This article was originally published at The Conversation. (opens in new tab) The publication contributed the article to Space.com's Expert Voices: Op-Ed & Insights (opens in new tab).
David Blair (opens in new tab), Emeritus Professor, ARC Centre of Excellence for Gravitational Wave Discovery, OzGrav, University of Western Australia
In 2017, astronomers witnessed the birth of a black hole for the first time. Gravitational wave detectors picked up the ripples in spacetime caused by two neutron stars colliding (opens in new tab) to form the black hole, and other telescopes then observed the resulting explosion.
But the real nitty-gritty of how the black hole formed, the movements of matter in the instants before it was sealed away inside the black hole’s event horizon, went unobserved. That’s because the gravitational waves thrown off in these final moments had such a high frequency that our current detectors can’t pick them up.
If you could observe ordinary matter as it turns into a black hole, you would be seeing something similar to the Big Bang played backwards. The scientists who design gravitational wave detectors have been hard at work to figure out how improve our detectors to make it possible.
Today our team is publishing a paper (opens in new tab) that shows how this can be done. Our proposal could make detectors 40 times more sensitive to the high frequencies we need, allowing astronomers to listen to matter as it forms a black hole.
It involves creating weird new packets of energy (or “quanta”) that are a mix of two types of quantum vibrations. Devices based on this technology could be added to existing gravitational wave detectors to gain the extra sensitivity needed.
Gravitational wave detectors such as the Laser Interferometer Gravitational-wave Observatory (LIGO) in the United States use lasers to measure incredibly small changes in the distance between two mirrors. Because they measure changes 1,000 times smaller than the size of a single proton, the effects of quantum mechanics – the physics of individual particles or quanta of energy – play an important role in the way these detectors work.
Two different kinds of quantum packets of energy are involved, both predicted by Albert Einstein. In 1905 he predicted that light comes in packets of energy that we call photons; two years later, he predicted that heat and sound energy come in packets of energy called phonons.
Photons are used widely in modern technology, but phonons are much trickier to harness. Individual phonons are usually swamped by vast numbers of random phonons that are the heat of their surroundings. In gravitational wave detectors, phonons bounce around inside the detector’s mirrors, degrading their sensitivity.
Five years ago physicists realised you could solve the problem of insufficient sensitivity at high frequency with devices that combine phonons with photons. They showed that devices in which energy is carried in quantum packets that share the properties of both phonons and photons can have quite remarkable properties.
These devices would involve a radical change to a familiar concept called “resonant amplification”. Resonant amplification is what you do when you push a playground swing: if you push at the right time, all your small pushes create big swinging.
The new device, called a “white light cavity”, would amplify all frequencies equally. This is like a swing that you could push any old time and still end up with big results.
However, nobody has yet worked out how to make one of these devices, because the phonons inside it would be overwhelmed by random vibrations caused by heat.
In our paper (opens in new tab), published in Communications Physics, we show how two different projects currently under way could do the job.
The Niels Bohr Institute in Copenhagen has been developing devices (opens in new tab) called phononic crystals, in which thermal vibrations are controlled by a crystal-like structure cut into a thin membrane. The Australian Centre of Excellence for Engineered Quantum Systems has also demonstrated an alternative system (opens in new tab) in which phonons are trapped inside an ultrapure quartz lens.
We show both of these systems satisfy the requirements for creating the “negative dispersion” – which spreads light frequencies in a reverse rainbow pattern – needed for white light cavities.
Both systems, when added to the back end of existing gravitational wave detectors, would improve the sensitivity at frequencies of a few kilohertz by the 40 times or more needed for listening to the birth of a black hole.
Our research does not represent an instant solution to improving gravitational wave detectors. There are enormous experimental challenges in making such devices into practical tools. But it does offer a route to the 40-fold improvement of gravitational wave detectors needed for observing black hole births.
Astrophysicists have predicted complex gravitational waveforms created by the convulsions of neutron stars as they form black holes. These gravitational waves could allow us to listen in to the nuclear physics of a collapsing neutron star.
For example, it has been shown that they can clearly reveal whether the neutrons in the star remain as neutrons or whether they break up into a sea of quarks, the tiniest subatomic particles of all. If we could observe neutrons turning into quarks and then disappearing into the black hole singularity, it would be the exact reverse of the Big Bang where out of the singularity, the particles emerged which went on to create our universe.
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