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Star Formation

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They also do not shine by light that is optical which means that they are observed and investigated by use of IR as well as radio telescopes (Whitworth, Thompson, 2012).Formation of stars starts when the denser regions of the cloud’s core collapse due to their own gravity or weight. The cloud’s core usually has got masses to the tune of 104 solar masses and is mostly in the structure of dust and gas. Being of higher density than the outside clouds, the cores collapse being the first ones. As they collapse, the cores fragment into clumps of about 0.1 parsecs in dimension and in masses of around ten to fifty solar masses. It is these clumps that lead to the formation of protostars, with the whole process taking about ten million years. This is known because many of the cloud cores have got IR sources which give evidence of energy that results from collapsing protostars. This is potential that is later converted into kinetic energy. Another piece of evidence is found in young stars that are bordered by gas clouds, which is the dark molecular cloud leftover. These occur in what is known as clusters-which are groups of stars forming from similar cloud core.The moment a clump breaks free from other regions of cloud’s core, it usually has its own distinct identity and gravity and this is what is known as a protostar. During the formation of protostar, loose gas simultaneously falls into its center. This infalling gas discharges kinetic energy in heat form and the pressure and temperature in the interior of the protostar rises. Thus as its heat draws near thousands of degrees, it is converted into a IR source (Naveed, 2008).During the preliminary collapse, the clump is typically transparent to any radiation and thus the collapsing progresses quite quickly. While the clump becomes denser, it turns opaque. Consequently, trapping of any escaping IR radiation occurs and the pressure and temperature in the middle starts to increase. The pressure later on at some particular point stops the infalling of more gas inside the core and the substance becomes stabilized as a protostar. Initially the protostar has got around 1% of its ultimate mass. However the star’s envelope goes on to develop as infalling substance is accreted (Lee, 2000).Thermonuclear fusion starts in the core of the star once a few million years have elapsed and subsequent production of a

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