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…
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,
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.
Of all the galaxies in the entire Universe these are the closest to our galactic system. About 170,000 light-years away from the Milky Way galaxy lie the Large Magellanic Cloud. With only 15 billion young bright stars, it is just one-quarter the size of our own galaxy. During the winter of 1987, a Canadian astronomer, Ian Shelton, spotted the first naked eye supernova since 1604, the result of a massive explosion. No more exciting and scientifically significant event has occurred over the last decade in science than Supernova 1987A, as it is known. Photographs taken on the night of February 23, 1987, of the Large Magellanic Cloud, a companion galaxy to our own Galaxy, at Canada's southern hemisphere observatory at La Silla, Chile, and at the Siding Springs Observatory in Australia, revealed a 6th-magnitude object where only 12th-magnitude blue supergiant stars had been observed before. Scientists believe that the progenitor of Supernova 1987A is a typical blue supergiant of spectral type B3. Spectra taken in 1977 do not suggest anything unusual happening in the outer layers of the star prior to undergoing the supernova outburst. This is not surprising since the real changes were occurring deep inside in a relatively tiny portion of the star's radius. The Large Cloud is quite important because it is the location of this Supernova 1987A, the exploded star that for a time shone brightly but that is now dim and dead.
2, Alter Dinsmore, Cleminshaw H. Clarence, Philips G John. Pictorial Astronomy. United States: Sidney Feinberg, 1963.
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.
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 an emission nebula because of the O-type and B-type stars contained within it. These high-temperature stars emit ultraviolet (UV) light that ionizes the surrounding hydrogen atoms into protons (H+) and electrons (e-). When the protons and electrons recombine, the electrons enter a higher energy level (n=3). Then, when the electron drops from the n=3 level to the n=2 level, an Hphoton is emitted. 2 This photon has a wavelength of 6563 Å, and therefore corresponds to the red portion of the visible spectrum. It is these H photons which give the nebula the distinctive red color which we see.
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
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
You see the star sparkling in the night and then you spot multiple stars that look like they are meant to form a shape, you connect the stars together and then you slowly get the picture. The pattern or shape in the night sky is called a constellation. There are many constellations, all different shapes and sizes. For example, there are horoscope constellations, or zodiac constellations, Big Dipper, Small Dipper, Pegasus, and etc. These constellations are all different shapes and sizes. But in this paper, there’s a certain type of constellation that will be discussed in this paper and those “certain type” are zodiac constellations. Not all 12 but only six: Taurus, Gemini, Leo, Libra, Sagittarius, and Aquarius. After you’re done with this paper, your knowledge of horoscope constellations will be expanded.
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...
McDaid, Liam . "44 Common Misconceptions About Astronomy." Sacramento City College. N.p., n.d. Web. 12 Nov. 2013. .
Tyler, Pat. Supernova. NASA’s Heasarc: Education and Public Information. 26 Jan. 2003. 22 Nov. 2004