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PPT - University of Delaware
... Usually neglected since speed of light is VERY large Becomes significant in very bright objects – e.g. Lasers, Hot Stars Question is: How big is this force vs. gravity? For the Sun, Mass lost over lifetime ~ 0.01% For hot stars (M = 10 - 50 M) mass can be reduced by ½! ...
... Usually neglected since speed of light is VERY large Becomes significant in very bright objects – e.g. Lasers, Hot Stars Question is: How big is this force vs. gravity? For the Sun, Mass lost over lifetime ~ 0.01% For hot stars (M = 10 - 50 M) mass can be reduced by ½! ...
Unit 12 Guide: Concepts of Earth Science Stars, Galaxies, and the
... 2. What evidence do scientists use to support the Big Bang Theory? Explain the sequence of events predicted by the Big Bang Theory. 3. Explain Hubble’s Law. 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward or away from Eart ...
... 2. What evidence do scientists use to support the Big Bang Theory? Explain the sequence of events predicted by the Big Bang Theory. 3. Explain Hubble’s Law. 4. Compare and contrast the apparent and actual motion of stars. How can scientists know if a star or galaxy is moving toward or away from Eart ...
Answer titese questions on a piece of loose leaf paper.
... to measure distances to nearby stars. Qiini: Think about the thumb demo we didin class.) I I . The Hcrczspiung-Russcll diagram shows the relationship between wliai two charaeteiistios of stars? 12- More than 90% of all stars arc cotisiderx;d stars and can be found in a diagonal path aaoss the center ...
... to measure distances to nearby stars. Qiini: Think about the thumb demo we didin class.) I I . The Hcrczspiung-Russcll diagram shows the relationship between wliai two charaeteiistios of stars? 12- More than 90% of all stars arc cotisiderx;d stars and can be found in a diagonal path aaoss the center ...
Everything Under and Over The Stars
... What are White Dwarfs? White Dwarfs are unstable stars that have a unique mass-radius relationship. This is that The higher the mass, the smaller the radius, thus no stable white dwarf can exist. White dwarfs evolve from other stars with three, four, sometimes higher solar masses. It then swells to ...
... What are White Dwarfs? White Dwarfs are unstable stars that have a unique mass-radius relationship. This is that The higher the mass, the smaller the radius, thus no stable white dwarf can exist. White dwarfs evolve from other stars with three, four, sometimes higher solar masses. It then swells to ...
How Is a Star`s Color Related to Its Temperature?
... will make your own Hertzsprung-Russell diagram. You will see how star brightness, color, temperature, and class are related. ...
... will make your own Hertzsprung-Russell diagram. You will see how star brightness, color, temperature, and class are related. ...
Unit 5 - Stars
... something, so badly. There are so many things that I could do if I only had the money. And when I think that I might be teaching and making money, and still all ...
... something, so badly. There are so many things that I could do if I only had the money. And when I think that I might be teaching and making money, and still all ...
Astronomy
... The mass of a star determines how quickly fusion will occur and therefore how long the star will “live”. ...
... The mass of a star determines how quickly fusion will occur and therefore how long the star will “live”. ...
name - New York Science Teacher
... out the answers to the following questions on the sheet of paper provided to be turned in. 1. Name the brightest star in the known universe. _____________________________ 2. What is its magnitude? ________________________ 3. Are the brightest stars low magnitude or high magnitude? __________________ ...
... out the answers to the following questions on the sheet of paper provided to be turned in. 1. Name the brightest star in the known universe. _____________________________ 2. What is its magnitude? ________________________ 3. Are the brightest stars low magnitude or high magnitude? __________________ ...
ASTR2050 Spring 2005 • In this class we will cover: Brief review
... Evolution off the Main Sequence First: “Low mass” stars (M < 5M!) Hydrogen in core is used up. Temperature in core is not high enough to burn helium. Hydrogen burns in “shell”. Helium core is “degenerate”. H burning He core is very ...
... Evolution off the Main Sequence First: “Low mass” stars (M < 5M!) Hydrogen in core is used up. Temperature in core is not high enough to burn helium. Hydrogen burns in “shell”. Helium core is “degenerate”. H burning He core is very ...
