Stars and Their Formation

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This study will focus on the understanding of stars as well as stars formation. An understanding of star formation and their morphologies are important in various fields of studies such as astrophysics. In this field, for instance, this understanding of the star’s evolution is used to answer several emerging issues related to the universe. Being able to understand the origin of stars must take into consideration the origin of the mass spectrum of the universe (Whitworth and Ward-Thompson 53). Energetic as well as chemistry makes use of knowledge on the star formation, which may later prove to be useful in the application of origin of life not forgetting the evolution of life as well.

Being able to understand the methodologies by which stars form will also increase the understanding of the foundation of their mass spectrum (Spitzer 20). The patterns that determine the flow of matter from the ancient periods of the universe should be understood. Following the formation of stars, they can produce substances that are more in weight that hydrogen through a process known as nuclear reactions (André and Ward-Thompson 56). After completing their life cycle, the stars return into the interstellar medium, where they come together to form larger bodies. At this point, they become a part of the matter that is retained being blocked in the residues.

Ultra-compact sections have been identified as those crucial regions in the initial phases in large mass star formation. At these very early phases, a newly developed large mass star is at very high temperatures and can emit large amounts of ultraviolet photons that can ionize the natural gas that is in the newly formed star environs as well as igniting the ultra-compact regions (Spitzer 20). However, it is observed that although the newly formed stars with large masses are usually formed in groups, a good understanding of the significance of newly developed stars on the surrounding environs is important

The new stars often referred to as protostars mainly develop by undergoing a mass accretion, it is also worth noting that stars with low masses do not attain the high temperatures needed to initiate a nuclear reaction. On the contrary, large mass stars will always produce those high temperatures that enable nuclear reactions while undergoing a process of contraction in a mechanism known as nucleosynthesis. The amount of ultraviolet light produced is due to the activities of the mass. These large activities of the stars cannot accommodate any kind of life in them, unlike the small stars that may be thought of to be able to accommodate life in their extraterrestrial.

The very final phase of stars formation is believed to be dependent on the stellar masses, whereas stars that are regarded to be of ~7Mo or with a value less than this is believed to be described as white dwarves in their nature (Lada 64). The stars that will be of a value~7Mo may end being ejected in the process after the major sequence phase, while four quarters of the weight that will go through the last phase of the red giant as well as the stages of the planetary nebulae (Lada 67). These stars considered to be of high masses are usually thought of to end up exploding like supernovae and as a result, produce a large number of high masses of elements. It is also noted that all the elements that have high masses usually exceeding that of iron is believed to be formed through supernovae.

The cycle of elements and atoms that is dependent on the activities of the stars is collected together in a massive molecular cloud that is seen as enhancements for density in comparatively lesser regions with low temperatures known as dense cores (Lada 66). The masses of the elements in the dense core have a relatively low limit. This is primarily because it is dependent on the jeans mass that is also determined by the temperatures in the cores that are determined by the existence of elements such as carbon monoxide as well as a dipole status that can be attained which is ignited at very low temperatures. The existence of these elements is determined by the presence of those elements that have dense masses that were ejected from the previous cycle of the stars (Prialnik 20).

The supernovae explosions forces out those highest masses of the stars through the interstellar standard and as a result very small remnants are left behind which is always relatively less than 10 percent of the initial mass as observed in the black holes as well as in the neutron stars. Ina very brief summary it is worth concluding that the lass massive a star is the longer it last, on the contrary it is also worth noting that at the end of the stars lifetime, they all undergo the same life cycles(Lada 60 ).

The higher the mass of a star, the shorter is its lifespan. In addition, an increase the mass of a star also increases the portion of matter that ultimately is retained in the interstellar substance that is composed of various elements that will be important in the formation of another generation of stars. As a result, it can be noted that chemical evolution that takes place in the universe is dependent on the activities of the large stars (Bonnell 11).

Giant molecular clouds are described as huge masses of condensed gas mixed with dust that are able to be identified and be mapped down. The giant molecular clouds are mainly composed of hydrogen gas but they can as well be identified in the region occupied by carbon monoxide because the hydrogen gas cannot be ignited at low temperatures (Prialnik 23). Carbon monoxide is the best-identified medium that the hydrogen gas can be diffused and that which is available in large quantities as well.

When stars of large masses have been formed, they can demolish the clouds in a span of a short period. The large masses of the clouds are destroyed by the stars and once the stars are seen to appear like circumstellar masses no longer hold them (Bonnell 11), thought the stars are still in the midst of groups in clicks that can be used to trace their origins (Bonnell 11).

Even though the formation of stars is an ongoing process with a distinctive cycle when the right side of the cloud is observed, it is noted that there exist stars that are relatively not attached to the clouds while not containing the elements that form the clouds. On the contrary, other stars are still attached at the edges of the clouds (Lada 276). The process of the stars formation is still ongoing, and that is the reason that holds to the fact that all the elements are still attached to their original parent cloud (Prialnik 25). These giant molecular clouds are found around the galactic plane; it is thought that the clouds get some support from that prevents it from collapsing, as a free fall would be witnessed due to the effect of gravity (Prialnik 20).

Works Cited

André, Paul and David Ward-Thompson. Proteus and Planets IV. New York, University of New York Press, 2000. Print.

Bonnell, Bate. “Star formation through gravitational collapse and competitive accretion”. Monthly Notices of the Royal Astronomical Society, 370.1 (2003): 488–49. Print.

Lada, Charlton. “Proc. of the NATO Advanced Study Institute on the Physics of Star Formation and Early Evolution- II Crete, Greece”. Sci.Am, 540.38 (2005): 273. Print

Prialnik, Dina. An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University, 2000. Print

Spitzer, Jr. Physical Processes in the Interstellar Medium. New York: Wiley, 2001. Print.

Whitworth, A and David Ward-Thompson. An Empirical Model for Protostellar Collapse. New York, NY: The American Astronomical Society, 2001. Print.

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Stars and Their Formation

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