# Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space

## TL;DR

This study uses advanced radiation-hydrodynamics simulations to analyze how a massive star's feedback affects a turbulent cloud's evolution and the variability of the FUV radiation field impacting nearby objects.

## Contribution

It introduces a detailed model of radiative feedback from a massive star in a turbulent cloud, including the first measurement of FUV field variation in a dynamic cluster environment.

## Key findings

- 75% of cloud mass disperses within 4.3 Myr
- Ionized mass is lower in higher mass clouds despite larger ionized volume
- FUV radiation field varies significantly over time, affecting protoplanetary disc evolution

## Abstract

We investigate radiative feedback from a 34 M$_\odot$ star in a $10^4$ M$_\odot$ turbulent cloud using three-dimensional radiation-hydrodynamics (RHD) models. We use Monte Carlo radiative transfer to accurately compute photoionization equilibrium and radiation pressure, with multiple atomic species and silicate dust grains. We include the diffuse radiation field, dust absorption/re-emission, and scattering. The cloud is efficiently dispersed, with 75 per cent of the mass leaving the (32.3 pc)$^3$ grid within 4.3 Myr (1.1 $t_{ff}$). This compares to all mass exiting within 1.6 Myr (0.74 $t_{ff}$) in our previously published $10^3$ M$_\odot$ cloud. At most 20 per cent of the mass is ionized, compared to 40 per cent in the lower mass model, despite the ionized volume fraction being 80 per cent in both, implying the higher mass cloud is more resilient to feedback. The total Jeans-unstable mass increases linearly up to 1500 M$_\odot$ before plateauing after 2 Myr, corresponding to a core formation efficiency of 15 per cent. We also measure the time-variation of the far-ultraviolet (FUV) radiation field, $G_0$, impinging on other cluster members, taking into account for the first time how this changes in a dynamic cluster environment with intervening opacity sources and stellar motions. Many objects remain shielded in the first 0.5 Myr whilst the massive star is embedded, after which $G_0$ increases by orders of magnitude. Gas motions later on cause comparable drops which happen instantaneously and last for $\sim$ 1 Myr before being restored. This highly variable UV field will influence the photoevaporation of protoplanetary discs near massive stars.