# Difference in Gravitational Waveforms for different objects?

This is an extension of one of my older questions:

How would the gravitational strain waveform look like for a planet in orbit with a star?

Let's say at some distance D there are two objects which are in binary inspiral. Both lets assume mass $M_1$ and $M_2$. And both these masses are sufficiently large and far away. Let's take three cases of these objects:

1) Two black holes in binary inspiral which will merge in the end.

2) A planet orbiting a star.

3) Two stars inspiral with each other.

I wanted to know if the individual properties of these bodies cause the gravitational waves ie Numerical Relativity Waveforms to look significantly different from each other? Like for example, the ringdown phase does not exist for both cases 2 and 3 in a numerical relativity waveform.

I wanted to know if there are any other factors that would cause the overall waveform to be different for these three cases. Assuming $M_1$ and $M_2$ where $M_1$ > $M_2$ . If there are any, how would the waveform differ?

What I'm trying to infer here is, are numerical relativity waveforms an outcome of just the mass of an object or does the property of the object come into question as well?