# Features of Accretion-phase Gravitational-wave Emission from Two-dimensional Rotating Core-collapse Supernovae

## TL;DR

This study analyzes how progenitor mass and rotation influence gravitational-wave signals during the accretion phase of core-collapse supernovae, revealing that rotation suppresses GW emission and that bounce signals are mass-independent.

## Contribution

It provides the first detailed 2D neutrino radiation-hydrodynamic simulations across various progenitor masses and rotation rates, highlighting the effects on GW emission features.

## Key findings

- GW strain at bounce is mass-independent but depends on angular momentum.
- Rotation suppresses postshock convection and SASI, reducing GW emission.
- Approximate GR treatment aligns well with full GR results.

## Abstract

We explore the influence of progenitor mass and rotation on the gravitational-wave (GW) emission from core-collapse supernovae, during the postbounce, preexplosion, accretion-phase. We present the results from 15 two-dimensional (2D) neutrino radiation-hydrodynamic simulations from initial stellar collapse to $\sim$300 ms after core bounce. We examine the features of the GW signals for four zero-age main sequence (ZAMS) progenitor masses ranging from 12 $M_\odot$ to 60 $M_\odot$ and four core rotation rates from 0 to 3 rad s$^{-1}$. We find that GW strain immediately around core bounce is fairly independent of ZAMS mass and---consistent with previous findings---that it is more heavily dependent on the core angular momentum. At later times, all nonrotating progenitors exhibit loud GW emission, which we attribute to vibrational g-modes of the protoneutron star (PNS) excited by convection in the postshock layer and the standing accretion shock instability (SASI). We find that increasing rotation rates results in muting of the accretion-phase GW signal due to centrifugal effects that inhibit convection in the postshock region, quench the SASI, and slow the rate at which the PNS peak vibrational frequency increases. Additionally, we verify the efficacy of our approximate general relativistic (GR) effective potential treatment of gravity by comparing our core bounce GW strains with the recent 2D GR results of other groups.