absence of gas feedback and it then generalized using a two-fluid approach, the fate of the nonaxisymmetric SGI, in either case, is an unexplored problem. We present a linear perturbation analysis of the nonaxisymmetric SGI in a PPD by implementing a two-fluid model. We explore the growth of the local, nonaxisymmetric perturbations using a set of linearized perturbation equations in a sheared frame. The nonaxisymmetric perturbations display significant growth during a finite time interval even when the system is stable against the axisymmetric perturbations. Furthermore, the surface density perturbations do not show continuous growth but are temporally amplified. We also study cases where the dust component undergoes amplification whereas the gas component remains stable. The amplitude amplification, however, strongly depends on the model parameters. In the minimum mass solar nebula (MMSN), for instance, the dust fluid amplification at the radial distance 100 au occurs when the Stokes number is about unity. But the amplification factor reduces as the dust and gas coupling becomes weaker. Furthermore, perturbations with a larger azimuthal wavelength exhibit a larger amplification factor.