Technology NewsSci-Techசக்திவாய்ந்த காஸ்மிக் வெடிப்புகள் பற்றிய நாசா அவதானிப்புகளால் வெளிப்படுத்தப்பட்ட சூப்பர் ஹெவி...

சக்திவாய்ந்த காஸ்மிக் வெடிப்புகள் பற்றிய நாசா அவதானிப்புகளால் வெளிப்படுத்தப்பட்ட சூப்பர் ஹெவி நியூட்ரான் நட்சத்திரங்கள்

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நியூட்ரான் நட்சத்திரங்களை ஒன்றிணைப்பது காமா கதிர்களின் வெடிப்பை உருவாக்குகிறது

இங்கே விளக்கப்பட்டுள்ள நியூட்ரான் நட்சத்திரங்களை ஒன்றிணைப்பது, ஒன்றாக வந்து கருந்துளைக்குள் விழும்போது காமா கதிர்களின் வெடிப்பை உருவாக்குகிறது. நாசாவின் காம்ப்டன் பணியின் இரண்டு வெடிப்புகளின் அவதானிப்புகள் அவற்றின் இறுதி சரிவுக்கு முன், பொருள்கள் சுருக்கமாக ஒரு சூப்பர்சைஸ் செய்யப்பட்ட நியூட்ரான் நட்சத்திரத்தை உருவாக்குகின்றன என்பதைக் குறிக்கிறது. கடன்: நாசாவின் கோடார்ட் விண்வெளி விமான மையம்/CI ஆய்வகம்

ஷார்ட் காமா-ரே பர்ஸ்ட்ஸ் (GRBs) எனப்படும் சக்திவாய்ந்த வெடிப்புகளின் காப்பக அவதானிப்புகளைப் படிக்கும் வானியலாளர்கள், ஒரு சூப்பர் ஹீவியின் சுருக்கமான இருப்பைக் குறிக்கும் ஒளி வடிவங்களைக் கண்டறிந்துள்ளனர்.[{” attribute=””>neutron star shortly before it collapsed into a black hole. This fleeting, massive object likely formed from the collision of two neutron stars.

“We looked for these signals in 700 short GRBs detected with NASA’s Neil Gehrels Swift Observatory, Fermi Gamma-ray Space Telescope, and the Compton Gamma Ray Observatory,” explained Cecilia Chirenti, a researcher at the University of Maryland, College Park (UMCP) and NASA’s Goddard Space Flight Center in Greenbelt, Maryland, who presented the findings at the 241st meeting of the American Astronomical Society in Seattle. “We found these gamma-ray patterns in two bursts observed by Compton in the early 1990s.”

A paper describing the results, led by Chirenti, was published Monday, January 9, in the scientific journal Nature.


இந்த உருவகப்படுத்துதல் இரண்டு சுற்றும் நியூட்ரான் நட்சத்திரங்கள் ஒன்றாக மோதியதால் ஈர்ப்பு அலை மற்றும் அடர்த்தி மாற்றங்களைக் கண்காணிக்கிறது. அடர் ஊதா நிறங்கள் குறைந்த அடர்த்தியைக் குறிக்கின்றன, அதே சமயம் மஞ்சள்-வெள்ளை அதிக அடர்த்தியைக் காட்டுகிறது. கேட்கக்கூடிய தொனி மற்றும் காட்சி அதிர்வெண் அளவுகோல் (இடதுபுறம்) அதிர்வெண்ணின் நிலையான உயர்வைக் கண்காணிக்கும்[{” attribute=””>gravitational waves as the neutron stars close. When the objects merge at 42 seconds, the gravitational waves suddenly jump to frequencies of thousands of hertz and bounce between two primary tones (quasiperiodic oscillations, or QPOs). The presence of these signals in such simulations led to the search and discovery of similar phenomena in the light emitted by short gamma-ray bursts. Credit: NASA’s Goddard Space Flight Center and STAG Research Centre/Peter Hammond

A neutron star forms when the core of a massive star runs out of fuel and collapses. This produces a shock wave that blows away the rest of the star in a supernova explosion. Neutron stars typically pack more mass than our Sun into a ball about the size of a city, but above a certain mass, they must collapse into black holes.

