New confirmation of Einstein's General Theory of Relativity

Einstein's 'impossible hope' comes true: Weighing a star with gravity
This illustration reveals how the gravity of a white dwarf star warps space and bends the light of a distant star behind it. Credit: NASA, ESA, and A. Feild (STScI)

Albert Einstein predicted that whenever light from a distant star passes by a closer object, gravity acts as a kind of magnifying lens, brightening and bending the distant starlight. Yet, in a 1936 article in the journal Science, he added that because stars are so far apart "there is no hope of observing this phenomenon directly."

Now, an international research team directed by Kailash C. Sahu has done just that, as described in their June 9, 2017 article in Science. The study is believed to be the first report of a particular type of Einstein's "gravitational microlensing" by a star other than the sun.

In a related perspective piece in Science, entitled "A centennial gift from Einstein," Terry Oswalt of Embry-Riddle Aeronautical University says the discovery opens a new window to understanding "the history and evolution of galaxies such as our own."

More specifically, Oswalt adds, "The research by Sahu and colleagues provides a new tool for determining the masses of objects we can't easily measure by other means. The team determined the mass of a collapsed stellar remnant called a white dwarf star. Such objects have completed their hydrogen-burning life cycle, and thus are the fossils of all prior generations of stars in our Galaxy, the Milky Way."

Oswalt, an astronomer and chair of the Department of Physical Sciences at Embry-Riddle's Daytona Beach, Florida campus, says further, "Einstein would be proud. One of his key predictions has passed a very rigorous observational test."

This time-lapse movie, made from eight Hubble Space Telescope images, shows the apparent motion of the white dwarf star Stein 2051 B as it passes in front of a distant star. The observations were taken between Oct. 1, 2013, and Oct. 14, 2015. The path of Stein 2051 B, due to its proper motion combined with its parallax due to the motion the Earth around the Sun, is shown by the wavy cyan line. Its proper motion in one year is shown by an arrow. Its parallax, enlarged by a factor of 5, is shown by an ellipse. Credit: NASA, ESA, and K. Sahu (STScI)

Understanding 'Einstein Rings'

The gravitational microlensing of stars, predicted by Einstein, has previously been observed. Famously, in 1919, measurements of starlight curving around a total eclipse of the Sun provided one of the first convincing proofs of Einstein's general theory of relativity - a guiding law of physics that describes gravity as a geometric function of both space and time, or spacetime.

"When a star in the foreground passes exactly between us and a background star," Oswalt explains, " results in a perfectly circular ring of light - a so-called 'Einstein ring.'"

New confirmation of Einstein's General Theory of Relativity
Astronomers made the Hubble observations of the white dwarf, the burned-out core of a normal star, and the faint background star over a two-year period. Hubble observed the dead star passing in front of the background star, deflecting its light. During the close alignment, the distant starlight appeared offset by about 2 milliarcseconds from its actual position. This deviation is so small that it is equivalent to observing an ant crawl across the surface of a quarter from 1,500 miles away. From this measurement, astronomers calculated that the white dwarf’s mass is roughly 68 percent of the sun’s mass. Credit: NASA, ESA, and K. Sahu (STScI)

Sahu's group observed a much more likely scenario: Two objects were slightly out of alignment, and therefore an asymmetrical version of an Einstein ring formed. "The ring and its brightening were too small to be measured, but its asymmetry caused the distant star to appear off-center from its true position," Oswalt says. "This part of Einstein's prediction is called 'astrometric lensing' and Sahu's team was the first to observe it in a star other than the Sun."

Sahu, an astronomer at the Space Telescope Science Institute in Baltimore, Maryland, took advantage of the superior angular resolution of the Hubble Space Telescope (HST). Sahu's team measured shifts in the apparent position of a as its light was deflected around a nearby white dwarf star called Stein 2051 B on eight dates between October 2013 and October 2015. They determined that Stein 2051 B - the sixth-closest to the Sun - has a mass that is about two-thirds that of the sun.

"The basic idea is that the apparent deflection of the background star's position is directly related to the mass and gravity of the white dwarf - and how close the two came to exactly lining up," explains Oswalt.

This animation shows the motion of a white dwarf star passing in front of a distant background star. During the passage, the faraway star appears to change its position slightly, because its light path has been altered by the white dwarf’s gravity. When the white dwarf Stein 2051 B passed in front of a background star, the distant star’s light was offset by only about 2 milliarcseconds from its actual position. This deviation is so small that it is equivalent to observing an ant crawl across the surface of a quarter from 1,500 miles away. From this measurement, astronomers calculated that the white dwarf’s mass is roughly 68 percent of the sun’s mass. Credit: NASA, ESA, and G. Bacon (STScI)

Among astronomers, the findings are significant for at least three reasons, according to Oswalt:

  • First, the research "solves a long-standing mystery about the mass and composition of Stein 2051 B," he says.
  • Second, he notes, "Sahu's team nicely confirms astrophysicist Subrahmanyan Chandrasekhar's 1930 Nobel Prize-winning theory about the relationship between the mass and radius of white dwarf stars. We now know that Stein 2051 B is perfectly normal; it's not a massive white dwarf with an exotic composition, as has been believed for nearly a century."
  • Third, Oswalt concludes, "This new tool for determining masses will be very valuable as huge new surveys uncover many other chance alignments over the next few years."
Hubble astronomers use a century-old relativity experiment to measure a white dwarf's mass
Looks can be deceiving. In this Hubble Space Telescope image, the white dwarf star Stein 2051B and the smaller star below it appear to be close neighbors. The stars, however, reside far away from each other. Stein 2051B is 17 light-years from Earth; the other star is about 5,000 light-years away. Stein 2051B is named for its discoverer, Dutch Roman Catholic priest and astronomer Johan Stein. Credit: NASA, ESA, and K. Sahu (STScI)

For the average star-gazer, he says, the findings are meaningful because "at least 97 percent of all the that have ever formed in the Galaxy, including the Sun, will become or already are white dwarfs - they tell us about our future, as well as our history."

Dr. Terry Oswalt discusses results from a new study by Sahu et al., reporting the first successful measurement of a star’s weight using Einstein’s theory of general relativity. Dr. Oswalt gives a physical demonstration using props to show how a star’s gravity deflects light. Scientists can then use this deflection of light to calculate the weight of star. Credit: Embry-Riddle Aeronautical University / Robert H. Score

More information: K.C. Sahu el al., "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star," Science (2017). … 1126/science.aal2879

"A centennial gift from Einstein," Science (2017). … 1126/science.aan2996

Journal information: Science

Provided by Embry-Riddle Aeronautical University

Citation: New confirmation of Einstein's General Theory of Relativity (2017, June 7) retrieved 29 November 2023 from
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