jackie822 beanerbutt777 life cycle of a star
... http://rigel.csi.cuny.edu/rowan/lectures/Hubble%20Nebulae_files/HelixNebula-HST.jpg ...
... http://rigel.csi.cuny.edu/rowan/lectures/Hubble%20Nebulae_files/HelixNebula-HST.jpg ...
Section 1 Notes on Stars
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
Document
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
Document
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
... chemical reactions. gravitational contraction. helium fusion. hydrogen fusion. nuclear fission. ...
12-1 MAIN-SEQUENCE STARS
... Red dwarfs less massive than about 0.4 solar mass are completely mixed. They cannot ignite a hydrogen-fusion shell, so they cannot become giant stars. Because they have little weight to support and can fuse nearly all of their hydrogen fuel, they will remain on the main sequence for many times the p ...
... Red dwarfs less massive than about 0.4 solar mass are completely mixed. They cannot ignite a hydrogen-fusion shell, so they cannot become giant stars. Because they have little weight to support and can fuse nearly all of their hydrogen fuel, they will remain on the main sequence for many times the p ...
Surveying the Stars
... stars are fusing hydrogen into helium in their cores like the Sun Luminous mainsequence stars are hot (blue) Less luminous ones are cooler (yellow or red) ...
... stars are fusing hydrogen into helium in their cores like the Sun Luminous mainsequence stars are hot (blue) Less luminous ones are cooler (yellow or red) ...
The Milky Way - University of North Texas
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
... b. Objects below this mass can only form in HI clouds. c. Objects below this mass are not hot enough to fuse normal hydrogen. d. They form too slowly and hot stars nearby clear the gas and dust quickly. e. Our telescopes do not have enough light gathering power to detect dim objects. ...
Double Stars in Scorpio`s Claws
... stars that are a rewarding challenge to any astronomer. Some of these are actual double stars (pairs of stars that orbit about each other), others are ‘apparent doubles’ – stars that simply lie along the same line of sight, but are very distant from each other in space. The map below indicates the l ...
... stars that are a rewarding challenge to any astronomer. Some of these are actual double stars (pairs of stars that orbit about each other), others are ‘apparent doubles’ – stars that simply lie along the same line of sight, but are very distant from each other in space. The map below indicates the l ...
JimH This is Your Life - The Atlanta Astronomy Club
... •Sound pitch is lower, light wavelength is longer (redder) ...
... •Sound pitch is lower, light wavelength is longer (redder) ...
Lecture 16
... The star that is now a subgiant was originally more massive. As it reached the end of its life and started to grow, it began to transfer mass to its companion (mass exchange). Now the companion star is more massive. ...
... The star that is now a subgiant was originally more massive. As it reached the end of its life and started to grow, it began to transfer mass to its companion (mass exchange). Now the companion star is more massive. ...
SPECTRAL WORKSHOP
... In the last 15 years or so, telescopes have become powerful enough to observe planets orbiting distant stars. When the planet moves in front of the star, it hides some of the star's light – this can be observed with a back-garden telescope as a periodic decrease in the light from the star. ...
... In the last 15 years or so, telescopes have become powerful enough to observe planets orbiting distant stars. When the planet moves in front of the star, it hides some of the star's light – this can be observed with a back-garden telescope as a periodic decrease in the light from the star. ...
Measuring Stars` Properties - Test 1 Study Guide
... • Many stars come in groups of 2 or 3 that are close (few AU) to each other: BINARY Star Systems • Gravitationally bound and probably formed at the same time • SiriusA is 23 times as bright as our Sun SiriusB is 0.005 times as bright as the Sun Their separation varies from 8 to 31 AU ...
... • Many stars come in groups of 2 or 3 that are close (few AU) to each other: BINARY Star Systems • Gravitationally bound and probably formed at the same time • SiriusA is 23 times as bright as our Sun SiriusB is 0.005 times as bright as the Sun Their separation varies from 8 to 31 AU ...
apparent magnitude - Harding University
... less than the main sequence star, and the spectral line exhibits less pressure broadening. Astonomers have developed 5 luminosity classes, in order of decreasing luminosity: I, II, III, IV, and V, with I signifying supergiants and V main sequence stars. Thus, the complete spectrascopic designation o ...
... less than the main sequence star, and the spectral line exhibits less pressure broadening. Astonomers have developed 5 luminosity classes, in order of decreasing luminosity: I, II, III, IV, and V, with I signifying supergiants and V main sequence stars. Thus, the complete spectrascopic designation o ...
Assignment 7 - Department of Physics and Astronomy
... c. luminosity is proportional to mass to the fourth power (luminosity increases strongly with mass) d. bright stars have more mass around them in the form of planets, comets, and asteroids e. the brightest stars are made of such light materials they hardly have any mass at all ____ 22. For what typ ...
