Exploring Supernova Gravitational Waves with Machine Learning

The gravitational wave strain from сore-collapse supernova simulations used in our analysis. The file contains 402 signals labeled as s00A0O00 or s00A0O00.0, where:

s00 -- corresponds to (zero-age) progenitor mass, e.g. s27 means 27 solar mass

A0 -- corresponds for a degree of differential rotation

O00 or O00.0 -- corresponds to central angular velocity, e.g. O07 or O07.5 means that our model has a central angular velocity of 7 or 7.5 rad/s, respectively

Our waveforms are represented as a quadrupole wave amplitude. One can get a strain h multiplied by the distance D (= 10 kpc) by the following formula: hD = our_data/3.66 cm; see Eq (20) of Dimmelmeier et al 2008 [link] for more information. All waveforms are represented in the time range from -15 to 20 ms with a 0.001 ms step size. The time of zero corresponds to the time of bounce. See [https://arxiv.org/abs/2209.14542] for more information.