Gamma-ray bursts are among the most energetic and explosive events in the universe. They are also short-lived, lasting from a few milliseconds to about a minute. This has made it tough for astronomers to observe a gamma-ray burst in detail.
Using a wide array of ground- and space-based telescope observations, an international team led by University of Maryland astronomers constructed one of the most detailed descriptions of a gamma-ray burst to date. The event, named GRB160625B, revealed key details about the initial “prompt” phase of gamma-ray bursts and the evolution of the large jets of matter and energy that form as a result of the burst. The group’s findings are published in the July 27, 2017 issue of the journal Nature.
“Gamma-ray bursts are catastrophic events, related to the explosion of massive stars 50 times the size of our sun. If you ranked all the explosions in the universe based on their power, gamma-ray bursts would be right behind the Big Bang,” said Eleonora Troja, an assistant research scientist in the UMD Department of Astronomy and lead author of the research paper. “In a matter of seconds, the process can emit as much energy as a star the size of our sun would in its entire lifetime. We are very interested to learn how this is possible.”
The group’s observations provide the first answers to some long-standing questions about how a gamma-ray burst evolves as the dying star collapses to become a black hole. First, the data suggest that the black hole produces a strong magnetic field that initially dominates the energy emission jets. Then, as the magnetic field breaks down, matter takes over and begins to dominate the jets. Most gamma-ray burst researchers thought that the jets were dominated by either matter or the magnetic field, but not both. The current results suggest that both factors play key roles.
“There has been a dichotomy in the community. We find evidence for both models, suggesting that gamma-ray burst jets have a dual, hybrid nature,” said Troja, who is also a visiting research scientist at NASA’s Goddard Space Flight Center. “The jets start off magnetic, but as the jets grow, the magnetic field degrades and loses dominance. Matter takes over and dominates the jets, although sometimes a weaker vestige of the magnetic field might survive.”
The data also suggest that synchrotron radiation—which results when electrons are accelerated in a curved or spiral pathway—powers the initial, extremely bright phase of the burst, known as the “prompt” phase.
“Synchrotron radiation is the only emission mechanism that can create the same degree of polarization and the same spectrum we observed early in the burst,” Troja said. “Our study provides convincing evidence that the prompt gamma-ray burst emission is driven by synchrotron radiation. This is an important achievement because, despite decades of investigation, the physical mechanism that drives gamma-ray bursts had not yet been unambiguously identified.”
Comprehensive coverage of GRB160625B from a wide variety of telescopes that gathered data in multiple spectra made these conclusions possible, the researchers said.
“Gamma-ray bursts occur at cosmological distances, with some dating back to the birth of the universe,” said Alexander Kutyrev, an associate research scientist in the UMD Department of Astronomy and a co-author of the research paper. “The events are unpredictable and once the burst occurs, it’s gone. We are very fortunate to have observations from a wide variety of sources, especially during the prompt phase, which is very difficult to capture.”
NASA’s Fermi Gamma-ray Space Telescope first detected the gamma-ray emission from GRB160625B. Soon afterward, the ground-based MASTER-IAC telescope, a part of Russia’s MASTER robotic telescope network located at the Teide Observatory in Spain’s Canary Islands, followed up with optical light observations while the prompt phase was still active.
MASTER-IAC gathered critical data on the proportion of polarized optical light relative to the total light produced by the prompt phase, providing the crucial link between synchrotron radiation and the prompt phase of this gamma-ray burst.
A magnetic field can also influence how much polarized light is emitted as time passes and the burst evolves. Because the researchers were able to analyze polarization data that spanned nearly the entire timeframe of the burst—a rare achievement—they were able to discern the presence of a magnetic field and track how it changed as GRB160625B progressed.
“There is very little data on polarized emission from gamma-ray bursts,” said Kutyrev, who is also an associate scientist at NASA’s Goddard Space Flight Center. “This burst was unique because we caught the polarization state at an early stage. This is hard to do because it requires a very fast reaction time and there are relatively few telescopes with this capability. This paper shows how much can be done, but to get results like this consistently, we will need new rapid-response facilities for observing gamma-ray bursts.”
In addition to the gamma-ray and optical light observations, NASA’s Swift Gamma-ray Burst Mission spacecraft captured X-ray and ultraviolet data. The Reionization and Transient InfraRed/Optical Project camera—a collaboration between NASA, the University of California system and the National Autonomous University of Mexico installed at Mexico’s Observatorio Astrónomico Nacional in Baja California—captured infrared data.
The group also gathered radio observations from Commonwealth Scientific and Industrial Research Organisation’s Australia Telescope Compact Array, located north of Sydney in rural New South Wales, and the National Radio Astronomy Observatory’s Very Large Array outside of Socorro, New Mexico.
In addition to Troja and Kutyrev, UMD co-authors of this paper include Adjunct Assistant Professor Brad Cenko and Astronomy Graduate Student Vicki Toy.
This research was supported by NASA (Award Nos. NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G, NNH14ZDA001N and NNH15ZDA001N), El Consejo Nacional de Ciencia y Tecnología, Mexico (CONACyT; Award Nos. INFR-2009-01-122785 and CB-2008-101958), the National Autonomous University of Mexico (Award No. IN113810), the University of California Institute for Mexico and the United States-El Consejo Nacional de Ciencia y Tecnología Collaborative Grants Program (UC MEXUS-CONACyT; Award No. CN 09-283), the Russian Science Foundation (Award No. 16-12-00085) and the United Kingdom Space Agency. The content of this article does not necessarily reflect the views of these organizations.