Hydrogen Alpha Research Paper

The main point of lecture was to continue discussing about the light spectra and atoms. Specifically, we used the equations and calculated a photon of light’s energy at a certain wavelength. Also, we discussed the light spectrum and how particular wavelengths of light are absorbed by matter.

2- It is impossible to identify all element with the naked eye because they don’t release enough energy, therefore the color is not as visible. Besides, not all elements give a light that it is in the visible part of the spectrum, so we need to use a prism.

When hydrogen is viewed through a spectroscope, a red line appears on the line spectrum. In a line spectrum, the spectrum of an element appears not a band of color, but as a sequence of lines.

For example, hydrogens line spectra emission shows three bands of color, red, light blue, and dark blue. The more lines of a specific color, the more that color is going to be viewed on the flame

Usually an excited state can take the form of the electron bouncing from its start energy level or annual also called the ground state. The excited states that are found in the atoms which are in molecules are really crucial for some chemical reactions. The excited electron does not stay in the excited state for a long time, in a while it goes down back to the ground state. When an electron goes down from the excited state, its energy decreases in the form of light, this process is called emission (What is an Excited

Absorption lines are created when light from something hot like a star passes through a cooler gas, cancelling out the emission lines the chemicals in the gas would normally create. When you look at the spectrum of a star, for example, you can see absorption lines because the star's outer atmosphere is cooler than the central part, explains Watson. in such an analysis of chemical abundances, the wavelength of each line is treated as fixed. However, this is not true when the star is moving towards us (the lines are observed at shorter wavelengths, or 'blueshifted, than those measured in the laboratory) or moving away from us. If the spectrum of a star is red or blue shifted, then you can use that to infer their velocities along the line of sight. During the first half of the 19th century, scientists such as John Herschel, Fox Talbot, and Willam Swan studied the spectra of different chemical elements in flames. Gradually, the idea that each element produces a set of characteristic emission lines has become established. Each element has several prominent, and many lesser, emission lines in a characteristic

Helium makes up about Helium is the second most abundant element in the universe. It was discovered on the sun before it was found on earth. In 1868 a french astronomer, Pierre-Jules-Cesar Janssen noticed a yellow line in the sun’s spectrum while studying a total solar eclipse. With a wavelength of 587.49 nanometers Norman Lockyer realized that this line could not be produced by any element at the time. It was hypothesized that the sun was responsible for this mysterious yellow emission. Lockyer named the unknown element helium.

This was supported by the data collected during the exercise; Neon had multiple lines within every color in the visible spectrum, whereas the other elements generally did not or had fewer than Neon. The emission spectrum for every element was different because every element has a series of shells that are approximately in the same place; when it is heated, the electron moves from a higher orbital to a lower orbital and releases a quanta of energy. When this happens, the emission spectra for each element is produced. Since the number of protons and electrons are different, the quanta required are different and produce a different wavelength. In future experiments, it would be interesting to perform flame tests on different compounds, and see what color the different elements chemically combined with each other

The purpose of this experiment is to use and calibrate a spectroscope, measure the emission spectrum of various gases, and measure the emission spectrum of various metal salts. From the emission spectrum of mercury, a calibration graph can be produced and this graph should be precise because the wavelengths of other unknowns can be found. If the calibration graph is skewed, than the wavelengths will be incorrect.

The precise origin of these 'Fraunhofer lines' as we call them today remained in doubt for many years, until Gustav Kirchhoff, in 1859, announced that the same substance can either produce emission lines or absorption lines. Now scientists had the means to determine the chemical composition of stars through spectroscopy. One of the most dramatic triumph of astrophysical spectroscopy during the 19th century was the discovery of helium. An emission line at 587.6 nm was first observed in the Solar corona during the eclipse of 1868 August 18th, although the precise wavelength was difficult to establish at the time. Two months later, Norman Lockyer used a cleaver technique and managed to observe the Solar prominence without waiting for an eclipse. He noted the precise wavelength of this line, and saw that no known terrestrial elements had a line at this wavelength. He concluded this must be a newly discovered element, and called it 'helium'. Helium was discovered on Earth eventually and showed the same 587.6 nm line. Today, we know that helium is the second most abundant element in the Universe. We also know today that the most abundant element is hydrogen. However, this fact was not obvious at

Spectrophotometry is a method of measurement of matter absorbance at different wave radiation frequencies and lengths (Houck 2015). It covers the magnetic spectrum from 185nm to 15000nm (Gore 2000). In most cases spectrophotometry is based on Beer-Lambert law. The law’s

12. Why do thermonuclear reactions in the Sun take place only in its core? Thermonuclear reactions take place when the nuclei of atoms are fused together due to extreme temperatures (G-13). The temperature of the Suns core is 15.5 X 10^6 and at temperatures above 10 X 10^6 hydrogen fuses into the element helium (hydrogen fusion). Therefore the core is the only place on the Sun where Thermonuclear reactions are able to take place. Additionally the fusion that occurs in the Suns core is enough to account for all of the energy that is emitted to the Sun (326).

Comparing the hydrogen to lithium, hydrogen is an element with little orbitals compared to lithium. Hydrogen has little amounts of energy levels, so its energy is diagram will

Under oxygen-restricted conditions, the mitochondrion has undergone reductive alterations of its content and function. These changes were most likely driven by the independence of ATP generation on oxidative phosphorylation in the mitochondria. These reduced mitochondria are called mitochondrion-related organelles (MROs) (9). There are two types which lack mitochondrial DNA--the hydrogenosome and the mitosome. They are distinguished by the fact that the hydrogenosome has retained ATP-generating capacity and the mitosome has not (5). The anaerobic metabolism performed by the hydrogenosome initially suggested that the organelle might have originated through endosymbiosis with an anaerobic bacterium such as Clostridium. It has subsequently been shown that genes for Cpn10, Cpn60, and Hsp70 are present in the nuclear

Planetary nebulae are often given the connotation PN or PNe for the plural by astronomers and exhibit the final stage of a star's life whose initial size is approximately between 1 and 8 solar masses, where the unused gases and elements left from nuclear fusion are blown away from the remaining core producing a luminous colourful halo around it. These phenomena can be very short lived in astronomical terms, possibly just tens of thousands of years.