Rotation in the ZAMS: Be and Bn stars
... Figure 3a shows the apparent V=7 magnitude limited counts of dwarf Be stars relative to dwarf B stars. There is an apparent lack of dwarf Be stars cooler than spectral type B7. This could be due to genuine Be stars whose discs are minute and/or too cool for the Hα emission be detectable and/or, to f ...
... Figure 3a shows the apparent V=7 magnitude limited counts of dwarf Be stars relative to dwarf B stars. There is an apparent lack of dwarf Be stars cooler than spectral type B7. This could be due to genuine Be stars whose discs are minute and/or too cool for the Hα emission be detectable and/or, to f ...
Date_________________ TWINKLE, TWINKLE
... the ion’s charge from their element. In addition, the temperature of a star will make the lines of some elements more prominent. Temperature also influences what ions are present too. However, all is not lost! Astronomers can still sort out which elements are present. The overall appearance of a sta ...
... the ion’s charge from their element. In addition, the temperature of a star will make the lines of some elements more prominent. Temperature also influences what ions are present too. However, all is not lost! Astronomers can still sort out which elements are present. The overall appearance of a sta ...
Stars are made of very hot gas. This gas is mostly hydrogen and
... burn helium. As they do these stars get much hotter This extra heat makes the outside of an old blue giant star stretch out further. Remember how hot air balloons stretch out as the air in them gets hotter The only difference between Giant Stars and Super Giant Stars is their size. Super Giant Stars ...
... burn helium. As they do these stars get much hotter This extra heat makes the outside of an old blue giant star stretch out further. Remember how hot air balloons stretch out as the air in them gets hotter The only difference between Giant Stars and Super Giant Stars is their size. Super Giant Stars ...
Star Lifecycle
... neutron star or black hole (most massive stars) Pulsars – Spinning neutron stars that give off pulses of radio sources. Left over from super massive star supernovas. Black Holes – From the most massive stars (More than 40 times bigger than our sun). Nothing can escape the gravity of a black hole ...
... neutron star or black hole (most massive stars) Pulsars – Spinning neutron stars that give off pulses of radio sources. Left over from super massive star supernovas. Black Holes – From the most massive stars (More than 40 times bigger than our sun). Nothing can escape the gravity of a black hole ...
Lives of stars HR
... Stars in the upper right are very large and stars in the lower left are very small. This defines only the SIZE of the star and not the MASS, since the density of stars can be very different. So the branch of stars to the upper right of the MS are giant and supergiant stars. ...
... Stars in the upper right are very large and stars in the lower left are very small. This defines only the SIZE of the star and not the MASS, since the density of stars can be very different. So the branch of stars to the upper right of the MS are giant and supergiant stars. ...
The Life Cycle of Stars Webquest
... Name ______________________________ Per. ______ Date _____________ Continue to read on to the section “The Circle of Life” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. Stars begin their lives as clouds of dust and gas called. 2. What is a proto ...
... Name ______________________________ Per. ______ Date _____________ Continue to read on to the section “The Circle of Life” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. Stars begin their lives as clouds of dust and gas called. 2. What is a proto ...
HR Diagram - Geneva 304
... Stars Star Color and Temperature 1. Stars give off _____ wavelengths of electromagnetic radiation. 2. What is the peak wavelength of a star? 3. A star that is _____ in color is hotter than a yellow star. This means that stars with _____ have a hotter temperature. 4. Stars are referred to as _____ be ...
... Stars Star Color and Temperature 1. Stars give off _____ wavelengths of electromagnetic radiation. 2. What is the peak wavelength of a star? 3. A star that is _____ in color is hotter than a yellow star. This means that stars with _____ have a hotter temperature. 4. Stars are referred to as _____ be ...
answer key
... compare their apparent brightnesses. If you want to know which star would be brighter if the two were side by side? Check their absolute brightnesses.) 8. How do astronomers measure stellar temperatures? They compare the star’s radiation emission curve with that of the hypothetical blackbody. This s ...
... compare their apparent brightnesses. If you want to know which star would be brighter if the two were side by side? Check their absolute brightnesses.) 8. How do astronomers measure stellar temperatures? They compare the star’s radiation emission curve with that of the hypothetical blackbody. This s ...
The Hertzsprung-Russell Diagramm
... The solution to this problem lies in the excitation and ionisation energies of H and Ca. The excitation energy of neutral H is higher than the ionisation energy of Ca. The difference is strong enough, so that almost all of the Ca atoms are ionised (and produce the Ca II-lines), whereas very few neu ...
