Faculty
Science
Supervisor Name
Dr. Shantanu Basu
Keywords
Massive Star Formation, Magnetic Braking, High Mass Accretion Rates, Direct Collapse Model, First Hydrostatic Core, Star Formation Models
Description
Recent simulations of massive star formation reveal that high mass accretion rates can prevent the formation of an intermediate hydrostatic "first core" (1-10 AU). Leading to a continuous, supersonic infall of matter directly onto the forming star, and bypassing the disk formation typically observed in low-mass star formation. In the absence of the first core, magnetic field dissipation is minimized, enabling magnetic braking to remain highly effective throughout the collapse. This results in a different evolutionary pathway for massive stars, characterized bydirect accretion onto the proto-star, weak outflows, and the absence of a rotationally supported disk (Dapp et al., 2012; Tsukamoto et al., 2015). These observations deviate from traditional star formation models, necessitating a re-evaluation of the role of magnetic fields and mass accretion dynamics in the formation of massive stars
Acknowledgements
This work was funded by the Western USRI program. Thank you to my supervisors Dr. Shantanu Basu and Dr. Sree Ram Valluri.
Creative Commons License
This work is licensed under a Creative Commons Attribution-Noncommercial 4.0 License
Document Type
Poster
Massive Star Formation through Direct Collapse regulated by the Magnetic Field
Recent simulations of massive star formation reveal that high mass accretion rates can prevent the formation of an intermediate hydrostatic "first core" (1-10 AU). Leading to a continuous, supersonic infall of matter directly onto the forming star, and bypassing the disk formation typically observed in low-mass star formation. In the absence of the first core, magnetic field dissipation is minimized, enabling magnetic braking to remain highly effective throughout the collapse. This results in a different evolutionary pathway for massive stars, characterized bydirect accretion onto the proto-star, weak outflows, and the absence of a rotationally supported disk (Dapp et al., 2012; Tsukamoto et al., 2015). These observations deviate from traditional star formation models, necessitating a re-evaluation of the role of magnetic fields and mass accretion dynamics in the formation of massive stars
Comments
References: https://docs.google.com/document/d/1CY_zsEXq_ycTko5fq9miIZobOGECjmYADKVgGLAQzXQ/edit?usp=sharing