Researchers have discovered why some white dwarf stars stop cooling, challenging previous understandings and affecting how astronomers determine the age of stars. This finding, stemming from the behavior of solid crystals within the stars, prompts a reevaluation of stellar age assessment and galaxy formation theories. Credit: SciTechDaily.com
New research reveals that white dwarf stars stop cooling due to floating crystals in their interior, offering insights into stellar aging processes.
In a paper published on March 6 in Nature, scholars from the Institute for Advanced Study; the University of Victoria, Canada; and the University of Warwick, U.K., have proposed a new theory that explains why a puzzling population of white dwarf stars stopped cooling for ten billion years.
Open any astronomy textbook to the section on white dwarf stars and you’ll likely learn that they are “dead stars” that continuously cool down over time. The cooling occurs because the white dwarfs have depleted their nuclear heat source. In the classic picture, this causes the dense plasma in a white dwarf’s interior to freeze, leading the star to solidify from the inside out.
Rethinking White Dwarf Star Physics
However, an analysis of data from the European Space Agency’s Gaia satellite, published in 2019 by Sihao Cheng, Martin A. and Helen Chooljian Member in the Institute’s School of Natural Sciences, contradicted this standard picture. It showed that some white dwarfs in fact remain hot for many billions of years (a large portion of the age of the Universe). This finding had confounded theorists, but today’s new paper might provide a compelling explanation.
“In order for these white dwarfs to cease cooling down, they must somehow produce additional energy,” says Cheng, who also contributed to the Nature paper. “Although we were initially uncertain about what this process might be, we now have a clearer understanding of how it occurs.”
This understanding was developed through a collaboration between Cheng, Antoine Bédard of the University of Warwick, and Simon Blouin of the University of Victoria.
Representation of white dwarf star V391 Peg. Credit: Chris Laurel, Celestia
They propose that in some white dwarfs, the dense plasma in the interior does not simply freeze from the inside out. Instead, the solid crystals that are formed upon freezing are less dense than the liquid, and therefore begin to float towards the surface. As the crystals float upwards, they displace the heavier liquid downward. The transport of denser material toward the center of the star releases gravitational energy, and this energy is enough to interrupt the star’s cooling process for billions of years.
“One fascinating aspect of this discovery is that the physics involved is similar to something we observe in daily life: the frozen crystals within the white dwarf star float instead of sink. We might compare their behavior to ice cubes floating in water,” says Cheng.
Why this happens in some white dwarfs and not others is uncertain, but the authors think it is likely due to the composition of the star.
“Some white dwarf stars are formed by the merger of two different stars. When these stars collide to form the white dwarf, it changes the composition of the star in a way that can allow the formation of floating crystals,” says Blouin.
Implications of the Discovery
White dwarfs are routinely used as age indicators: the cooler a white dwarf is, the older it is assumed to be. However, due to the extra delay in cooling found in some white dwarfs, some stars of a given temperature may be billions of years older than previously thought. Better understanding the ages and other aspects of white dwarf stars will help scientists reconstruct the formation of our galaxy.
“Our work will necessitate updates to astronomy textbooks,” adds Cheng. “We hope that it will also prompt astronomers to reassess the methods employed to calculate the age of stellar populations.”
Reference: “Buoyant crystals halt the cooling of white dwarf stars” by Antoine Bédard, Simon Blouin and Sihao Cheng, 6 March 2024, Nature.
DOI: 10.1038/s41586-024-07102-y
The research is supported by the National Sciences and Engineering Research Council of Canada (NSERC), the Banting Postdoctoral Fellowship program, the European Research Council, the Canadian Institute for Theoretical Astrophysics (CITA), and the Institute for Advanced Study’s Fund for Natural Sciences.
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