\item Consider a mass $m$ is performing simple harmonic motion along $z$ axis. Compute $h_{+}$ and $h_{\times}$ and power radiated. Plot the angular distribution of emitted power.
\item Discuss the physical differences in the two radiation pattern obtained in Problem 2 and 3. Discuss the symmetry of the radiation pattern for both cases.
\end{enumerate}
\subsection{Tutorial 6}
\begin{enumerate}
\item link to mathematica notebook \href{http://gitlab.icts.res.in/ajith/gwcourse2023/tree/master/tuturials}{http://gitlab.icts.res.in/ajith/gwcourse2023/tree/master/tuturials}
\end{enumerate}
\subsection{Tutorial 7}
\begin{enumerate}
\item Assume that all the spin down of pulsar is due to GW emissions, compute the strain amplitude of all pulsars in the \href{https://www.atnf.csiro.au/research/pulsar/psrcat/}{ATNF} catalog, using the $f$ and $\dot{f}$ values from the catalog.
\item Plot the amplitude of the GW signals as a function of the Fourier frequency for the following continuous sources of GWs.
\begin{itemize}
\item Known binary white dwarfs from our galaxy. You can get the masses and orbital period from some existing catalogs (e.g.\href{https://ieeexplore.ieee.org/document/8223753}{https://ieeexplore.ieee.org/document/8223753)})
\item Known binary pulsars
\item Isolated spinning neutron stars from the ATNF pulsar catalog. Assume an ellipticity of $10^{-8}.$
\item SMBH binaries with total mass 1e6 and 1e9 Msun. Use the following orbital separations $\mathrm{R}=1\mathrm{pc},\;10^{-3}\mathrm{pc}$.
\item Stellar mass BHs with total mass 10 Msun with orbital separation 1AU.
