Star formation is a messy and chaotic mechanism that involves several physical processes including gravity, magnetic fields, turbulence, and stellar feedback. The interplay of the processes inherent to star formation are often interdependent and entangled, thereby hindering the acceptance of a universal theory of star formation. Therefore, it is challenging to determine the relative importance of the various processes, especially when this importance is environment-dependent.
State-of-the-art telescopes are providing ground-breaking observations of star-forming regions and young stellar objects with unprecedented detail. Such observations have shed light on how these various physical processes work in concert to lead to star formation.
Simultaneously, state-of-the-art numerical simulations are greatly advancing star formation theory on all scales – from the birth of isolated stars to the formation and early evolution of entire star clusters. These simulations are providing detailed explanations of the effects of the various physical processes and attempting to decouple their effects. On their own and also by comparing to observations, numerical studies are greatly advancing star formation theory.
This Research Topic focuses on numerical star formation. The goal is to provide a comprehensive overview that will be a go-to resource for new and experienced star formation scientists alike. We aim to begin this collection with a discussion of numerical methods used in state-of-the-art simulations (including resolved physical processes and unresolved stellar feedback mechanisms via sub-grid models), followed by a discussion of the current numerical results (ranging in scales from individual stars and protoplanetary disks to star clusters and eventually to galaxies. ) We will conclude with a discussion of applications to bridge the gap between simulations and observations including comparing the numerical results to observations via synthetic observations).
We welcome review articles and mini-reviews on the topic of numerical star formation. To compile a comprehensive review, we appreciate contributions on the following:
1. Methods & Algorithms
1a. Numerical Methods (e.g., SPH, AMR, moving mesh, N-body)
1b. Numerical Algorithms (e.g., Trees, Gravity solvers, Sink/Star/cluster particles)
1c. Initial conditions including geometry
1d. Radiation transport (e.g., Monte-Carlo, ray tracing, moment-methods)
1e. Sub-grid physics (e.g., Sink/Star/cluster particles, feedback models)
1f. Chemical models
2. Results
2a. Galaxy to cloud scales
2b. Cloud to core to 'star' scales
2c. Core to protostar & disc scales
2d. Disk evolution and Planet Formation
3. Applications
3.a. Synthetic observations and comparison with observations
4. Conclusions
4a. Historical perspective and future directions
4b. New computing frameworks
In all reviews, we would appreciate a comparison of the various methods/results. We
would also appreciate a discussion of caveats including shortcomings and what can/will be
done in the future to overcome these issues.
Star formation is a messy and chaotic mechanism that involves several physical processes including gravity, magnetic fields, turbulence, and stellar feedback. The interplay of the processes inherent to star formation are often interdependent and entangled, thereby hindering the acceptance of a universal theory of star formation. Therefore, it is challenging to determine the relative importance of the various processes, especially when this importance is environment-dependent.
State-of-the-art telescopes are providing ground-breaking observations of star-forming regions and young stellar objects with unprecedented detail. Such observations have shed light on how these various physical processes work in concert to lead to star formation.
Simultaneously, state-of-the-art numerical simulations are greatly advancing star formation theory on all scales – from the birth of isolated stars to the formation and early evolution of entire star clusters. These simulations are providing detailed explanations of the effects of the various physical processes and attempting to decouple their effects. On their own and also by comparing to observations, numerical studies are greatly advancing star formation theory.
This Research Topic focuses on numerical star formation. The goal is to provide a comprehensive overview that will be a go-to resource for new and experienced star formation scientists alike. We aim to begin this collection with a discussion of numerical methods used in state-of-the-art simulations (including resolved physical processes and unresolved stellar feedback mechanisms via sub-grid models), followed by a discussion of the current numerical results (ranging in scales from individual stars and protoplanetary disks to star clusters and eventually to galaxies. ) We will conclude with a discussion of applications to bridge the gap between simulations and observations including comparing the numerical results to observations via synthetic observations).
We welcome review articles and mini-reviews on the topic of numerical star formation. To compile a comprehensive review, we appreciate contributions on the following:
1. Methods & Algorithms
1a. Numerical Methods (e.g., SPH, AMR, moving mesh, N-body)
1b. Numerical Algorithms (e.g., Trees, Gravity solvers, Sink/Star/cluster particles)
1c. Initial conditions including geometry
1d. Radiation transport (e.g., Monte-Carlo, ray tracing, moment-methods)
1e. Sub-grid physics (e.g., Sink/Star/cluster particles, feedback models)
1f. Chemical models
2. Results
2a. Galaxy to cloud scales
2b. Cloud to core to 'star' scales
2c. Core to protostar & disc scales
2d. Disk evolution and Planet Formation
3. Applications
3.a. Synthetic observations and comparison with observations
4. Conclusions
4a. Historical perspective and future directions
4b. New computing frameworks
In all reviews, we would appreciate a comparison of the various methods/results. We
would also appreciate a discussion of caveats including shortcomings and what can/will be
done in the future to overcome these issues.
