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When people quote the discovery of gravitational waves no reference seems to be made to the frequency, presumably this is about the current state of detectors. Or are the frequencies detected the same as the resonant frequencies of the bars used? What range of frequencies are gravitational waves expected to have?

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    $\begingroup$ There's a lot of information about this! If you check the LIGO papers there is detailed information on how sensitive LIGO is at different frequencies and about the frequency of GW150914. The paper has nice spectra, showing it climbing fro ~60Hz to ~300Hz. $\endgroup$
    – user107153
    Apr 5, 2016 at 10:14
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    $\begingroup$ @tfb figure 3 in that paper shows sensitivity in the 20-2000Hz range. The Einstein @ Home distributed computing program has searched that entire range for CW signals (from pulsar spin down) in data collected from the previous generation instruments; and is currently doing an initial search of the 20-100Hz range in data from ALIGO. $\endgroup$ Apr 5, 2016 at 14:00
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    $\begingroup$ Did you search the page you link for the word "frequency"? $\endgroup$
    – rob
    Apr 5, 2016 at 15:22
  • $\begingroup$ I was restricted to popular accounts $\endgroup$
    – jim
    Apr 6, 2016 at 8:59

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Have a look at an announcement from LIGO where they describe the experiment.

ligo

The first plot shows the frequencies detected.

The original waves are redshifted.

ligo2

Estimated source parameters for GW150914. We report the median value as well as the range of the 90% credible interval. Masses are measured in the source frame; to convert masses to detector frame, multiply by (1 + z). The source redshift assumes standard cosmology.

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Or are the frequencies detected the same as the resonant frequencies of the bars used?

The LIGO detectors, which measured the waves, do not use bar detectors; they use interferometers. Bar detectors have been used for decades, but they have not been sensitive enough to make actual detections. They are necessarily very short, which reduces the effect of a gravitational wave. As you indicate they also have fairly narrow resonant frequencies at which they are most sensitive. Interferometers, on the other hand, can be made 4 kilometers long (like the LIGO detectors), which magnifies the effect of the waves. They are also sensitive over a fairly broad range -- roughly 40Hz to 2000Hz.

As anna v rightly points out, there actually are plenty of references to frequency if you look at the science papers. I work in gravitational-wave astronomy, and decomposing things into frequencies is our bread and butter. There's less coverage of this in the popular press, presumably because the public tunes out talk of frequencies, and pop-sci journalists know where their bread is buttered. But Fourier transforms are really how the analysis gets done.

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There are plenty of references made to the frequency. The gravitational waves that were detected swept up in frequency and amplitude from an undetectable level at a few tens of Hz to abut 150 Hz as the black holes merged. This is known as a "chirp".

Gravitational wave sources might have a variety of frequencies. For binary systems, the principle gravitational frequency is twice the orbital frequency.

A more general rule of thumb is that the highest gravitational wave frequencies produced will be at around the reciprocal of the freefall timescale for a system $f_{\rm max} \sim \sqrt{G\rho}$, where $\rho$ is the average density of the system. In the case of the merging black holes here, $\rho$ can be represented as the mass of the black holes divided by a volume defined by their event horizons and $f_{\rm max} \sim 1$ kHz.

As the event horizon radius is proportional to $M$, then $f_{\rm max} \propto M^{-1}$ and so merging events for supermassive black holes are expected to be at much lower frequencies.

For a core collapse supernova - $R \sim 10$ km and $M\sim 1M_{\odot}$ and my simple formula suggests gravitational waves with $f_{\rm max} \sim 5$ kHz.

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You can classify GWs according to their power: When BH merge, the power in the final stage increases to probably $10^{40}$ watts and the frequency to around 200 Hz. These are the sources proven so far. You can receive them for a few milliseconds.

Binary systems of two stars like Algol emit about $10^{10}$ watts at frequencies around $10~\mu$Hz. These are continuous GW, which probably carry interesting information, such as the number, orbital period and mass of planets. Since the interferometers are insensitive in this frequency range, these signals cannot yet be received due to the lack of an antenna.

For years people have been trying unsuccessfully to detect continuous GW in the frequency range 20 Hz to 1000 Hz because only that can be received by the interferometers. It is unclear whether there are any sources in this frequency range that are not rotationally symmetrical. If there are fast-spinning pulsars with high mountains, they could radiate power around $10^4$ watts. If you compare this with the top performance of mergers, it becomes clear why searches have so far been unsuccessful.

There could also be GW at much lower frequencies around 1 nHz. If these were created right after the Big Bang at 1 Hz, redshift could have greatly reduced the frequencies. It is unclear whether there are preferred frequencies.

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