Star Patterns

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

The area on the H-R diagram where “normal” stars can be found is known as the _________.

2) Why are there different brightness of stars and how do we describe their brightness as compared to one another?

It’s called the HR diagram because it tells about the life cycles of stars. By observing and looking at the life cycles of many other stars we can evaluate the date that will tell us all different stages of evolution and growth. While discovering luminosities this helped measure how much energy a star gives off as well as it’s colour that makes categorizing pretty spot on. Because of that a Danish astronomer research combied with russells research based on their spectral types this helped figure out there life cycle of the stars. Even though two women was behind it and it should be named after them but you know how it goes.

14. Why do stars have different levels of brightness, and how does one describe their brightness as compared to one another?

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

Another property of a star is temperature. By measuring the temperature of a star, scientists are able to tell how hot the star is. They use color to measure the temperature of stars. The red ones are the coolest (3,500 K), the yellow ones are warmer (5,000 to 7,000 K), the white ones are warmer still (9,000 to 15,000 K), and the blue ones are the hottest (20,000 to 50,000 K).

They are very luminous stars that have a relatively cool surface temperature compared to the stars in the main sequence that have about the same luminosity. Red giants typically have low to intermediate mass than a regular star, even though they are about 1000 times larger in the red giant phase of stellar evolution. Red supergiants are known as the biggest stars by radius. The biggest red supergiant is mentioned as VY Canis Majoris. This star is about 1800 times bigger than our sun. Although there are plenty of red giants in space, none of them are that close to us. The closest red giant is Gamma Crucis (88 light years away).3

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

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,

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.

A Hertzsprung - Russell diagram is a graph of the luminosity of a star against its colour or surface temperature. With the luminosity being recorded on the vertical axis and the surface temperature on the horizontal axis. The stars are not randomly placed on the H-R graph but contained into specific