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Understanding the formation of stellar clusters requires following theinterplay between gas and newly formed stars accurately. We therefore couplethe magnetohydrodynamics code FLASH to the N-body code ph4 and the stellarevolution code SeBa using the Astrophysical Multipurpose Software Environment(AMUSE) to model stellar dynamics, evolution, and collisional N-body dynamicsand the formation of binary and higher-order multiple systems, whileimplementing stellar feedback in the form of radiation, stellar winds andsupernovae in FLASH. We here describe the algorithms used for each of theseprocesses. We denote this integrated package Torch. We then use this novelnumerical method to simulate the formation and early evolution of severalexamples of open clusters of ~1000 stars formed from clouds with a mass rangeof 10^3-10^5 M_sun. Analyzing the effects of stellar feedback on the gas andstars of the natal clusters, we find that in these examples, the stellarclusters are resilient to disruption, even in the presence of intense feedback.This can even slightly increase the amount of dense, Jeans unstable gas bysweeping up shells; thus, a stellar wind strong enough to trap its own H IIregion shows modest triggering of star formation. Our clusters are bornmoderately mass segregated, an effect enhanced by feedback, and retained afterthe ejection of their natal gas, in agreement with observations.

Modelling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method