Star Hertzsprung-Russell Diagram

I pick the star Antares, from the H-R diagram I can tell that it it is a Red Supergiant, and it has a surface temperature that is around 3,000 degrees kelvin, which is cooler than the Sun by at least 2,000 degrees kelvin, but its luminosity is around 10,000 solar units, which means it produces much more energy than our Sun does, so it is a lot brighter. The spectral type of Antares is a M, I could tell that its spectral type was M because I read the H-R Diagram, the VLab told me that the star ‘Betelgeuse’ has a spectral type of M, and Antares is right below, and basically inside Betelgeuse. Stars with the same spectral type have the same chemical composition, so Antares has the chemical composition Ca (calcium), TiO (titanium oxide), CH (methylidene).

In our Milky Way galaxy, there are over a hundred billion stars, and within the universe there are billions of galaxies (Classifying Stars). Astronomers have always come up with different techniques to make their jobs easier. One important technique in, not only astronomy but science itself, is trying to classify something into groups to find a certain pattern. Since there are so many stars in a single galaxy, astronomers must find methods for organization. Stars are not all the same, they vary in size, temperature, and brightness. To keep track of all these different characteristics, astronomers had to come up with a diagram. The Hertzsprung-Russell diagram is one of the most useful plots for stellar astronomy (Classifying Stars). The diagram

5. On what kind of diagram are stars plotted according to their surface temperature and luminosity?

Every clear, cloudless night, away from the bright town lights, the night sky treats us to a dazzling spectacle. Countless twinkling stars shine down from the heavens, sprinkled all around like fairy dust. It’s illustrated right above us much like Michelangelo’s Sistine Chapel. But just like the painting, the display is complex and difficult to understand. There are many different parts of the sky with many different topics to go over. One of those topics is the intricacy of constellations. In order to understand what exactly they are, one must start from the beginning, so the most appropriate place to start off is the birth of a star.

It also has the ability to collect sufficient light from the dim and distant stars. After information was captured, it was then reviewed on a computer. The focus was placed on the black vertical lines known as absorption lines which corresponded with different chemical elements in the outer shell of the star. The information that has been collected and analyzed over the past years shows both halo stars and dim dwarf galaxy stars have weak absorption lines. When the photon energy is close to the energy difference between the lower and higher states, the process is called resonance, this produces high absorption. When the opposite is true, the absorption is small (Frebel,

Today we have new technology that allows us to do many incredible things. One of those things is the ability to calculate the stars, where they will go and where

I can tell many things about the star B-Centauri by looking at this H-R diagram. First of all I can see that it has a temperature of almost 30,000 K, that means it is almost five times hotter than our sun. Next, B-Centauri's luminosity is 10, 000 Lu which means it produces ten thousand times the energy of our sun. I know that B-Centauri is a spectral type O by reading the H-R diagram. During the Vlab we found that Naos was a spectral type O. All stars that are spectral type O are blue, meaning they are the hottest type of stars. Stars of the same spectral type have the same composition. Since Naos has hydrogen, helium, and helium ions so does B-Centauri. The mass of B-Centauri is twenty times the mass of our sun. The radius of B-Centauri

I can tell many things about the star B-Centauri by looking at this H-R diagram. First of all I can see that it has a temperature of almost 30,000 K, that means it is almost five times hotter than our sun. Next, B-Centauri's luminosity is 10, 000 Lu which means it produces ten thousand times the energy of our sun. I know that B-Centauri is a spectral type O by reading the H-R diagram. During the Vlab we found that Naos was a spectral type O. All stars that are spectral type O are blue, meaning they are the hottest type of stars. Stars of the same spectral type have the same composition. Since Naos has hydrogen, helium, and helium ions so does B-Centauri. The mass of B-Centauri is twenty times the mass of our sun. The radius of B-Centauri

This drawing shows the observations of Brahe. It shows 9 stars labeled with the letters from A-I. While some are spread

This episode provides an overview of the composition of stars, and their fate in billions of years. Tyson describes how early man would identify stars via the use of constellations that tied in with various myths and beliefs, such as the Pleiades. Tyson describes the work of Edward Charles Pickering to capture the spectra of multiple stars simultaneously, and the work of the Harvard Computers or "Pickering's Harem", a team of women researchers under Pickering's mentorship, to catalog the spectra. This team included Annie Jump Cannon, who developed the stellar classification system, and Henrietta Swan Leavitt, who discovered the means to measure the distance from a star to the earth by its spectra, later used to identify other galaxies in the

We determined the elements and compounds of the stars by the size and mass of the star. Also where it is located in our solar system. Some stars contained many elements as many as 4 main elements. But some had as little as 2 and 3 main elements. You can tell the temperature by looking on how much energy and light the star gives off. Hotter stars have negative B-V indices, and cooler stars have lower B-V indices. HR diagrams tell you the relationship between a stars temperature and luminosity.

Stars come in a variety of sizes, luminosities, surface temperatures and masses. Through these different characteristics, it is found that there is a pattern (with some special cases). This pattern was first recognized by Danish astronomer Ejnar Hertzsprung and American astronomer Henry Norris Russel during the first decade of the 20th century. They plotted various stars' luminosities on one axis and spectral types on the other. This showed the pattern. These patterns are shown on graphs and are referred to as Hertzsprung-Russel (H-R) diagrams. These types of diagrams are used today still as they are important tools in astronomical research.

Finally, Figure 3 shows Messier 46. This is an open cluster in the constellation of Puppis, which is roughly 5400 light years away. This makes it the closest of the objects by far. As it is an open cluster, there is no clear center of the object. This makes it slightly easier to analyze, as there is no center of light obscuring the individual stars. If we compare it to an image from Jose Luis Martinez, shown below, we can see that there are not too many differences. It is clear that the star structure is very similar, and while Jose’s image is more zoomed and enhanced, there are only a few more stars visible in his. We can see in both images that the stars towards the center of the cluster are slightly larger and more luminous, and it would

The first objects I observed were Albireo, two binary stars. They are about three hundredths to four hundredths and ten light years away. According to Stauffer Mark T from the American Psychological Association, “Albireo’s stunning colors provide a vivid contrast that has earned this double recognition as the most beautiful in the sky. Albireo is easily split using small telescopes at low magnifications, which show a smattering of background stars in addition to the double.” The binary stars known as Albireo is located in the midst of the Summer Triangle formed by Altair, Deneb, and Vega. Although most stars look similar as far color is concerned when observed with the naked eye, they vary in color. Research shows, the primary among the two binary stars is a rich golden orange while the fainter stars’ color resembles a clear sapphire blue light. Their color differences are not simply a contrast because it reflects their real color. According to James Mullaney from Sky & Telescope Media, “Albireo is a wide double; even a

Our night sky, always seems to be sparkling at night, due to stars. Stars are luminous ball of gas, mostly hydrogen and helium, held together by its own gravity. Our night sky is filled with groupings of stars creating a galaxy, or also known as The Milky Way. The Milky Way, is one of many galaxies in a Local Group, containing between 100- 400 billion stars. Observing these stars with the naked eye is sometimes difficult, however technology today has made it much easier. In the experiment “Number the Stars”, we used two different types of telescopes, and a paper towel roll to record different counts of stars in different brightness’s in the sky. Between my partner and I we hypothesized that the larger focal point on the telescope, would