Some supermassive black holes launch powerful beams of material, or jets, away from them, while others do not. Astronomers may now have identified why.
Using data from NASA’s Chandra X-ray Observatory, ESA’s XMM-Newton, Germany’s ROentgen SATellite (ROSAT), the NSF’s Karl G. Jansky Very Large Array, the Sloan Digital Sky Survey, and other telescopes, researchers have studied more than 700 quasars – rapidly growing supermassive black holes – to isolate the factors that determine why these black holes launch jets.
Jets from supermassive black holes can inject huge amounts of energy into their surroundings and strongly influence the evolution of their environments. Previously, scientists realized that a supermassive black hole needs to be spinning rapidly to drive strong jets – but not all rapidly spinning black holes have jets.
“We found there’s another determining factor of whether a supermassive black hole has jets, something called a black hole corona threaded by magnetic fields,” said Shifu Zhu, a graduate student at Penn State and the leader of the study. “If you don’t have a black hole corona that’s bright in X-rays, it seems like you don’t have powerful black hole jets.”
In astronomy, the term “corona” is commonly associated with the outer atmosphere of the Sun. Black hole coronas, on the other hand, are regions of diffuse hot gas that lie above and below a much denser disk of material swirling around the gravitational sinkhole. Like the corona around the Sun, black hole coronas are threaded with strong magnetic fields.
“It’s like baking bread where you need a few ingredients to successfully follow the recipe for a loaf,” said co-author Niel Brandt, Verne M. Willaman Professor of Astronomy and Astrophysics and professor of physics at Penn State. “Our results show that one ingredient you can’t do without when ‘making’ powerful quasar jets is a bright corona.”
The team obtained their results by gaining a better understanding of X-ray emission from quasars. Previous studies had shown that quasars without jets show a characteristic link between the strength of their X-ray and ultraviolet emission. This correlation is explained by ultraviolet light from the disk of the black hole striking particles in the corona. The resulting energy boost converts the ultraviolet light to X-rays.
In the new study the team chose to investigate the behavior of quasars that do have jets. They found a correlation between how bright the different quasars are in X-rays and ultraviolet light that is remarkably similar to that found for quasars without jets. They concluded that the X-ray emission in the jet-powering quasars is also produced by a black hole corona.
This conclusion was a surprise. Previously, astronomers thought that X-ray emission from quasars with jets comes from the base of the jets because quasars with jets tend to be brighter in X-rays than those without. The new study confirms this difference in brightness, but concludes that the extra X-ray emission is from brighter black hole coronas than those of quasars with weaker or non-existent jets.
“The finding that the X-rays in quasars with jets comes from a black hole corona, rather than from the jets, challenges 35 years of thinking about the basic nature of this emission,” said co-author Guang Yang, a former Penn State graduate student and current postdoctoral researcher at Texas A&M University. “It could provide new insight into the physics of these jets.”
An important implication of their work is that to produce powerful jets a quasar must have a bright black hole corona, threaded by strong magnetic fields, in addition to a rapidly spinning black hole. Quasars with fainter black hole coronas and weaker magnetic fields have less powerful or non-existent jets whether or not their supermassive black holes are spinning quickly.
“Both a quasar’s powerful jets and bright corona occurring together may be fundamentally driven by magnetic fields,” said Zhu.
Stronger magnetic fields may result from a thicker disk caused by a higher rate of matter falling into the black hole.
These results are similar to those found for stellar-mass black holes, which weigh less than a hundred times the mass of the Sun, compared to supermassive black holes that weigh millions or billions of times the Sun’s mass. This supports the idea that these two different classes of black hole may be similar in terms of their behavior despite their very different sizes.
The team’s sample consists of 729 quasars with jets. Chandra, XMM-Newton, and ROSAT data were used for 212, 278, and 239 quasars respectively. The size and quality of the team’s sample explain why they were able to uncover the cause of the X-ray emission.
These results were published in the Monthly Notices of the Royal Astronomical Society on June 20, 2020. The paper is also available online. The other co-authors of the paper, all of whom share a connection to Penn State, are Bin Luo, a former graduate student and postdoctoral researcher who is now a professor at Nanjing University in China, Jianfeng Wu, a former graduate student and current professor at Xiamen University in China, and Y.Q. Xue, a former postdoctoral researcher and current professor at the University of Science and Technology of China in Hefei, China.
NASA’s Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory’s Chandra X-ray Center controls science and flight operations from Cambridge and Burlington, Massachusetts.