Einstein’s 100-year old theory of General Relativity has withstood every test. Why then do many scientists believe it will need to be modified, and what new evidence could be obtained in the next 10 years to point the way?
It has been a century since Einstein published his mind- and space-bending theory of general relativity (GR). When it passed its first real test during the total solar eclipse of 1919, where the bending of light from distant stars around our Sun was exactly as GR predicted, Einstein became an international celebrity. GR replaced Newton’s model of gravity as a simple force with the revolutionary idea of curved space-time that responds dynamically to mass and energy.
Since then, and especially in the last few decades, GR has elegantly explained the gravitational nature of our Universe from the earliest times and at the largest scales in cosmology, to the compact and extremely warped regions of space-time near black holes and neutron stars (as near as we have yet been able to measure), and even here throughout our solar system, where GR allows atomic clocks to keep perfect and synchronized time and thus for GPS devices to provide our locations to within a few meters. Time and again GR has been tested with ever improving precision using new and inventive astronomical observations, and each time Einstein’s theory has withstood the test. Yet surprisingly, there is a broad scientific consensus that general relativity is almost certainly not the final answer on gravity: that at some scale, under some circumstances, the theory of GR will break down.
Proving Einstein wrong would be a sad moment. But creating a new, quantum-friendly version of General Relativity would be a monumental achievement.
The problem is the apparent conflict between GR and the other dominant and successful theory of physics, quantum mechanics. The quantum world, while perhaps even more counter-intuitive than relativity, has been tested to exquisite precision and both explains the nature of matter and predicts its behavior at the level of subatomic particles, atoms, and molecules; it underlies chemistry, the nature of materials, and all of the technologies that power our modern society. The pervasive nature of quantum mechanics in all aspects of modern physics except gravity strongly suggests that gravity should be part of the same fold—that matter on a planetary or galactic scale should not behave differently than matter on an atomic scale.
One good example of the apparent gap between GR and quantum mechanics comes from modern cosmology. Increasingly detailed satellite measurements of the cosmic microwave background—the relic radiation left over from the Big Bang—combined with ground- and space-based observations of supernovae and the large-scale structures in the universe have led to a consensus model based firmly on GR that beautifully explains the observations. Yet the model suggests that over 95% of the “stuff” in our universe is currently a complete mystery to us, the famous dark matter and dark energy. Is GR showing us the way to new physics via that 95%? Or is it pointing us to flaws in GR?
Another aspect of the dilemma is the expectation that GR’s space-time, since it responds to mass and energy that are quantized, should also display quantum characteristics. But the curved, smoothly varying space-time of GR has resisted decades of attempts at quantization. Even so there are hints, such as Stephan Hawking’s still-untested prediction of quantum-mechanically generated radiation from black holes. So scientists continue to push on the theory, looking at extremes of scale or curvature where it might begin to break down. To take the next big step in fundamental physics, in effect, scientists now need to find the limitations of Einstein’s theory. The opportunity to do that, and to re-invent or refine the theory of gravity, now seems increasingly immanent.
The opportunity stems primarily from several next-generation efforts to detect and measure gravitational waves or to directly image the effects of strongly curved space-time. Gravitational waves are the only remaining prediction of GR that has not been observed, and if their characteristics differ from what GR predicts—or if they don’t exist—then the door to new physics is wide open. An early test will come from ground-based laser interferometers, such as LIGO (Laser Interferometer Gravitational-Wave Observatory), which seeks to detect gravitational waves with millisecond periods coming from pairs of black holes or neutron stars as they orbit closer and closer to each other before coalescence. According to GR, pairs of moving masses will emit gravitational waves in space-time much like moving boats cause ripples in the surface of a pond. The waves carry energy and momentum away from the systems, causing the orbits to shrink, a prediction of GR that has been confirmed by timing pulses from pulsars in compact binary systems. While the direct detection of gravitational waves would be another confirmation of Einstein’s theory, the detailed shapes of the waveforms could potentially point to problems with GR.
