Searching for the best black hole recipe
Scientists are tackling this problem by studying the number of black holes in galaxies with different compositions.
December 7, 2012
In this holiday season of home cooking and carefully honed recipes, some astronomers are asking: What is the best mix of ingredients for stars to make the largest number of plump black holes?
NGC 922, located about 157 million light-years from Earth, was formed by the collision between two galaxies. One of these galaxies is shown in this composite image with X-rays from Chandra (red) and optical data from Hubble (appearing as pink, blue, and yellow). // Credit: X-ray (NASA/CXC/SAO/A.Prestwich et al); Optical (NASA/STScI)
They are tackling this problem by studying the number of black holes in galaxies with different compositions. One of these galaxies, the Ring Galaxy (NGC 922), is seen in this composite image containing X-rays from NASA’s Chandra X-ray Observatory (red) and optical data from the Hubble Space Telescope (appearing as pink, yellow, and blue).
NGC 922 formed from the collision between two galaxies — one seen in this image and another located outside the field of view. This collision triggered the formation of new stars in the shape of a ring. Some of these were massive stars that evolved and collapsed to form black holes.
Most of the bright X-ray sources in Chandra’s image of NGC 922 are black holes pulling material in from the winds of massive companion stars. Seven of these are what astronomers classify as “ultraluminous X-ray sources” (ULXs). They are thought to contain stellar-mass black holes that are at least 10 times more massive than the Sun, which places them in the upper range for this class of black hole. They are a different class from the supermassive black holes found at the centers of galaxies, which are millions to billions of times the mass of the Sun.
Theoretical work suggests that the most massive stellar-mass black holes should form in environments containing a relatively small fraction of elements heavier than hydrogen and helium, called “metals” by astronomers. In massive stars, the processes that drive matter away from the stars in stellar winds work less efficiently if the fraction of metals is smaller. Thus, stars with fewer of these metals among their ingredients should lose less of their mass through winds as they evolve. A consequence of this reduced mass-loss is that a larger proportion of massive stars will collapse to form black holes when their nuclear fuel is exhausted. This theory appeared to be supported by the detection of a large number (12) of ULXs in the Cartwheel Galaxy, where stars typically contain only about 30 percent of the metals found in the Sun.
To test this theory, scientists studied NGC 922, which contains about the same fraction of metals as the Sun, meaning that this galaxy is about three times richer in metals than the Cartwheel Galaxy. Perhaps surprisingly, the number of ULXs found in NGC 922 is comparable to the number seen in the Cartwheel Galaxy. Rather, the ULX tally appears to depend only on the rate at which stars are forming in the two galaxies, not on the fraction of metals they contain.
One explanation for these results is that the theory predicting that the most massive stellar-mass black holes should form in metal-poor conditions is incorrect. Another explanation is that the metal fraction in the Cartwheel Galaxy is not low enough to have a clear effect on the production of unusually massive stellar-mass black holes and, therefore, will not cause an enhancement in the number of ULXs. Recent models incorporating the evolution of stars suggest that a clear enhancement in the number of ULXs might only be seen when the metal fraction falls below about 15 percent of the Sun’s value. Astronomers are investigating this possibility by observing galaxies with extremely low metal fractions using Chandra. The number of ULXs is being compared with the number found in galaxies with higher metal content.