796247_Evolution_of-Stars..docx - 1 Astronomy Final Paper...

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1Astronomy Final Paper Project: Evolution of Stars Student’s Name:Institutional Affiliation:Instructor:Due Date:
2Astronomy Final Paper Project: Evolution of Stars The process of the planetary evolution of stars involves a sequence of scientificprocesses. The conditions of the sun in its interior illustrates the internal features of a typicalstar. Star evolution refers to the process that characterizes the changes that a star undergoesover time, which results in an equilibrium state typically known as the main sequence star(Sills et al., 2018). Nuclear fusion powers the existence of every star. Thus the purpose of thisfinal astronomy paper is to critically analyze the evolution of stars and its role in theevolution of philosophical and religious ideas.Hertzsprung-Russel Diagram Showing the Effects of Aging on Stars of Different MassFrom the Hertzsprung-Russel Diagram of the Planetary Nebulae Stage and WhiteDwarfsdiagram above, the clusters of young stars have the entire or a large percentage oftheir members on top of the main sequence. Sills et al. (2018), the rationale behind theevident features of these clusters of actors is that they are still undergoing the process ofcontraction and that they have not attained the level of stability with the entire power
3acquired from the thermonuclear fusion. Ultimately, these clusters of stars would settle on themain sequence. Zero-Age Main SequenceWithin the core, the chemical composition of stars changes gradually as the conversionof hydrogen to helium occurs. In a period of 4.6 million years since the formation of the sun,it has utilized at its center approximately one half of its hydrogen. The gradual progressiveprocess which marks the conversion of hydrogen with the light weight into fewer nuclei withheavier hydrogen is subsequently followed by the gradual changes in the physical factors inthe stellar interior (Eldridge, & Tout, 2018). Also, there are accompanying slow changes inthe surface conditions of the stars in its gradual evolution process. In the due course after allthe hydrogen in the core has been exhausted, then a star is evident making spontaneouschanges under its structure. Thus this gradual process of the stars that marks their aging isscientifically known as stellar evolution. During the onset of the thermonuclear reactions, the chemical composition of a star ischaracterized with homogeneity throughout its interior. The stability structure of such a givenstar has a surface temperature which is warmer and has a luminosity which is smaller than atypical star in that particular position of the main sequence. The locus exhibited by the newlyformed Zero-age main sequence which has chemical homogeneity forms a border to thelower left region of the main sequence (Sills et al., 2018). There is the conversion of theHydrogen with lightweight to a fewer number of nuclei of massive helium as star ages. Forthe maintenance of adequate central pressure for the balancing with gravity, both the central

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Term
Fall
Professor
vdsvs ssdfs
Tags
Stellar Evolution, Stellar classification, main sequence, Sills

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