Dying star ashes hold clues to carbon in Milky Way
New research sheds light on how and when stars in our galaxy made carbon, "ending up within the raw material from which the sun and its planetary system..."
The final breaths of dying stars called white dwarfs shed light on carbon’s origin in the Milky Way, researchers report.
As dying stars take their final few breaths of life, they gently sprinkle their ashes into the cosmos through the magnificent planetary nebulae. These ashes, spread via stellar winds, are enriched with many different chemical elements, including carbon.
“The findings pose new, stringent constraints on how and when carbon was produced by stars of our galaxy, ending up within the raw material from which the sun and its planetary system were formed 4.6 billion years ago,” says Jeffrey Cummings, an associate research scientist in the Johns Hopkins University physics and astronomy department and coauthor of the study in Nature Astronomy .
The galactic origins of carbon
The origin of carbon, an element essential to life on Earth, in the Milky Way galaxy is still debated among astrophysicists: some are in favor of low-mass stars that blew off their carbon-rich envelopes by stellar winds became white dwarfs, and others place the major site of carbon’s synthesis in the winds of massive stars that eventually exploded as supernovae .
Using data from the Keck Observatory near the summit of Mauna Kea volcano in Hawaii from between August and September 2018, the researchers analyzed white dwarfs belonging to the Milky Way’s open star clusters. Open star clusters are groups of up to a few thousand stars held together by mutual gravitational attraction.
From this analysis, the research team measured the white dwarfs’ masses, and using the theory of stellar evolution, also calculated their masses at birth.
The connection between the birth masses to the final white dwarf masses is called the initial-final mass relation, a fundamental diagnostic in astrophysics that contains the entire life cycles of stars. Previous research always found an increasing linear relationship: the more massive the star at birth, the more massive the white dwarf left at its death.
But when Cummings and his colleagues calculated the initial-final mass relation, they were shocked to find that the white dwarfs from this group of open clusters had larger masses than astrophysicists previously believed. This discovery, they realized, broke the linear trend other studies always found.
In other words, stars born roughly 1 billion years ago in the Milky Way didn’t produce white dwarfs of about 0.60–0.65 solar masses, as it was commonly thought, but they died leaving behind more massive remnants of about 0.7–0.75 solar masses.
Sprinkling ashes in space
The researchers say that this kink in the trend explains how carbon from low-mass stars made its way into the Milky Way. In the last phases of their lives, stars twice as massive as the Milky Way’s sun produced new carbon atoms in their hot interiors, transported them to the surface, and finally spread them into the surrounding interstellar environment through gentle stellar winds.
The research team’s stellar models indicate that the stripping of the carbon-rich outer mantle occurred slowly enough to allow the central cores of these stars, the future white dwarfs, to grow considerably in mass.
The team calculated that stars had to be at least 1.5 solar masses to spread its carbon-rich ashes upon death.
The findings help scientists understand the properties of galaxies in the universe, according to first author Paola Marigo, a professor of physics and astronomy at the University of Padova. By combining the theories of cosmology and stellar evolution, the researchers expect that bright carbon-rich stars close to their death, like the progenitors of the white dwarfs analyzed in this study, are presently contributing to the light emitted by very distant galaxies.
This light, which carries the signature of newly produced carbon, is routinely collected by the large telescopes from space and Earth to probe the evolution of cosmic structures. Therefore, this new understanding of how carbon is synthesized in stars also means having a more reliable interpreter of the light from the far universe.
Additional coauthors are from the Johns Hopkins University; the American Museum of Natural History; the University of Padova; the University of Warwick; the University of California, Santa Cruz; the Université de Montréal; Uppsala University; the International School for Advanced Studies; the Astronomical Observatory of Padova-INAF; the Space Telescope Science Institute; and the University of Geneva.
Funding for the study came from the European Research Council Consolidator Grant and the European Union’s Horizon 2020 research and innovation program.
Source: Johns Hopkins University
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