• DOI:10.2458/azu_uapress_9780816531240-ch020
• Corpus ID: 118539135

Jets and Outflows from Star to Cloud: Observations Confront Theory

@article{Frank2014JetsAO,
  title={Jets and Outflows from Star to Cloud: Observations Confront Theory},
  author={Adam Frank and Tom P. Ray and S. Cabrit and Patrick Hartigan and H{\'e}ctor G. Arce and Francesca Bacciotti and J. M. Bally and Myriam Benisty and Jochen Eisloffel and Manuel Gudel and Sergey V. Lebedev and Brunella Nisini and A. C. Raga},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2014},
  pages={451}
}

• A. Frank, T. Ray, +10 authors A. Raga
• Published 14 February 2014
• Physics
• arXiv: Solar and Stellar Astrophysics

In this review we focus on the role jets and outflows play in the star and planet formation process. Our essential question can be posed as follows: are jets/outflows merely an epiphenomenon associated with star formation or do they play an important role in mediating the physics of assembling stars both individually and globally? We address this question by reviewing the current state of observations and their key points of contact with theory. Our review of jet/outflow phenomena is organized into three length-scale domains: Source and Disk Scales ($0.1-10^2$ au) where the connection with protostellar and disk evolution theories is paramount; Envelope Scales ($10^2-10^5$ au) where the chemistry and propagation shed further light on the jet launching process, its variability and its impact on the infalling envelope; Parent Cloud Scales ($10^5-10^6$ au) where global momentum injection into cluster/cloud environments become relevant. Issues of feedback are of particular importance on the smallest scales where planet formation regions in a disk may be impacted by the presence of disk winds, irradiation by jet shocks or shielding by the winds. Feedback on envelope scales may determine the final stellar mass (core-to-star efficiency) and envelope dissipation. Feedback also plays an important role on the larger scales with outflows contributing to turbulent support within clusters including alteration of cluster star formation efficiencies (feedback on larger scales currently appears unlikely). A particularly novel dimension of our review is that we consider results on jet dynamics from the emerging field of High Energy Density Laboratory Astrophysics (HEDLA). HEDLA is now providing direct insights into the 3-D dynamics of fully magnetized, hypersonic, radiative outflows.