this is for holding javascript data
Matteo Cantiello edited untitled.tex
over 8 years ago
Commit id: db5bd01b47bea3d0438bafc97e7f950c719d9961
deletions | additions
diff --git a/untitled.tex b/untitled.tex
index 8d043be..9c4476b 100644
--- a/untitled.tex
+++ b/untitled.tex
...
\section{Steady vs Eruptive Massloss}
The mass loss rates during the last few hundred years of evolution of some core collapse supernova progenitors seem to violate the maximum values allowed by line-driven winds ($\dot{M} \sim 10^{-4}$M$_\odot$yr$^{-1}$, Smith \& Owocki 2006).
Intense, eruptive Intense stellar mass loss during the final years before core collapse could be caused by
internal gravity waves excited by core convection during Neon and Oxygen fusion (Quataert \& Shiode 2012).
The Most importantly, the model predicts a correlation between the energy associated with pre-SN mass ejection and the time to core collapse, with the most intense mass loss preferentially occurring closer to core collapse (Shiode \& Quataert 2014).
Binary interaction in the final years before core collapse could also cause enhanced, irregular mass loss. The rate of stars exploding during or short-after the onset of binary interactions should be small ($< 5$\%, De Mink, Priv. Comm.) and in this case no correlation is expected between mass loss rate and time to core collapse.