Models describe the mysterious feature of controlling the magnetic properties of the sun

In the late 1980s, scientists found that they could understand the internal characteristics of the sun by observing the waves of sounds that resonate inside it. This technique, known as the Heliosismology, revealed a mysterious vibrant layer in the inner part of the sun, known as the Tachoclin.

The Techcoin is extremely thin but it is believed that it plays an important role in running the magnetic properties of the sun. For years, scientists have done these layers of the sun, calculating and modeling, but the question of the dynamics that leads to the existence of Taekline has been a very complex mathematical puzzle.

Now, researchers from the University of California, Santa Cruz, have developed the first self -interior models of the sun that include proper dynamics and develop a techocront, which has taken an important step forward for solar physics.

Their models were developed using NASA’s most powerful supercomputer, and the results were published The letters of the astronomical journal.

For us on Earth, Touchen is important because of its expected role in the preparation of the sun’s magnetic fields. These fields stimulate events such as solar flare and coronal massive insulations – sun -out -of -the -activity outburst that can destroy global power grid and affect our satellite. Trustently predict when these events will occur, solar entry needs to be modeling properly, especially Touchen.

Far from home, insights about the features of our Sun’s TacoClin can provide the insights of other stars magnetic activity. Scientists believe that the magnetic properties of a star can be very important for the ability to host other planets that maintain life.

“We know a lot of information about the sun, but the sun is just a star,” said Loren Matelsky, the post documentary scholar and the first author of the research.

“We are learning a lot about the dynamics of our sun, and in this process, I think we are also learning how it works on other stars. In the light of other dark systems and explanations, Teachukleine’s questions become more important.”

Extremely thin

At the Baskin School of Engineering, Applied Mathematics Professor Nicholas Bromeile, and a former student of UC Santa Cruz, Lydia Corey, who is now a researcher at Colorado Bolder University, is a researcher at the Center Center.

This large multi -institutional group, which is an important part of UC Santa Cruz, seeks to understand the solar “dinumo”, which is a physical process that creates the magnetic fields of the sun.

Tachukleine plays an important role in the solar dinum, in which it separates two separate regions of the sun. The bottom of the techuchin is a radling zone, which is 70 % of the sun’s inner through radius and strictly rotates the way solid baseball.

The top of the techuleine is the connective zone, which is the largest sun’s largest through the radius, which rotates differently with the gas -feature flow. There is a very thin techuline between these two zones, with large variations at the speed of which potentially play a key role in dinumo.

“Looking at the dynamics initially, you will not expect that the Techcoin will be thin because there are numerous processes that spread the Techukleine when they are left on their own devices – so there is always a huge mystery ‘Why is it so tight?”

For years, researchers have been trying to resolve the mathematical equality of magnetic fluid dynamics for solar geometry so that they can confirm the predictions and models around the technocaline.

But the sun is a very powerful and tumultuous ball of gas, which means that too small (say, 10 meters) to very large (, one million kilometers) has to do a lot of scales with its motivations. Similarly, there is a huge range of relevant time scales. This makes it extremely difficult to model the sun, and past efforts may not be re -prescribed to the realistic dynamic process at work in the solar entry.

The calculation of ‘hero’

In spite of these difficulties, Metalsky, in his words, “welcomed a good challenge.” He and Koree took a large number of “heroes” calculations-excessive complex and major mathematicals, which modeling the physical process more accurately while working in the government.

The past efforts to model the sun have struggled to properly prioritize the physical process that affects solar dinum. This is once again due to the extent of length and time scales on which this process is spread. In this work, for the first time, the team was able to invest in computational resources needed to achieve the correct sequence of dynamics.

Their models are in favor of this process called “Ready Ato Spreading”, which has a tendency to thicken the Techcoin over time, and it is believed that another thickening process is believed to be not in the sunshine called “adhesive spread”.

“Loren and Lydia are doing very painful, huge imitation, where we make the imitation enough and difficult, so that we can lose the vocabulary in favor of more realistic radiation -spreading process,” Bromere said.

When running their refrigerated models, NASA AIMS’s Paleids using a supercomputer for tens of millions of supercompoting hours to provide electricity to their imitation power in 15 months, they managed to create for the first time, a completely independent model of technocracy.

Especially without indicating this, the model of their convective and radiation areas developed a tachocline. Interestingly, these were the forces that were created by the dynamic zone -run dinumo, which was the key to maintaining the thinner of the TacoClin in this model.

“There is a harmony here, because it is believed that Techukleine plays a key role in creating the process of dinumo. Now it seems that it can also be true, in the meantime that the magnetic field from dinumo can create a toss of toucony in the first place.”