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\begin{document}

\title{Rotation in massive stars:\\ Progenitors, Core Collapse and Compact Remnants}


\author{Jim Fuller}
\affil{Affiliation not available}

  
\author{Matteo Cantiello}
\affil{Affiliation not available}
  



\date{\today}

\maketitle




\section{Main Topics} \\
\subsection{What determines the rotation rates of progenitor stars}
\begin{itemize}
\item Single star evolution (hydrodynamic instabilities/circulations, magnetic torques, internal gravity waves, mass loss, etc.)
\item Binary star evolution (mass accretion, tides, mergers, etc.)
\end{itemize}


\subsection{How does rotation affect core collapse and the eventual SN/GRB explosion?}
\begin{itemize}
\item Typical core-collapse SNe
\item Central engines (GRBs, SLSNe)
\end{itemize}


\subsection{How can rotation be inferred from compact remnants?}

\begin{itemize}
\item White Dwarfs
\item Pulsars
\item X-ray binaries
\item Black Holes
\end{itemize}




\section{Questions}



\subsection{Is rotation important for the explosion mechanism of typical core collapse supernovae (Type II, Ib, Ic)?}
a. Yes \\
b. No \\





\subsection{For which of the following types of supernovae is rotation most important?}
a. Type IIp \\
b. Type Ib/c \\
c. Type IIn \\
d. Electron capture SNe \\


\subsection{What sets the rotation rate of young neutron stars and black holes?}
a. Pre-collapse rotation rate \\
b. Supernova dynamics (e.g., SASI, kicks, turbulence, fallback, etc.) \\
c. R-mode instability \\
d. Other \\



\subsection{Is rotation important for enhancing mass loss shortly before core collapse?}
a. Yes \\
b. No \\



\subsection{Is mass accretion the most common reason for very rapid pre-collapse rotation?}
a. Yes \\
b. No \\



\subsection{Which compact objects provide the most robust constraints for rotation rates at core collapse?}
a. White dwarfs \\
b. Neutron stars \\
c. Black holes \\
d. Other \\


\subsection{What future measurements can be used to most strongly constrain the role of rotation in supernovae?}
a. Supernovae \\
b. Compact object rotation rates \\
c. Gravitational waves \\
d. Neutrinos \\


\subsection{Is the commonly used assumption of "angular momentum conservation" during the core-collapse reasonable?}
a. Yes\\
b. No\\

\subsection{Is the rotational axis direction preserved throughout the core-collapse phase?}
a. Yes\\
b. No\\

\subsection{Black holes formed through fall-back mechanism versus direct-collapse are expected to differ on:}
a. Mass\\
b. Spin\\
c. Kick\\
d. All three\\
e. Other\\

\subsection{Is there a correlation  between the angular momentum content/profile of the pre-core-collapse star and the SN kick that the NS/BH will receive?}
a. Yes\\
b. No

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