XMM-Newton Detects The Dwarf X-Ray Superflare

XMM-Newton detects the dwarf X-ray superfilar of high school, using data from the European Photon Imaging Chamber (EPIC) at the ESA XMM-Newton X-ray Observatory. At the ESA XMM-Newton X-ray Observatory using data from the European Photon Imaging Chamber (EPIC).

Astronomers have detected for the first time a powerful X-ray flare of an ultrafresh spectral-class dwarf L. 3XMM J033158 .9-27392525 (hereinafter J0331-27). The asteroid is about 783 light years away. Within minutes, it receives 10 times more energy from the Sun, which is the most intense flare.

The impression of an artist of the star of El Dwarf, a star with a mass so low that it is actually above the threshold of being a star, was caught in the act of emitting a massive super X-ray flare, as in XMM – from ESA. X-ray space observatory detected by Newton.

Flares are emitted when the magnetic field in a star’s atmosphere becomes unstable and collapses in a simple configuration. In this process, it releases a large part of the energy that has been stored in it. This explosive release of energy suddenly illuminates the glow and this is where the new comments present their greatest enigma.

“This is the most interesting scientific part of the discovery, because we did not expect dwarf stars L to give rise to such outbreaks to store enough energy in their magnetic fields,” said Dr. Astronomer, an institute of the institute. Beat Stelzer said und Astrophysik Tübingen and INAF Osservatorio Astronomico di Palermo.

Energy can only be placed in a star’s magnetic field by charged particles, also known as ionized materials and produced in high temperature environments. However, as a dwarf, J0331-27 has a low surface temperature of only 2,100 K for a star compared to approximately 6,000 K in the Sun.

Astronomers did not think that such a low temperature would be able to produce enough charged particles to feed so much energy in a magnetic field. So is Candram: How is a super flare possible on such a star? This is a good question. We only know that nobody knows, dr. Beat said.

Understanding the similarities and differences between this new superflare and so far unique in the dwarf and flares observed earlier, it is now a priority for the team, which is found in all wavelengths in stars of great mass. But to do this, they need to find more examples.

The burning stars more frequently release less energy each time, while they rarely release El dwarf energy, but again it is a really big event. Why this may be the case remains an open question that needs more research. The discovery of this Superflare The Dwarf is a great example of research based on the XMM-Newton collection.

Which demonstrates the vast scientific potential of the mission. I look forward to the next surprise, Dr. XMM-Newton Project Scientist for ESA. Norbert Shorttel said. The star is high energy, the little sun will surprise scientists. A SMALL STAR, with a mass equal to eight percent of our Sun, was observed to have a very intense (or intense) X-ray flare.

That star is high energy, the little sun will surprise scientists. A SMALL STAR, with a mass equal to eight percent of our Sun, was observed to have a very intense (or intense) X-ray flare. The star, known as J0331-27, belongs to the category of brown-square dwarf L. Its mass is sufficient to trigger only those nuclear reactions that produce the emitted energy.

The discovery by a team led by researchers from the National Institute of Astrophysics, thanks to observations from Essa’s XMM-Newton space telescope, surprised the scientific community. Also important in this case, the contribution of Enaf Palermo to the investigation.

Until now, no one thought that high-energy explosions could be so powerful that they could be caused by a star of such a small mass. The brightness of the X-rays produced by J0331-27 was seen on July 5, 2008 from the Epic (European Photon Imaging Camera) written on the blackboard of the observatory for XM-Newton radiography.

Within a few minutes, the smallest star has released ten times more energy than the most intense flares emanating from the Sun. Current theories indicate that triggers are triggered by the sudden release of magnetic energy generated within the star.

This causes the charged particles to heat the plasma on the star surfaces, releasing this large amount of radiation in the optical and ultraviolet systems, and in the X-ray process you release a large amount of energy stored in the star.

It is precisely in this regard that new observations have made the puzzle the largest for scientists, as they did not expect the dwarf for the brown L to store enough energy in its magnetic fields to produce explosions of this magnitude. Giving birth to The reason for this is that energy can only be placed in a star’s magnetic field by charged particles, also known as ionized matter.

This material is made in high-temperature environments, but J0331-27, the class for which the temperature is too low for a star, is only 2,100 Kelvin (compared to 6,000 Kelvin from the Sun). At these temperatures, it was thought that it was not possible to generate charged particles, enough to feed as much energy into the magnetic field.

Beit Stelzer from the Institute of Astronomy and Astrophysics at the University of Tübingen in Germany says: “This is the most scientifically interesting discovery, and now it is applied at Inaf Palermo. The researcher is on the team he studied, which is astronomy and astronomy Posted in Physics magazine.

How is it possible, then, that a star is so cold that it is capable of causing such a flash? There is still a definitive answer to this question. Only one flare was recorded in J0331-27, even though the star observed Axum Newton for a total of 3.5 million seconds, which is about a thousand hours.

“It seems like the fact that an L-class brown dwarf uses more than one star to accumulate energy, which is then suddenly released with a large magnitude,” says Stelzer. Super-Flare was discovered within the framework of the project by analyzing XMM-Newton’s vast catalog of nearly 400,000 X-ray sources, funded by Xtra, the European Union, and coordinated by Andrea de Luca, Inaf, Milan.

The team, in search of special phenomena, has found “bread with J0331-27” for their teeth. Similar to this, it was observed that some stars have a very powerful flare in the visible radiation band, but this is the first detection of the disparity. A super flare wavelength is important in X-rays because it indicates which region of the star’s atmosphere the super flare is coming from.

Light in the optical range comes from the deepest layers of the star’s atmosphere, from the area around its visible surface, while X-rays are generated in the highest region of the atmosphere. Understanding the similarities and differences between this new super style and what was seen previously is now a priority for the team. But to do this, the key is to find other similar events.

“There’s still a lot to discover in the archives,” says De Luca, “in a sense, I think it’s the tip of the iceberg.” “The Republic will always fight against its readers and against all those who have principles of democracy and civil coexistence in defense of freedom of information.”

The findings were published in the journal Astronomy and Astrophysics.

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