In our lab report for the this section we learned how to use a diagram created by two discovering astronomers, Ejnar Hertzsprung of Denmark and Henry Norris Russell. This diagram is called the HR Diagram where we use different classifications for stars and plot them on the diagram. To see a full chart of the pattern of stars. During this lab we utilized the HR Diagram Explorer to complete the experiments in our lab. We adjusted the different temperatures (x-axis) and luminosity (y-axis) and were able to see the stars plot on the diagram. This diagram shows the different categories of stars; Supergiants, Main Sequence, Dwarfs and the many others. The stars that where mostly plotted in the middle are the Main Sequence stars. These star make …show more content…
up 90% of the stars. The outliers are Supergiants, Red and Blue Giants, White Dwarfs and red Dwarfs. The stars are also classified by temperature and depending on the range is where they will fall into the Stellar Spectra.
This was created by Annie Cannon; it is a spectra the classifies stars from hottest to coolest. These colors are O’s that are cool, H-R are bluer, M’s are red. These letter correspond with the temperature of the stars. Astronomers use the HR Diagram to learn many different factors of a star. They can analyze the distance, determine its temperature, identify its classification, establish the star luminosity and plot the stars position. All of these factors can be tied into the HR Diagram. In conclusion, this experiment helped me understand the many different items that are relevant to identifying a star. I found it interesting that the stars are all different even in the slightest ways. The most luminous stars are in the upper right section of the HR Diagram. These stars are the most developed stars and are where the Supergiants are mostly populated. These super stars are at the end of there life and are the most evolved. I believe that we can learn the most from these stars. Then that knowledge can then be applied to monitor the younger stars. The information we gather from our stars is; “One small step for man, one giant leap for mankind.” Neil Armstrong; July 20,
1969.
The Star Betelgeuse is classified as the ninth brightest star in the night sky and is the second brightest star in Orion's’ constellation. Betelgeuse is a very unique star in the sky when it is compared to other stars.Betelgeuse is classified as a high mass star. Some introductory facts about the star include its luminosity, which is 140,000 suns, temperature is 3,488 Kelvin, its distance from the sun is 640 light years, radius compared to the sun is 667 times the sun, its apparent magnitude is 0.43, its color on the Hertz sprung- Russell diagram is orange and it is one of the most brightest stars that we have studied. The life of Betelgeuse will be shorter than lower mass stars, which lower mass stars’ lifespan
The purpose of the experiment is to determine the ID of an unknown diprotic acid by establishing its pKa values. The first phase is to determine the unknown diprotic acid by titration, which is a technique where a solution of known concentration is used to determine the molecular weight. While the second phase involved seeing how much NaOH needed to standardize diprotic acid.
However, galactic interactions do often share many characteristics. The most notable feature associated with interacting galaxies is often the “starburst” phenomenon. A starburst is an extremely high rate of star formation over part or all of a galaxy over a cosmologically short period of time (possibly a few billion years as opposed to several billion years). Galaxy interactions cause gravitational instabilities in interstellar gas clouds, which compress the gas in the clouds and trigger star formation (Mouri 2003). When astronomers look at an ongoing starburst in a distant galaxy, they see the starburst as a bluer region than the surrounding parts of the host galaxy. That is due to the extremely hot and energetic, yet short lived, O-type stars produced in the burst, which outshine all of the other stars being born around them as well as the older, redder stars that populate the galaxy.
Although carbon stars are the reddest of the red stars, there are different levels of red in these stars. Astronomers determine a star’s redness by observation and simple math. They measure the star’s magnitude through blue (B) and visual (V) filters. Then they subtract the visual magnitude from the blue. This leaves a number designated B-V called the color index. The more positive the color index, the redder the star is.
Stars are born and reborn from an explosion of a previous star. The particles and helium are brought together the same way the last star was born. Throughout the life of a star, it manages to avoid collapsing. The gravitational pull from the core of the star has to equal the gravitational pull of the gasses, which form a type of orbit. When this equality is broken, the star can go into several different stages. Some stars that are at least thirty times larger than our sun can form black holes and other kinds of stars.
Ever since the early days of human civilization, people gazed up into the sky into the beyond, wondering what secrets the stars held from them. The mass of stars compared to our sun is a frequented question by many astronomers. The answer lies within the luminosity and mass of the star. There are 2 different ways humans can calculate the mass of stars, both using luminosity. One way is to calculate luminosity with radius and temperature of the star being observed. Another much simpler way is to convert apparent magnitude, the brightness of the star observed from earth, to absolute magnitude, the brightness of stars when they are all lined up at the same distance, then convert into luminosity. Once luminosity is calculated, the mass — luminosity relation can be used to find mass.
The Orion Nebula is a spectacular sight. Consequently, it has been a preferred target of the Hubble Space Telescope (HST) over recent years. The HST has provided a great deal of insight into the complicated process of star formation. In June of 1994, C.
AIM: - the aim of this experiment is to find out what the effects of exercise are on the heart rate. And to record these results in various formats. VARIABLES: - * Type of exercise * Duration of exercise * Intensity of exercise * Stage of respiration
Long ago a ancient tribes used the stars to identify different gods and goddesses. Depending on what constellation that was out at night depended on what offerings needed to be made. Like the lion constellation requires a big game offering such as elk or deer and how the libra constellation requires a equal offering of metal and gems.
Tyler, Pat. Supernova. NASA’s Heasarc: Education and Public Information. 26 Jan. 2003. 22 Nov. 2004
A star begins as nothing more than a very light distribution of interstellar gases and dust particles over a distance of a few dozen lightyears. Although there is extremely low pressure existing between stars, this distribution of gas exists instead of a true vacuum. If the density of gas becomes larger than .1 particles per cubic centimeter, the interstellar gas grows unstable. Any small deviation in density, and because it is impossible to have a perfectly even distribution in these clouds this is something that will naturally occur, and the area begins to contract. This happens because between about .1 and 1 particles per cubic centimeter, pressure gains an inverse relationship with density. This causes internal pressure to decrease with increasing density, which because of the higher external pressure, causes the density to continue to increase. This causes the gas in the interstellar medium to spontaneously collect into denser clouds. The denser clouds will contain molecular hydrogen (H2) and interstellar dust particles including carbon compounds, silicates, and small impure ice crystals. Also, within these clouds, there are 2 types of zones. There are H I zones, which contain neutral hydrogen and often have a temperature around 100 Kelvin (K), and there are H II zones, which contain ionized hydrogen and have a temperature around 10,000 K. The ionized hydrogen absorbs ultraviolet light from it’s environment and retransmits it as visible and infrared light. These clouds, visible to the human eye, have been named nebulae. The density in these nebulae is usually about 10 atoms per cubic centimeter. In brighter nebulae, there exists densities of up to several thousand atoms per cubic centimete...
Scientist have placed stars on groups based on how they are the same and how they are different. The brightness of a star depends on their surface temperature so the blue and the white stars
Democritus, a pre-socratic philosopher, is credited with first hypothesizing that the bright band which runs across the night sky may be a close cluster of stars. Democritus lived around the year 400 BC. It wasn’t until the 17th century that Galileo Galilei provided proof that the galaxy was made up of many stars, using an early telescope. Then in the 18th century a man name Thomas Wright postulated that the galaxy what actually a gigantic rotating clus...
From 1922 to 1925 Hubble devised a classification system for galaxies by grouping them according to their content, distance, shape, size, and brightness. The galaxy classification system had become the Hubble morphological (The study of form, structure and the like. ) sequence of galaxy types. Previous to this, no satisfactory system existed, thus Hubble's powerful, yet simple scheme was an incredibly important scientific achievement.