What if the one who shapes the stars

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In sixty-four stage productions , so far - starring in twenty-six of them in London. More results all-star co-star one-star pop star two-star film star five-star See all results. This might sound like a long time, but on an astronomical timescale it is considered a fairly swift process compared, for instance, to the age of the Universe, which is almost 14 billion years. The core contracts until it is around 1, AU Figure 1C.

After 50, years has passed, the system will have formed a disk around the central core, and excess material will be ejected outward from the poles of the star. A pole on a star is like those on the Earth, namely defined as the axis that the star spins around. In Figure 1C , you can see two fountain-like structures where this excess material is ejected. These structures are called jets, and they obey the laws of physics.

The random motion of the gas and dust that we described earlier, combined with the system's contraction as the pre-stellar core forms, will cause the whole system to rotate. This process causes a flat disk to form around the pre-stellar core. This is similar to the way a dress forms a flat disk around a spinning ice-skater. If the skater was not rotating, the dress would not be a flat disk around her, but instead would hang along her sides.

The jets at the poles arise to keep the system in balance. The system is now called a proto-star, which means it is at its very first stage of becoming a real star. The disk is crucial for the proto-star to grow into a properly sized star. The disk is mainly composed of gas, which rotates with the disk and slowly approaches the surface of the proto-star.

When the gas comes close enough to the star, it falls onto the surface of the star because of gravity, and the star grows. This process of growing is called an accretion process and the star is said to accrete accumulate matter from the disk.

Over the next 1, years, the matter from the disk is either accreted by the star or expelled from the disk Figure 1D. The star has grown enough in size and density for the central region to initiate a nuclear reaction, which causes the star to shine, like the Sun. At this point, the star is called a T-tauri star, and this is the first time that the star can be observed visually.

The star eventually stops accreting matter from the disk, but the remaining material around the star is still in a disk-like shape Figure 1E. The disk no longer serves the purpose of feeding the star with matter to make the star grow. Instead, the disk is now just a circular moving plane of material, which will slowly start to clump together and orbit the star.

These small clumps, made from the left-over material from the star's creation, will form new planets. This means that the planets in our solar system are made of the leftover material from the Sun's birth! This is also why all the planets in the solar system are found in the same plane! The final solar system Figure 1F is finished when the disk is completely exhausted, and all the planets are formed. Over the next 10 billion years, the star will burn nuclear fuel in its center and emit energy as the radiation we call sunlight.