... c. luminosity is proportional to mass to the fourth power (luminosity increases strongly with mass) d. bright stars have more mass around them in the form of planets, comets, and asteroids e. the brightest stars are made of such light materials they hardly have any mass at all ____ 22. For what typ ...
Document
... “H II regions are regions of hot (several thousand K), thin hydrogen emission nebulae that glow from the fluorescence of hydrogen atoms. The roman numeral ``II'' of H II means that hydrogen is missing one electron. A He III nebula is made of helium gas with two missing electrons. A H I nebula is mad ...
... “H II regions are regions of hot (several thousand K), thin hydrogen emission nebulae that glow from the fluorescence of hydrogen atoms. The roman numeral ``II'' of H II means that hydrogen is missing one electron. A He III nebula is made of helium gas with two missing electrons. A H I nebula is mad ...
LAB #5 - GEOCITIES.ws
... the physical reason for these differences in spectra were not understood until the 1930’s and 1940’s. Then it was realized that, while there were some chemical differences among stars, the main thing that determined the spectral type of a star was its surface temperature. Stars with strong lines of ...
... the physical reason for these differences in spectra were not understood until the 1930’s and 1940’s. Then it was realized that, while there were some chemical differences among stars, the main thing that determined the spectral type of a star was its surface temperature. Stars with strong lines of ...
H-R Diagram
... To identify the characteristics of a star from data in the diagram To classify a star by its position in the diagram To compare the life cycle stages of stars based on their positions in the diagram Background The Hertzsprung-Russell diagram, or H-R diagram, is a graph in which a star's temperature ...
... To identify the characteristics of a star from data in the diagram To classify a star by its position in the diagram To compare the life cycle stages of stars based on their positions in the diagram Background The Hertzsprung-Russell diagram, or H-R diagram, is a graph in which a star's temperature ...
Lecture 7
... that stars are still forming. The denotation “ad” in Sa Sd correlates with the amount of gas and young stars. Sa’s have only a small amount of gas and are quite red---their star-forming phase is nearly over, and their average stars are quite old. Sd’s in contrast have a lot of gas and have a long ...
... that stars are still forming. The denotation “ad” in Sa Sd correlates with the amount of gas and young stars. Sa’s have only a small amount of gas and are quite red---their star-forming phase is nearly over, and their average stars are quite old. Sd’s in contrast have a lot of gas and have a long ...
IOSR Journal of Applied Physics (IOSR-JAP) ISSN: 2278-4861.
... of Ref 8 , from different spectral classes of stars. At the use of these intensity ratios J H = 13.595 eV for hydrogen was used. The electron temperatures for different spectral classes have earlier been determined in Tab 1 in Ref 9 . A summary of the values from the spectral classes of this paper i ...
... of Ref 8 , from different spectral classes of stars. At the use of these intensity ratios J H = 13.595 eV for hydrogen was used. The electron temperatures for different spectral classes have earlier been determined in Tab 1 in Ref 9 . A summary of the values from the spectral classes of this paper i ...
Lecture 10 Advanced Variable Star Stuff March 18 2003 8:00 PM
... A white dwarf is the remnant that is left after a star similar to our Sun dies. It blows off all of its outer layers and leaves behind a hot dense core. There is no more fuel for nuclear fusion (the elements left are mainly things like carbon and iron, not easy to fuse). If we add too much fuel, wha ...
... A white dwarf is the remnant that is left after a star similar to our Sun dies. It blows off all of its outer layers and leaves behind a hot dense core. There is no more fuel for nuclear fusion (the elements left are mainly things like carbon and iron, not easy to fuse). If we add too much fuel, wha ...
HR Diagram - TeacherWeb
... A. Which star group does Proxima Centauri belong to? _________________________ B. On the H-R diagram, which star would Proxima Centauri be near? ______________ 8. Describe: Locate the Sun on the H-R diagram. How will the Sun’s luminosity and temperature change as it ages? How will these changes affe ...
... A. Which star group does Proxima Centauri belong to? _________________________ B. On the H-R diagram, which star would Proxima Centauri be near? ______________ 8. Describe: Locate the Sun on the H-R diagram. How will the Sun’s luminosity and temperature change as it ages? How will these changes affe ...
File
... In what other ways can we measure a star’s properties? • Star radii differ greatly – Most are roughly the size of our Sun – Some, like Betelgeuse, are hundreds of times larger. These are Giants – Smaller stars, including our Sun, are Dwarfs, or ...
... In what other ways can we measure a star’s properties? • Star radii differ greatly – Most are roughly the size of our Sun – Some, like Betelgeuse, are hundreds of times larger. These are Giants – Smaller stars, including our Sun, are Dwarfs, or ...
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.