(HR) Diagrams
... 13. Using a Question 10 label, by far the largest population of stars is what type? 14. Using a Question 10 label, the second largest population of stars is what type? 15. When you look at the night sky with your naked eyes, can you see most of the nearest stars to earth? a. Why or why not? ...
... 13. Using a Question 10 label, by far the largest population of stars is what type? 14. Using a Question 10 label, the second largest population of stars is what type? 15. When you look at the night sky with your naked eyes, can you see most of the nearest stars to earth? a. Why or why not? ...
the life cycle of stars
... TYPES OF STARS • A star can be classified as one type of star early in its life, and as a different type of star as it gets older. • A star is classified differently as its properties change. ...
... TYPES OF STARS • A star can be classified as one type of star early in its life, and as a different type of star as it gets older. • A star is classified differently as its properties change. ...
How Is a Star`s Color Related to Its Temperature? - d
... Rigel is blue, and Betelgeuse is red. Capella and our sun are yellow. In this activity you will make your own HertzsprungRussell diagram. You will see how star brightness, color, temperature, and class are related. ...
... Rigel is blue, and Betelgeuse is red. Capella and our sun are yellow. In this activity you will make your own HertzsprungRussell diagram. You will see how star brightness, color, temperature, and class are related. ...
Astronomy – Interpreting Main Sequence Star Data The
... Astronomy – Interpreting Main Sequence Star Data The classification of stars by surface temperature and spectral pattern is a painstaking process requiring the efforts of many scientists from hundreds of observatories around the world. To make it easier to refer to the different types of main sequen ...
... Astronomy – Interpreting Main Sequence Star Data The classification of stars by surface temperature and spectral pattern is a painstaking process requiring the efforts of many scientists from hundreds of observatories around the world. To make it easier to refer to the different types of main sequen ...
main sequence star
... • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainter. • When there is no more energy being emitted (released), they are called ...
... • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainter. • When there is no more energy being emitted (released), they are called ...
Worksheet: Stars and the HR Diagram
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
... Background: The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the br ...
Stellar Classification - Solar Physics and Space Weather
... • Class M has the most number of stars • All red dwarfs are Class M • More than 90% of stars are red dwarfs, such as Proxima Centauri. • M is also host to most giants and some supergiants such as Antares and Betelgeuse. • The spectrum of an M star shows lines belonging to molecules and neutral metal ...
... • Class M has the most number of stars • All red dwarfs are Class M • More than 90% of stars are red dwarfs, such as Proxima Centauri. • M is also host to most giants and some supergiants such as Antares and Betelgeuse. • The spectrum of an M star shows lines belonging to molecules and neutral metal ...
Study Guide Astronomy
... 9. What is the relationship between surface temperature and brightness for main sequence stars on the Hertzsprung-Russell Diagram? ...
... 9. What is the relationship between surface temperature and brightness for main sequence stars on the Hertzsprung-Russell Diagram? ...
Star Life Cycle and classroom textbooks for research!
... Star Life Cycle You need to investigate the life cycle of stars and other objects in the universe. Use the internet and classroom textbooks for research! You may work alone or with a partner and turn in one assignment. You may type your answers directly within this document or in PowerPoint. Turn yo ...
... Star Life Cycle You need to investigate the life cycle of stars and other objects in the universe. Use the internet and classroom textbooks for research! You may work alone or with a partner and turn in one assignment. You may type your answers directly within this document or in PowerPoint. Turn yo ...
Chapter 30
... B. They collapse and become white dwarfs. C. They switch to fission reactions. D. They contract and turn into neutron stars. ...
... B. They collapse and become white dwarfs. C. They switch to fission reactions. D. They contract and turn into neutron stars. ...
Chapter 13 Notes – The Deaths of Stars
... o Very hot, dense layer of non-_____________ hydrogen on the WD surface o Explosive onset of ___________ fusion o Nova explosion ...
... o Very hot, dense layer of non-_____________ hydrogen on the WD surface o Explosive onset of ___________ fusion o Nova explosion ...
Problem set 1 1. The binding energy per nucleon for 56Fe is 8.8MeV
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
AnwerkeyTypes-of-stars-and-HR-diagram
... 2. How does surface temperature of White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors fro ...
... 2. How does surface temperature of White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors fro ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.