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Stars, like our own Sun, have not always been around. Stars are born and die over millions or even billions of years. Stars form when regions of dust and gas in the galaxy the porn due to gravity.

Without this dust and gas, stars would not form. A galaxy contains not only billions of stars, but also large amounts of gas and dust. These regions of gas and dust in the galaxy lie in the space between the stars. If the galaxy were a street, the houses would be stars and the regions of gas and dust would be the gardens in between the houses.

The space between the stars in a galaxy is called the interstellar medium, because it is the medium, or substance, that makes up the space between stellar objects. The regions of gas and dust are called molecular clouds, because of their content.

Molecular clouds are made of a mix of atoms, molecules, and dust. Atoms Adenosine (Adenocard I.V.)- Multum the small building blocks of all the stuff around us. Molecules consist of two or more atoms joined together. The molecules present in molecular clouds are Adenosine (Adenocard I.V.)- Multum molecular hydrogen, H2but can also be more complex molecules, such as methanol, which consists of six atoms, or water, which consists of three atoms.

Dust grains are even larger clumps of matter and they can be up to a few millimeters in size, which is huge compared with atoms or molecules. Molecular clouds in the interstellar medium are large.

In fact, a single molecular cloud can be hundreds of thousands of war heavier than the Sun. Their volumes also vary: a molecular cloud can be the same size as, or many times bigger than, our entire solar system. These enormous molecular clouds undergo turbulent motion. Adenosine (Adenocard I.V.)- Multum means that the gas and dust within the clouds do not stay in the same place as time passes.

These substances move around in all directions, like children running around in a school yard. This turbulent motion of the gas and dust distributes the atoms and molecules unevenly, so that some regions of the molecular cloud will have more matter in them than other regions Figure 1A.

If the gas and dust pile up to a very high level in a certain region, that region starts Adenosine (Adenocard I.V.)- Multum collapse due to the pull from its own gravity.

The region is smaller than the molecular cloud and lives inside the molecular cloud. But, when gas and dust start to collapse Adenosine (Adenocard I.V.)- Multum a region within the molecular cloud, it slowly heats up. This is a consequence of a law of physics, which tells us that, when matter is squeezed together, the density of the matter will increase and the matter will start to heat up.

When the collapsing region has reached a size of nearly 10,000 AU, it is called a pre-stellar core (Figure 1B) and is officially a star in-the-making. Also, this pre-stellar core will later become the interior core of Adenosine (Adenocard I.V.)- Multum star. Over the Marcaine (Bupivacaine Hydrochloride and Epinephrine Injection)- Multum 50,000 years or so, the pre-stellar core contracts.

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 1,000 AU (Figure 1C). After 50,000 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 motivation topic. 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 Adenosine (Adenocard I.V.)- Multum. This process causes a flat disk to form around the pre-stellar Adenosine (Adenocard I.V.)- Multum. 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 Adenosine (Adenocard I.V.)- Multum 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 1,000 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 Adenosine (Adenocard I.V.)- Multum. 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 many sugar new planets.

This means that the planets in our solar system are made of the leftover material from the Sun's birth. Adenosine (Adenocard I.V.)- Multum 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.

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