A star is burning! How cosmic winds are key to galaxy patterns

Illustration of an acceleration disk around a young star showing the wind of material swirling around it (Image credit: T. Müller, R. Launhardt)

Cosmologists have discovered an important step in the formation of stars, how they prevent the constituent galaxies from escaping. The "rescue mechanic" is the "cosmic wind", which is formed by the accumulation of gas and dust clouds - these clouds gradually accumulate to form hot and dense galaxies. In addition, these clouds can slow down the rotation of stars. A team of scientists led by researchers from the Max Planck Institute used radio waves to observe a young star CB26 460 light-years from Earth in a dark cosmic cloud. Combining observations with a number of analytical techniques, they were able to establish the flow of material around the star CB26. This discovery may reveal how stars form from accreting gaseous clouds without their own regular momentum and rotation.

"Baby stars" are the most unfavorable factor in its composition

Stars begin to burn when cosmic clouds gather under the influence of their own gravity and become too dense. These clouds are made of hydrogen, helium, and some heavy elements - eventually forming what cosmologists call "metals." When the gathered clouds reach a certain density and temperature, a process known as nuclear fusion occurs within them. This cataclysmic process converts hydrogen atoms in the cloud into helium atoms, generating a huge amount of energy, and new stars are born. But there is a key point in this process, that is, the gaseous cloud moves normally, but the flash factor of the cloud actually requires a faster rotation speed.

Think of it like a skier spinning fast in a cosmic arm. The faster the spin, the stronger the inertial centrifugal force that pulls matter away from the axis of rotation at the center of the star. These form "baby stars" - or "protostars" - where enough matter is pulled away from the center of the accretion cloud but not enough to generate nuclear fusion. Cosmologists call this dilemma the conventional momentum problem of star formation.

The answer lies in cosmic winds

A possible solution to this problem is to enter the central region of the accretion cloud to form a gas-dust acceleration disk around the protostar, providing the material that escapes during the rapid rotation necessary to trigger nuclear fusion.

The accelerator disk material also provides momentum for the nova to break away from the protostar. This happens when the hydrogen in the accelerated gaseous rotating material becomes hot. Electrons are separated from the protostar, creating a large number of plasma particles. The movement of these particles creates a magnetic field in the accelerator disk, which in turn affects the plasma streams, some of which even cross the magnetic field lines. These escaping plasma streams eventually collide with the charged neutron star material, carrying some of the material out of the "wind disk" with the momentum of conventional matter.

The loss of conventional momentum stars comes from the gaps in the rapid rotation of the central protostar. The weakening of centrifugal force can solve the conventional momentum problem. This hypothesis has loopholes until the observational evidence appears now. This is also because we are observers located on the earth, and even the twinkling stars appear very small to us.

Even astronauts found evidence 20 years later (2009), when observing the material flow around a CB26 nova (one of the closest disks around the protostar), the Bielue Telescope Array in the Alps, which consists of many individual, large radio telescopes observing separately. Based on the carbon mixture, the research team saw changes in the light escaping from the Earth, this wavelength stretching is called redshift, and the microwaves that are emitted to the Earth are called blueshift.

This shows that the clouds in the acceleration disk are separated from the normal momentum, and this process is like a tornado. In 2009, Launhart and colleagues at the Max Planck Institute could not measure how far the cosmic wind is from the nova. The key point is to understand whether the cosmic wind can transfer enough of the normal running momentum of the nova and keep it from being torn apart. - Stars have their own normal weight when they form - Dark matter atoms may form shadow galaxies when forming stars rapidly - Why is the universe so dark even if it is full of stars?

In the new study, Lauenhart and his team obtained further conclusions and more conclusions about neutron stars. The Max Planck team obtained more conclusions in the observation of radio waves than the team's first observation. The researchers also determined the distribution between wind field matter and field matter using mature model scales.

This is also the first time that the research team has measured the size of the conical material flow. They found that the basic size of the outer flow is three times the distance between the Earth and Neptune, about 8.1 billion kilometers. This also means that the wind field carries more large conventional momentum bodies than the wind - which also provides evidence for how the constant source stars differentiate and evolve. The research team is evaluating the source galaxy of CB26 stars and using it in an upgraded version of the Planck interferometer, which the research team calls "Vault" and has updated the number of antennas to 12. The results of the research were published in the October 17 issue of Cosmos and Cosmology.

BY:Robert Lea

FY: Ho Tan Wai

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