Spectroscopy Research Paper

Spectroscopy is the study of light. A spectrophotometer is a machine used to determine the absorbance of light at any given wavelength. It does this by using a source of white light through a prism, which gives multiple wavelengths that can be individually focused (Ayyagari and Nigam, 2007). Substances are put into cuvettes that are glass or quartz containers that light can easily travel through. The light that is being focused travels through the substance gets absorbed by the

[27] Scientists can determine what a distant star is made of by looking at ____.

Cooler stars emit heat in the infrared area of the electromagnetic spectrum, and thus, they appear to be red. It should also be noted that hot stars radiate energy at the ultraviolet and blue areas, making them appear white or blue. The surface temperature of a celestial object can be determined by using the relationship between the wavelength of the light and the temperature of the blackbody and in the case of an increase in temperature, the tip of the spectrum becomes shorter in

Annie Jump Cannon was most famous for developing a star spectra that is still used today. Many astronomers remember the order of the star spectra by “Oh Be A Fine Girl Kiss Me” (Annie Jump Cannon theorist of star spectra, n.d.). Some people call her the “The Census Taker of the Sky” (drfate0000,2014),and cataloged many stars in her lifetime (Census taker of the sky, 2014). She rearranged Pickering’s order for the star spectra (Annie Cannon, 2015). She examined and classified bright southern hemisphere stars (Annie Jump Cannon theorist of the star spectra,

Primary Calibrators were set up to bounce radar waves throughout the solar system to help determine distances between objects and Earth. Secondary Calibrators were designed to determine brightness of stars from Earth. The method of brightness

By using the line spectrum astronomers can determine the composition of stars by observing the colors that are produce when using a line spectrum and comparing it to known elements and their signature colors on a line spectrum. Each element has a signature color line patter when observed on a line spectrum, because each element has a different number of electrons which give off different amounts of energy when jumping down sub-levels when excited. Scientists can use both of these tests by observing the colors given off, to help them determine the identity of an element, whether in a solid or gaseous

Light is made up of different wavelengths (visible light is made up of the rainbow). If a substance could absorb specific wavelengths of light, then each substance will have a unique ‘fingerprint’. This could be proven by forcing light through a substance and seeing the different wavelengths of light that were displayed on the other side. If there are dark lines, that means that wavelength was missing and was absorbed. A second way to prove this would be to test if that same substance would release the wavelength it absorbed. In the candle experiment, the salt should give off a wavelength because of the intensity of the flame. If it is the same as the sodium street lamp, then that proves sodium will absorb and emit a specific wavelength consistently.

Those stars in the night sky seem small and tiny, but up close they would be millions of times larger than the Earth. Stars are the most recognized astronomical objects and are the building blocks of the galaxies. These luminous spheres made of plasma are responsible for the creation of heavy elements like carbon, nitrogen, and oxygen. They were among the first objects in the early universe. Most of the elements found in the human body originated in stars, this means that we are literally made of stardust. When you are staring at stars from the night sky, you are actually looking back in time, the light you see could be from a million years ago. The study of the birth, life and death of stars are the central field of astronomy today.

The absorption spectra is seen as the black lines when white light is passed through the test sample because the atoms absorb photons, light energy, so that the lower level electrons can move to a higher level, and these wavelength are absorbed in the process. The emission spectra can be seen through the use of a spectrometer as white light is passed through a prism and separates the wavelengths so only the wavelengths of that certain element remains on the photographic film. This comes from when the excited electrons do not have enough energy to remain in the higher energy levels and must return to it original energy level and photon energy is given off, the lines we see in a spectrometer. Both the absorption and emission spectra are forms of line spectra where only few wavelengths are absorbed or released and shown on a spectrum. If you put the absorption and emission spectra together you have a continuous spectra that shows all the wavelengths in the color of the rainbow. The most easiest example of a continuous spectra is white light because it has all

A way to see the color and temperature are where the stars are located. The left of the H R diagram is hot bluish stars and on the right is cooler reddish stars. The way to know which stars are brighter and which stars are dimmer on the diagram are the brighter ones are located near the top and the dim ones are located near the bottom. Depending on if the stars are hot or cold. All you saw at night was a yellow star, but now you know the placement of stars on this diagram which stars are hot which stars are not, the absolute, magnitude , color, temperature and luminosity of stars on an H R

Knowing the properties of the planets, the astronomers can tell the conditions of the planets like their atmosphere, and surface environments especially to the exoplanets because this is the only way,

There is a relationship between what the stars look like and it’s temperature. In the experiment, we observed the temperature, color, and brightness of the light bulb. The color changed and grew brighter when the temperature expanded to a higher rate. The brightness started from a dull red, to an orange, yellow, and ended at a very bright white. The temperature started at 24 degrees and expanded to 40, 60, 80, and grew higher than 110 degrees Celsius. When the colors are darker, a decrease in the temperature; the brighter the colors, an increase in the temperature. A possible error made during the experiment was the thermometer could’ve been moving when put on the beaker and could be farther away from the light bulb then another time in the

The information about stars that Hertzsprung-Russell diagram provides is an important relationship in the understanding study of the stars. It plots the measure of the stars’ intrinsic brightness verves the temperature of stars against their luminosity, or the color of stars against their absolute magnitude. While depending on the main sequence and initial mass, every star goes through specific evolutionary stage and is spoke by its internal structure and how it produces energy.

Wave models of light help us understand the similarities between light and the movement of water to explain properties of light we can 't see. Refer to diagram 2.1 for example. For example of this we can look at a prism. When a white light shines through it, it splits into seven different colors. ROYGBIV: Red, Orange, Yellow, Green, Blue, Indigo, and violet. This is called the visible spectrum.

The spectra of stars have revolutionized our knowledge but there were issues in getting the information that we needed. The earths atmosphere was the biggest issue that was encountered. As light comes through our atmosphere the wavelengths at the shorter end of the spectrum like blue and violet are more easily scattered than longer wavelengths like red, orange, and yellow that are more difficult to scatter. This means that we detect more light that is toward the yellow end of the spectrum rather than the true colors that were actually emitted. To fix the problem we would have to remove the atmosphere. That was not an actual option for scientists, so they had to send telescopes up into space. Once scientists were able to launch the equipment they needed into space they were able to receive the actual spectral patterns for stars. They gathered data in the form