Abstract
Abstract Understanding the formation of stellar clusters requires following the interplay between gas and newly formed stars accurately. We therefore couple the magnetohydrodynamics code FLASH to the N-body code ph4 and the stellar evolution code SeBa using the Astrophysical Multipurpose Software Environment (AMUSE) to model stellar dynamics, evolution, and collisional N-body dynamics and the formation of binary and higher-order multiple systems, while implementing stellar feedback in the form of radiation, stellar winds, and supernovae in FLASH. We here describe the algorithms used for each of these processes. We denote this integrated package Torch. We then use this novel numerical method to simulate the formation and early evolution of several examples of open clusters of ∼1000 stars formed from clouds with a mass range of 103 M ⊙ to 105 M ⊙. Analyzing the effects of stellar feedback on the gas and stars of the natal clusters, we find that in these examples, the stellar clusters are resilient to disruption, even in the presence of intense feedback. This can even slightly increase the amount of dense, Jeans unstable gas by sweeping up shells; thus, a stellar wind strong enough to trap its own H ii region shows modest triggering of star formation. Our clusters are born moderately mass segregated, an effect enhanced by feedback, and retained after the ejection of their natal gas, in agreement with observations.
Highlights
Star cluster formation is a nonlinear, attenuated, feedback problem: initially cold and dense gas starts forming stars, and the more dense gas is available, the more vigorous the star formation becomes (Mac Low & Klessen 2004)
Analyzing the effects of stellar feedback on the gas and stars of the natal clusters, we find that in these examples, the stellar clusters are resilient to disruption, even in the presence of intense feedback
In the current study we focus on describing the numerical methods developed to implement stellar feedback of the stars acting on gas, and their consequences
Summary
Star cluster formation is a nonlinear, attenuated, feedback problem: initially cold and dense gas starts forming stars, and the more dense gas is available, the more vigorous the star formation becomes (Mac Low & Klessen 2004). Subsequent studies have further investigated feedback in the form of radiation (Rosen et al 2016; Corresponding author: Mordecai-Mark Mac Low (Kim & Ostriker 2015; Simpson et al 2015; Ibanez-Mejıa et al 2016; Girichidis et al 2016) with increasing accuracy. None of these works has included at the same time ionizing radiation, winds, supernovae, stellar evolution, and collisional N-body dynamics capable of following the formation and dynamical evolution of wide binaries and multiple systems.
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