Beyond LIGO there are a series of planned attempts to test GR more directly, some quite expensive and lengthy big science projects, others much less expensive and potentially capable of more rapid results. These include:
- A major international project to build a space-based gravitational wave interferometer called LISA, which would provide very precise gravity wave measurements from massive black hole systems; the U.S. has recently withdrawn from this project, but a scaled-down version, called eLISA, is being planned in Europe for development in the 2020s and launch in the mid-2030s. It would detect waves with hour-long periods from thousands of emitting systems.
- A very different ground-based mega-science project, the Square Kilometer Array, has tests of GR as one of its major scientific objectives. This continent-sized network of radio telescopes will be able to track pulsars—rotating neutron stars—in binary systems very precisely and also to detect very long wavelength gravitational waves from pairs of super-massive black holes orbiting each other in the centers of other galaxies. Phase one of the SKA is expected to be operational only in 2024 and the full array not before 2030. The U.S. is not currently involved in the SKA.
- The Event Horizon Telescope (EHT) uses a network of atomic clocks to precisely synchronize existing radio telescopes around the planet, turning them into an Earth-sized virtual telescope. With the greatest magnifying power ever achieved in astronomy, the EHT is on track to make the first image of a black hole, and thereby test GR theory within the most extreme environment in the cosmos. The U.S. leads this international effort to “see the un-seeable,” which could alter our ideas of gravity and quantum mechanics, and prove, once and for all, that black holes exist.
- A similar effort called NANOGrav is attempting to directly detect very low-frequency gravitational waves by precisely timing pulsars and looking for deviations in these otherwise extremely regular radio beacons. It has the potential to detect these waves at modest cost and within a few years. The effort, part of a larger international collaboration, uses the existing Green Bank and Arecibo radio telescopes currently funded by the National Science Foundation, but will need additional support.
Einstein’s theory of general relativity is most deservedly a central pillar in the framework of modern physics. Yet the lack of a quantum version of GR suggests to many scientists that experiments in the future will find its limitations. While proving Einstein “wrong” would be a sad moment, creating a new, quantum-friendly theory of gravity would also mark a monumental achievement for the progress of fundamental physics.
The XO File
Measuring the Shadow of a Massive Black Hole
A long-standing goal in astronomy, math and physics is to image and time-resolve the boundary of a black hole — the event horizon — where intense gravity prevents even light from escaping. If it were possible to zoom in to the event horizon, General Relativity predicts that we would see a ’shadow’ against a backdrop of glowing super-hot gas as the black hole absorbs and bends the light surrounding it. Direct observation of this unique signature holds the answers to some of the most fundamental questions we can ask: Do black holes exist? Does GR hold in the strongest gravity environment? How do supermassive black holes affect the evolution of entire galaxies?
The Event Horizon Telescope (EHT) project is aimed at realizing this goal through the technique of Very Long Baseline Interferometry (VLBI): combining simultaneous observations across a global network of radio dishes to forge an Earth- sized telescope. By leveraging advanced electronics to build a new generation of VLBI instrumentation, the project will achieve a magnifying power 2000 times finer than the Hubble Space Telescope. A prime target is Sagittarius A*, the supermassive black hole in the center of the Milky Way that has a mass of about 4 million suns, and which has the largest apparent event horizon in the sky. Observations with a prototype EHT have confirmed the size of SgrA* to be very close to the predicted value by GR, and this proof of concept has brought the project to a tipping point: over the next few years, the prospects for imaging this black hole and tracking the dynamics of in-falling matter are excellent.
The main EHT challenge is in forming the electronic ‘lens’ that combines data captured at all the geographic sites, in much the same way a mirror focuses optical light in a conventional telescope. Currently, these data streams are combined in a modest purpose-built computer cluster. But data rates at each site are to exceed 8 GBytes/second within two years, so a next-generation system that can handle this torrent of data is needed. An investment of $7M would ensure completion of this EHT ‘lens’, including refinement of algorithms to efficiently form images. With funding already in-hand from the NSF and international partners to support work at the individual telescopes, an investment on this scale would have considerable leverage, and would ensure continued US leadership of the project.