Asset Details
Do you wish to reserve the book?
The core collapse of a 16.5 M\\(_{\\odot}\\) star
Hey, we have placed the reservation for you!
By the way, why not check out events that you can attend while you pick your title.
Oops! Something went wrong.
Looks like we were not able to place the reservation. Kindly try again later.
Are you sure you want to remove the book from the shelf?
The core collapse of a 16.5 M\\(_{\\odot}\\) star
Do you wish to request the book?
The core collapse of a 16.5 M\\(_{\\odot}\\) star
Please be aware that the book you have requested cannot be checked out. If you would like to checkout this book, you can reserve another copy
We have requested the book for you!
Your request is successful and it will be processed during the Library working hours. Please check the status of your request in My Requests.
Oops! Something went wrong.
Looks like we were not able to place your request. Kindly try again later.
Paper
The core collapse of a 16.5 M\\(_{\\odot}\\) star
2024
Overview
We investigate the 1D stellar evolution of a 16.5 M\\(_{\\odot}\\) zero-age main-sequence star having different initial rotations. Starting from the pre-main-sequence, the models evolve up to the onset of the core collapse stage. The collapse of such a massive star can result in several kinds of energetic transients, such as Gamma-Ray Bursts (GRBs), Supernovae, etc. Using the simulation parameters, we calculate their free-fall timescales when the models reach the stage of the onset of core collapse. Estimating the free-fall timescale is crucial for understanding the duration for which the central engine can be fueled, allowing us to compare the free-fall timescale with the T\\(_{\\rm 90}\\) duration of GRBs. Our results indicate that, given the constraints of the parameters and initial conditions in our models, rapidly rotating massive stars might serve as potential progenitors of Ultra-Long GRBs (T\\(_{\\rm 90}\\) \\(>>\\) 500 sec). In contrast, the non-rotating or slowly rotating models are more prone to explode as hydrogen-rich Type IIP-like core-collapse supernovae.
Publisher
Cornell University Library, arXiv.org
