SXS gravitational wave data question

I need to do some analysis for a project with the SXS gravitational wave data: https://data.black-holes.org/waveforms/catalog.html but I am a bit confused about the initial conditions of their simulations. I read the paper they published about the data (it can be found at that website) but i am still not sure I understand. I attached several weaveforms I extracted from their database (the y axis has $$h_+$$). So it seems like the starting time (in their units) is the same for all the waveforms. But I am not sure how that is defined. More specifically, for the purpose of my project, I would like to know what defines the initial frequency of the each gravitational wave in their simulations. Can someone help me with this? Thank you!

• The link you gave has a table which states what the initial conditions are. Please clarify your question. Commented Dec 7, 2019 at 9:31

The initial gravitational frequency is just determined from the initial orbital parameters (masses and separations) that are given in the table that comes up when you follow the link you provided. These give an initial orbital frequency (given roughly by Kepler's third law for binaries which are reasonably well separated to begin with), and for gravitational waves that depend on the acceleration of the square of the quadrupole mass moment, this means, that for circular orbits, the gravitational wave frequency is twice the orbital frequency.

Binary compact objects that have orbital frequencies high enough to be detected by aLIGO are expected to have circularised. The timescale for circularisation is shorter than the timescale on which the orbital separation changes. However, it is possible that mergers triggered by three-body interactions might lead to eccentric binary GW sources (Lower et al. 2018).

Eccentric binaries have a more complex waveform, with additional significant contributions at the orbital frequency and three times the orbital frequency. The waveform would also depend on the orientation of the orbit as we see it. Some mathematics and examples are shown in Martel & Poisson (1999).

Compact binaries with significant component spins and/or misalignment of their spin and orbital angular momentum will also produce (small) harmonics of the orbital frequency (e.g. Arun et al. 2009.

The site you link to contains a catalogue of different waveforms calculated using a numerical scheme. The calculations are complex and consumes lot of computing resources. Each calculation is followed over some tens of cycles prior to the binary merger. What determines the starting point is I think just restricting the simulation to frequencies that are in the relevant sensitivity window of GW detectors.

• Thank you for your reply! I guess my confusion is on how do they choose the initial parameters, mainly the location of the black holes. Commented Dec 7, 2019 at 23:15
• One more question, does the fact that the gravitational wave frequency is twice the orbital one, always hold (in the Newtonian limit)? Or does it have a dependence on eccentricity? Commented Dec 7, 2019 at 23:52
• @BillKet I still don't know what you mean The website gives a library of waveforms for many different binaries. Good point about eccentricity. See edit. Commented Dec 8, 2019 at 9:59
• Thank you for this! So I kinda figured out this issues with frequency, but since you seem to know a lot about this, I have one more question. For some waveforms, the amplitude is not smoothly increasing, but after each period the amplitude is going up and down between 2 values (on top of the overall increase). Is this possible (maybe due to spin?) or am I just extracting the data in a wrong way. Again thanks a lot for the help! Commented Dec 9, 2019 at 8:12
• @BillKet Eccentricity can do this. See the examples in the reference I've cited. Commented Dec 9, 2019 at 12:05