Cosmo Chemistry

Introduction

It is great wonder to discover the things that is beyond the reach of the people. Many scientists participated in the kind of adventure to recognize on how beautiful the earth piroueroutting pivot on its axis. Discovering the composition and the various elements of one matter is the work of the chemists. But the level of knowledge and understanding differs on how the chemists applied it in his nature of work.

Background and Problem Statement

Cosmo chemistry has a duty to discover the things as well as the composition of the elements that is hanging in the universe. There are various evidences that lead to the creation of the solar system and its composition such as the oxygen isotopes, hydrogen isotopes and the carbon isotopes. Based on their knowledge, practice, and the standards that they follow, the chemistry has all the luck to decode the secret that lies in the universe. However, how can a Cosmo chemist discover the composition of the solar system based on their findings on the isotopes and the other element?

Research Objectives

The first objective of the study is to recognize the difficulty in terms of the nature of work includes in the Cosmo chemistry and the various application of the knowledge and experience in the field of their work. The second objective of the study is to recognize the composition of the solar system that is with the oxygen isotopes, hydrogen isotopes and the carbon isotopes.

Research Questions

The study understands the difficulty involved in studying the Cosmo chemistry as well as understanding the various procedures that involved in the field of work. Therefore, the presentation of the several questions can help the study to achieve and meet the objectives.

1. What is the history that lies in discovering the composition of the solar system?

2. What are the influences of the isotopes in the entire system?

3. How can Cosmo chemistry measure the process that the composition plays in building the solar system?

Literature Review

For a very long time, the chemists are continuously working on their duties about assessing the composition of the solar system. From the accumulation of the dust that continuously increasing and aggregates with other chemicals such as calcium aluminum and other isotopes. Due to the reduction of the numerical spread in oxygen isotopic composition, the asteroids and planets are formed. The variations of the oxygen isotopic compositions are many orders of magnitude larger than would be predicted by a simple, random accumulation model that begins in a well-mixed nebula, no matter what size objects are used as the beginning or end points of the calculation. This discrepancy implies either that some as yet unspecified but relatively long-lived process acted on the solids in the solar nebula to increase the spread in oxygen isotopic composition during each and every stage of accumulation, or that the nebula was heterogeneous and maintained this heterogeneity throughout most of its nebular history. Depending on its origin, large-scale nebular heterogeneity could have significant consequences for many areas of Cosmo chemistry, including the application of well-known isotopic systems to the dating of nebular events and the prediction of bulk compositions of planetary bodies on the basis of a uniform cosmic abundance. The evidence supports a scenario wherein the oxygen isotopic composition of nebular solids becomes progressively depleted with time due to chemical processing within the nebula and causing its initial collapse (Nuth and Hill, 2004). Chemists have known for a long time that chemical processes produce isotopic fractionations in hydrogen, carbon, nitrogen, oxygen via chemical reactions predominantly to differences in zero-point energies of the products and in some cases to a shift from an exo- to an endoergic reaction once the heavier isotopes are placed in the reactant molecules. Therefore, by investigating the radiation-induced isotopic enrichment in Solar System ices containing oxygen, carbon, nitrogen, and hydrogen, these studies will also shed light on isotope enrichment processes at an early stage of our Solar System. Similar processes will be studied to simulate the radiation-induced isotopic fractionation in minerals (NASA; and Kuramoto and Yurimoto, 2005).

Methodology

The applied method in the study is the use of the comparative case studies. Various studies can help the study to generate its own findings regarding the composition of the solar system. In addition, the study can gain its position in an advantage for the method allows the study to drive a comprehensive comparison, review on the past literatures, and assess the presentation of the information. The use of the sufficient information is the most valid technique that the study can realize.

References:

Ices in Extraterrestrial Environments, NASA [Online] Available at: http://www.chem.hawaii.edu/Bil301/solidstate.html [Accessed 16 March 2010].

Kuramoto, K., & Yurimoto, H., 2005. Oxygen Isotopic Evolution during the formation and Evolution of the Solar Nebula: Molecular Cloud Origin Hypothesis for the Isotopic Anomaly and its Implications, Workshop on Oxygen in the Earliest Solar System [Online] Available at: http://www.lpi.usra.edu/lpi/c1278Oxygen.pdf [Accessed 16 March 2010].

Nuth, J., & Hill, H., 2004. Palnetary Accretion, Oxygen Isotopes, and the Central Limit Theorem, Meteoritics & Planetary Science, Vol. 39, No. 12 [Online] Available at: http://digitalcommons.library.arizona.edu/objectviewer?o=uadc%3A%2F%2Fazu_maps%2FVolume39%2FNumber12%2Fp1957-1965 [Accessed 16 March 2010].