Infant stars are glowing gloriously in this infrared image of the Serpens star-forming region, captured by NASA's Spitzer Space Telescope.

At solar system’s birth, no exploding star

U. CHICAGO (US) —New research challenges the notion that the force of an exploding star prompted the formation of the solar system.

The study shows that radioactive isotope iron 60—the telltale sign of an exploding star—was low in abundance and well mixed in solar system material. Cosmochemists look for remnants of stellar explosions in meteorites to help determine the conditions under which the solar system formed.

Some remnants are radioactive isotopes: unstable, energetic atoms that decay over time. Scientists in the past decade have found high amounts of the radioactive isotope iron 60 in early solar system materials.

“If you have iron 60 in high abundance in the solar system, that’s a ‘smoking gun’—evidence for the presence of a supernova,” says Nicolas Dauphas, professor in geophysical sciences at the University of Chicago.

Iron 60 can only originate from a supernova, so scientists have tried to explain this apparent abundance by suggesting that a supernova occurred nearby, spreading the isotope through the explosion.

But the new results, published online in Earth and Planetary Science Letters, are different from previous work: levels of iron 60 were uniform and low in early solar system material. They arrived at these conclusions by testing meteorite samples. To measure iron 60’s abundance, they looked at the same materials that previous researchers had worked on, but used a different, more precise approach that yielded evidence of very low iron 60.

Earlier methods kept the meteorite samples intact and did not remove impurities completely, which may have led to greater errors in measurement. The new approach, however, required that Dauphas and co-author Haolan Tang “digest” the meteorite samples into solution before measurement, which allowed them to thoroughly remove the impurities.

This process ultimately produced results with much smaller errors. “Haolan has dedicated five years of very hard work to reach these conclusions, so we did not make those claims lightly. We’ve been extremely careful to reach a point where we’re ready to go public on those measurements,” Dauphas says.

To address whether iron 60 was widely distributed, Tang and Dauphas looked at another isotope of iron, iron 58. Supernovae produce both isotopes by the same processes, so they were able to trace the distribution of iron 60 by measuring the distribution of iron 58.

“The two isotopes act like inseparable twins: Once we knew where iron 58 was, we knew iron 60 couldn’t be very far away,” Dauphas explains.

They found little variation of iron 58 in their measurements of various meteorite samples, which confirmed their conclusion that iron 60 was uniformly distributed. To account for their unprecedented findings, Tang and Dauphas suggest that the low levels of iron 60 probably came from the long-term accumulation of iron 60 in the interstellar medium from the ashes of countless stars past, instead of a nearby cataclysmic event like a supernova.

If this is true, Dauphas says, there is then “no need to invoke any nearby star to make iron 60.” However, it is more difficult to account for the high abundance of aluminum 26, which implies the presence of a nearby star.

Instead of explaining this abundance by supernova, Tang and Dauphas propose that a massive star (perhaps more than 20 times the mass of the sun) shed its gaseous outer layers through winds, spreading aluminum 26 and contaminating the material that would eventually form the solar system, while iron 60 remained locked inside the massive star’s interior.

If the solar system formed from this material, this alternate scenario would account for the abundances of both isotopes. “In the future, this study must be considered when people build their story about solar system origin and formation,” Tang says.

The research was funded by NASA, the National Science Foundation, and the Packard Foundation.

Source: University of Chicago

chat2 Comments


  1. SnowballSolarSystem

    Iron-58 is stable, so if it’s formed concomitantly with iron-60 in super novae, then then 58Fe is an easily-measured proxy for 60Fe, but if the short-lived radionuclides (60Fe, 26Al et al.) and stable isotopes (58Fe, 16O et al.) of the early solar system formed in a binary stellar merger, luminous red nova (LRN), rather than in a supernova (SN), then the relative proportions of 58Fe and 60Fe may be different than thought.

    An alternative solar system hypothesis suggests that our Sun formed as a binary star that merged at 4.567 Ga.

  2. Steve Koppes

    Thank you for the compliment. All Futurity content is produced by science writers at the respective member institutions of the American Association of Universities. We are not at the moment accepting guest contributions, but we appreciate your offer.

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