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Automatic Motor Injection Machine Check Indicator Turns On, No Panic … No Panic!


The secret of fast radio bursts (FRB) continues to amaze astronomers. No one is really sure what causes these intense ultrashort radio waves from outer space, but astronomers have now tracked five FRBs back to the original galaxy.

This is the Hubble Space Telescope Appearing with more cargo. Ultraviolet and infrared cameras in telescopes are used to figure out where these five bursts appear on a star map, giving us a better understanding of how they appeared in the first place.

Previously, only about 15 out of a thousand or so FRBs discovered so far have been traced back to specific galaxies, so tracking these bursts is an important indicator of how the phenomenon works.

“Our results are new and exciting,” said astronomer Alexandra Mannings of the University of California, Santa Cruz. “This is the first high-resolution display of a group of FRBs, and Hubble has revealed that five of them are located near or above the spiral arms of the galaxy. Most of these galaxies are large, relatively small, and still form stars. “

“This imaging allows us to get a better idea of ​​the overall characteristics of the host galaxy, such as the mass and rate of star formation, and examine what is happening in person. FRB Its position is because Hubble has extraordinary subtlety. “

The FRB produces energy in thousandths of a second like the Sun does in one year, and the more we find it, the more interesting it becomes. It couldn’t possibly be a connection from a foreign life… could it? (Maybe not, sorry.)

Part of the difficulty in learning these bursts is that they last for milliseconds and rarely repeat. Scientists also don’t really know where to look for the next thing, which makes tracing its origin and cause extremely difficult.

It turns out that these five galaxies originate from the blunter part of the spiral arms around the galaxy, which is what many experts are telling us about. The spiral arms are a gathering place for the hottest and younger stars in the galaxy, but the FRB does not come from the brightest parts of the arm.

Four FRB sites. (NASA, European Space Agency, Alexandra Mannings, Wayne Fei Fung; Image Processing: Alyssa Pagan)

Because we know what types of stars are inside and not in the spiral arm region, the results support the hypothesis that the FRB may come from a ferromagnetic star – a dense star with a very strong magnetic field that might be found at the FRB site Hubble observed. .

“Due to the strong magnetic field, magnets are completely unpredictable,” said astronomer Winning Fei Fung of Northwestern University. “In this case, the FRB is thought to have come from the flare of a young magnetic star.”

“Massive stars undergo stellar evolution and become neutron stars, and some of them can be strongly magnetized, producing flares and magnetic processes on their surfaces, which can emit radio light. Our study fits that description and excludes FRB progenitors who are both fledgling and very young. “

This Hubble-based investigative work is also one step ahead of previous research in linking FRBs to galaxies that have a specific basic structure – in this case, spiral arms. This is a link that hasn’t been clearly established before.

Slowly but surely, experts are gathering some solid information about this elusive pulse of energy being released through space. After identifying this event in 2007, astronomers last year found the first evidence of FRB in our galaxy.

The question of what FRBs actually are and where they come from remains unanswered, but studies like the NASA study are just beginning to rule out some of the possibilities as other people judge them, and the more detailed images we can get from outer space, the better.

“We don’t know what causes the FRB, so it’s very important to use context when we have it,” said Fong. “This technique has succeeded in recognizing the ancestors of other transient types, such as supernovae and gamma ray bursts. Hubble also played a big role in this research. “

This research is not yet published, but will appear on Journal of Astrophysics. Now available as an introductory print at arXiv.org.

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