Ethan Winch
YOU?
Author Swipe
View article: The black hole–pair instability boundary for high stellar rotation
The black hole–pair instability boundary for high stellar rotation Open
The pair instability (PI) boundary is crucial for understanding heavy merging black holes (BHs) and the second mass gap’s role in galactic chemical evolution. So far, no works have critically and systematically examined how rotation and ma…
View article: The black hole - pair instability boundary for high stellar rotation
The black hole - pair instability boundary for high stellar rotation Open
The Pair Instability (PI) boundary is crucial for understanding heavy merging Black Holes (BHs) and the second mass gap's role in galactic chemical evolution. So far, no works have critically and systematically examined how rotation and ma…
View article: Decomposing the AIA 304 Å Channel into Its Cool and Hot Components
Decomposing the AIA 304 Å Channel into Its Cool and Hot Components Open
The AIA 304 Å channel on board the Solar Dynamics Observatory (SDO) offers a unique view of $\approx 10^{5}\text{ K}$ plasma emitting in the He ii 304 Å line. However, when observing off-limb, the emission of the (small) cool struc…
View article: Decomposing the AIA~304 channel into its cool and hot components
Decomposing the AIA~304 channel into its cool and hot components Open
The AIA~304 channel on board the \textit{Solar Dynamics Observatory} (SDO) offers a unique view of low transition region (TR) plasma emitting in the He II 304 ˚A line. However, when observing off-limb, the emission of the (small) cool stru…
View article: Predicting the heaviest black holes below the pair instability gap
Predicting the heaviest black holes below the pair instability gap Open
Traditionally, the pair instability (PI) mass gap is located between 50 and 130 M⊙, with stellar mass black holes (BHs) expected to ‘pile up’ towards the lower PI edge. However, this lower PI boundary is based on the assumption that the st…
View article: Predicting the Heaviest Black Holes below the Pair Instability Gap
Predicting the Heaviest Black Holes below the Pair Instability Gap Open
Traditionally, the pair instability (PI) mass gap is located between 50\,and 130\,$M_{\odot}$, with stellar mass black holes (BHs) expected to "pile up" towards the lower PI edge. However, this lower PI boundary is based on the assumption …
View article: Bringing Stellar Evolution and Feedback Together: Summary of Proposals from the Lorentz Center Workshop
Bringing Stellar Evolution and Feedback Together: Summary of Proposals from the Lorentz Center Workshop Open
Stars strongly impact their environment, and shape structures on all scales throughout the universe, in a process known as “feedback.” Due to the complexity of both stellar evolution and the physics of larger astrophysical structures, ther…
View article: Bringing Stellar Evolution & Feedback Together: Summary of proposals from the Lorentz Center Workshop, 2022
Bringing Stellar Evolution & Feedback Together: Summary of proposals from the Lorentz Center Workshop, 2022 Open
Stars strongly impact their environment, and shape structures on all scales throughout the universe, in a process known as ``feedback''. Due to the complexity of both stellar evolution and the physics of larger astrophysical structures, th…