AR Scorpii – NASA’s Uniquely Remarkable Binary Star System
A red dwarf star is being ‘lashed’ with high speed electrons that are emanating from a nearby white dwarf star in binary system AR Scorpii.
In May 2015, a group of amateur astronomers from Germany, Belgium and the UK came across a star system that was exhibiting behavior unlike anything they had ever encountered before. Follow-up observations led by the University of Warwick and using a multitude of telescopes on the ground and in space, including the NASA/ESA Hubble Space Telescope, have now revealed the true nature of this previously misidentified system.
The star system AR Scorpii, or AR Sco for short, lies in the constellation of Scorpius, 380 light-years from Earth. It comprises a rapidly spinning white dwarf, the same size as Earth but containing 200 000 times more mass, and a cool red dwarf companion one third the mass of the Sun. They are orbiting one another every 3.6 hours in a cosmic dance as regular as clockwork.
Video courtesy: Space.com
A Dramatic Light Show
In a unique twist, this binary star system is exhibiting some brutal behavior. Highly magnetic and spinning rapidly, AR Sco’s white dwarf accelerates electrons up to almost the speed of light. As these high energy particles whip through space, they release radiation in a lighthouse-like beam which lashes across the face of the cool red dwarf star, causing the entire system to brighten and fade dramatically every 1.97 minutes. These powerful pulses include radiation at radio frequencies, which has never been detected before from a white dwarf system.
Lead researcher Tom Marsh of the University of Warwick’s Astrophysics Group commented: “AR Scorpii was discovered over 40 years ago, but its true nature was not suspected until we started observing it in June 2015. We realised we were seeing something extraordinary the more we progressed with our observations.”
The observed properties of AR Sco are unique. And they are also mysterious. The radiation across a broad range of frequencies is indicative of emission from electrons accelerated in magnetic fields, which can be explained by AR Sco’s spinning white dwarf. The source of the electrons themselves, however, is a major mystery. It is not clear whether it is associated with the white dwarf, or its cooler companion.
White dwarfs form late in the life cycles of stars with masses up to eight times that of our Sun. After hydrogen fusion in a star’s core is exhausted, the internal changes are reflected in a expansion into a red giant. This is followed by a contraction accompanied by the star’s outer layers being blown off in great clouds of dust and gas. A white dwarf is left behind, Earth-sized but 200 000 times more dense. A single spoonful of the matter making up a white dwarf would weigh about an elephant here on Earth.
AR Scorpii was first observed in the early 1970s. Its regular fluctuations in brightness every 3.6 hours led it to be incorrectly classified as a lone variable star. The true source of AR Scorpii’s varying luminosity was revealed thanks to the combined efforts of amateur and professional astronomers. Similar pulsing behavior has been observed before, but from neutron stars rather than white dwarfs.
Boris Gänsicke, co-author of the new study, concludes: “We’ve known about pulsing neutron stars for nearly fifty years. And some theories predicted white dwarfs could show similar behavior. It’s very exciting that we have discovered such a system. And it has been a fantastic example of amateur astronomers and academics working together.”
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