From AAS NOVA: ” Maxing Out the Mass of Early Stars”


American Astronomical Society

16 June 2017
Susanna Kohler

An artist’s impression of the first generation of stars forming in our universe. A new study examines just how large some of these early stars could have grown. [NASA/JPL-Caltech/R. Hurt (SSC)]

Primordial supermassive stars might be responsible for the earliest supermassive black holes in our universe. But just how big can a star grow before it inevitably collapses into a black hole?

Artist’s illustration of a high-redshift quasar, a black hole feeding on the material around it. [ESO/M. Kornmesser]

The Puzzle of Distant Quasars

Quasars — supermassive black holes that are actively feeding — have been observed with enormous sizes (billions of solar masses) at very large distances (redshifts of z > 6). These monsters pose a problem: how could they have accreted so much mass in so little time since the beginning of the universe?

One theory is that these black holes formed from the direct collapse of stars. The larger the original star before collapse, the better the chances that the resulting black hole will be able to grow quickly. But even theorized Pop III stars (which have hundreds of solar masses) would have to accrete at rates higher than believed possible to achieve the black-hole masses we observe so quickly. For this reason, the commonly invoked explanation now is supermassive stars.

Early Giants

Supermassive stars are theoretical stars that formed in the very different environment of the early universe.

A composite infrared and X-ray image showing a molecular cloud and newly formed stars around Cepheus B. [X-ray: NASA/CXC/PSU/K. Getman et al.; IR: NASA/JPL-Caltech/CfA/J. Wang et al.]

In ordinary star formation, halos of gas cool primarily due to emission by molecules. When these clouds cool, they fragment and then collapse into normal-sized stars.

In the supermassive star-formation scenario, hydrogen molecules in primordial halos are broken down — possibly by ultraviolet radiation from nearby star formation. This prevents the halos from cooling by molecular emission, instead allowing them to grow to an enormous 107–108 solar masses before they start cooling due to atomic emission. At this point they finally collapse to form a star.

Stars forming via this scenario quickly grow to be very massive, as the halo material falls onto the core at catastrophic rates of 0.01–10 solar masses per year. After a short period of this rapid accretion, the supermassive star then collapses into a black hole due to instability. But how massive could such a star grow before its collapse?

Simulating Growth

To answer this question, a team of scientists led by Tyrone Woods (Monash University, Australia) ran stellar-evolution simulations of the birth, growth, and eventual collapse of accreting, non-rotating supermassive stars. Their simulations included the effects of nuclear burning and captured the hydrodynamics of the instability that causes the stars to collapse into black holes, allowing the authors to follow the whole evolution.

The final mass at collapse of a star as a function of its accretion rate. Most stars collapse due to instability during hydrogen burning. [Woods et al. 2017]

Woods and collaborators found that for accretion rates above 0.1 solar masses per year, the supermassive stars generally collapsed into black holes at masses of 150,000–330,000 solar masses. Since the final mass at collapse grows only logarithmically with accretion rate, the upper end of this range represents an approximate upper limit on the mass of supermassive stars.

This also sets the maximum mass of the supermassive black holes formed by direct collapse of stars in the early universe. At hundreds of thousands of solar masses, these first quasars provide much more plausible seeds than Pop III stars for growing the billion-solar-mass monsters we observe at high redshifts. Supermassive stars may indeed be the key to the formation of the first and most luminous quasars in our universe.


T. E. Woods et al 2017 ApJL 842 L6. doi:10.3847/2041-8213/aa7412

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