Both the Compton data and computer simulations revealed mega neutron stars tipping the scales by 20% more than the most massive, precisely measured neutron star known – dubbed J0740+6620 – which weighs in at nearly 2.1 times the Sun’s mass. Superheavy neutron stars also have nearly twice the size of a typical neutron star, or about twice the length of Manhattan Island.

Compton Gamma Ray Observatory Deployment

Astronauts imaged the Compton Gamma Ray Observatory during its deployment from space shuttle Atlantis in April 1991. Credit: NASA/STS-37 crew

The mega neutron stars spin nearly 78,000 times a minute – almost twice the speed of J1748–2446ad, the fastest pulsar on record. This rapid rotation briefly supports the objects against further collapse, allowing them to exist for just a few tenths of a second, after which they proceed to form a black hole faster than the blink of an eye.

“We know that short GRBs form when orbiting neutron stars crash together, and we know they eventually collapse into a black hole, but the precise sequence of events is not well understood,” said Cole Miller, a professor of astronomy at UMCP and a co-author of the paper. “At some point, the nascent black hole erupts with a jet of fast-moving particles that emits an intense flash of gamma rays, the highest-energy form of light, and we want to learn more about how that develops.”

Neutron Star Spins in Disk of Gas

In this animation, a neutron star (blue sphere) spins in the center of a colorful disk of gas, some of which follows the magnetic field (blue lines) and flows (blue-white arcs) onto the object’s surface. One interpretation of the quasiperiodic oscillations seen in X-rays in these systems is the formation of a hot spot (white oval) near the disk’s inner edge, which expands and contracts as its properties change. Because of this irregular orbit, the hot spot emission varies within a range of frequencies. Credit: NASA’s Goddard Space Flight Center Conceptual Image Lab

Short GRBs typically shine for less than two seconds yet unleash energy comparable to what’s released by all the stars in our galaxy over one year. They can be detected more than a billion light-years away. Merging neutron stars also produce gravitational waves, ripples in space-time that can be detected by a growing number of ground-based observatories.

Computer simulations of these mergers show that gravitational waves exhibit a sudden jump in frequency – exceeding 1,000 hertz – as the neutron stars coalesce. These signals are too fast and faint for existing gravitational wave observatories to detect. But Chirenti and her team reasoned that similar signals could appear in the gamma-ray emission from short GRBs.

Astronomers call these signals quasiperiodic oscillations, or QPOs for short. Unlike, say, the steady ringing of a tuning fork, QPOs can be composed of several close frequencies that vary or dissipate over time. Both the gamma-ray and gravitational wave QPOs originate in the maelstrom of swirling matter as the two neutron stars coalesce.

While no gamma-ray QPOs materialized in the Swift and Fermi bursts, two short GRBs recorded by Compton’s Burst And Transient Source Experiment (BATSE) on July 11, 1991, and Nov. 1, 1993, fit the bill.

The larger area of the BATSE instrument gave it the upper hand in finding these faint patterns – the tell-tale flickering that revealed the presence of mega neutron stars. The team rates the combined odds of these signals occurring by chance alone at less than 1 in 3 million.

“These results are very important as they set the stage for future measurements of hypermassive neutron stars by gravitational wave observatories,” said Chryssa Kouveliotou, chair of the physics department at George Washington University in Washington, who was not involved in the work.

By the 2030s, gravitational wave detectors will be sensitive to kilohertz frequencies, providing new insights into the short lives of supersized neutron stars. Until then, sensitive gamma-ray observations and computer simulations remain the only available tools for exploring them. 

Reference: “Kilohertz quasiperiodic oscillations in short gamma-ray bursts” by Cecilia Chirenti, Simone Dichiara, Amy Lien, M. Coleman Miller and Robert Preece, 9 January 2023, Nature.
DOI: 10.1038/s41586-022-05497-0

Compton’s BATSE instrument was developed at NASA’s Marshall Space Flight Center in Huntsville, Alabama, and provided the first compelling evidence that gamma-ray bursts occurred far beyond our galaxy. After operating for almost nine years, the Compton Gamma Ray Observatory was deorbited on June 4, 2000, and destroyed as it entered Earth’s atmosphere.

Goddard manages both the Swift and Fermi missions.



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