... The solution to this problem lies in the excitation and ionisation energies of H and Ca. The excitation energy of neutral H is higher than the ionisation energy of Ca. The difference is strong enough, so that almost all of the Ca atoms are ionised (and produce the Ca II-lines), whereas very few neu ...
Brown Dwarfs and M Dwarfs
... failure and its many consequences” • Low mass “objects” do not have stable thermonuclear reactions to heat their cores and halt the gravitational contraction → rapid rotation and degenerate convective cores → secular cooling of the atmosphere. • Cool atmospheres have very low ionization → decoupling ...
... failure and its many consequences” • Low mass “objects” do not have stable thermonuclear reactions to heat their cores and halt the gravitational contraction → rapid rotation and degenerate convective cores → secular cooling of the atmosphere. • Cool atmospheres have very low ionization → decoupling ...
Star Formation
... and spend most of their lives • Once on the main sequence, a star stays in the same location on the H-R diagram until it runs out of fuel and begins to die ...
... and spend most of their lives • Once on the main sequence, a star stays in the same location on the H-R diagram until it runs out of fuel and begins to die ...
HR Diagram and Life of a star
... temp This means that they are very large and can range in size from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium ...
... temp This means that they are very large and can range in size from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium ...
ASTR2050 Spring 2005 •
... • Measuring the masses of stars • Measuring the sizes (radii) of stars ...
... • Measuring the masses of stars • Measuring the sizes (radii) of stars ...
The Sun: Example of Radiation Laws
... Low-mass stars (M < 8M⊙ ) evolve into a red giant phase in which their surfaces expand enormously and also cool, but their interiors shrink and heat. This occurs when the H fuel in the star’s core is depleted. A red giant burns He into C and O. When the He fuel is eventually exhausted, the outer ste ...
... Low-mass stars (M < 8M⊙ ) evolve into a red giant phase in which their surfaces expand enormously and also cool, but their interiors shrink and heat. This occurs when the H fuel in the star’s core is depleted. A red giant burns He into C and O. When the He fuel is eventually exhausted, the outer ste ...
and Concept Self-test (1,2,3,5,6,7,8,9)
... Table at right “V” is measured using “visible” light range (490-590 nm) and “B” blue line sees only “blue” light from 380-480 nm. Star “A”is Rigel, where it is very hot, (30,000 K) so more blue light than yellow. Star (c) is like Betelguese, having more red than blue, being a cooler star at 3000 Kel ...
... Table at right “V” is measured using “visible” light range (490-590 nm) and “B” blue line sees only “blue” light from 380-480 nm. Star “A”is Rigel, where it is very hot, (30,000 K) so more blue light than yellow. Star (c) is like Betelguese, having more red than blue, being a cooler star at 3000 Kel ...
Teacher Guide Lives of Stars
... 112.33(c)-10B: distinguish between nuclear fusion and nuclear fission, and identify the source of energy within the Sun as nuclear fusion of hydrogen to helium. 112.33(c)-11A: identify the characteristics of main sequence stars, including surface temperature, age, relative size, and composition. 112 ...
... 112.33(c)-10B: distinguish between nuclear fusion and nuclear fission, and identify the source of energy within the Sun as nuclear fusion of hydrogen to helium. 112.33(c)-11A: identify the characteristics of main sequence stars, including surface temperature, age, relative size, and composition. 112 ...
Starlight and What it Tells Us
... • Color is directly related to temperature • Temperature is the only determinant of color • Energy per unit area is the same if temperature is the same – If two stars have the same color and distance, difference in brightness is due to difference in size – Dwarf and giant stars are literally dwarfs ...
... • Color is directly related to temperature • Temperature is the only determinant of color • Energy per unit area is the same if temperature is the same – If two stars have the same color and distance, difference in brightness is due to difference in size – Dwarf and giant stars are literally dwarfs ...
Neutron Star - Perry Local Schools
... other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
... other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
Types of Stars http://space.about.com/od/stars/tp/What-Are
... Most stars we see in the night sky maintain a constant brightness (the twinkling we sometimes see is actually an atmospheric effect and not a variation of the star), but some stars actually do vary. While some stars owe their variation to their rotation (like rotating neutron stars, called pulsars) ...
... Most stars we see in the night sky maintain a constant brightness (the twinkling we sometimes see is actually an atmospheric effect and not a variation of the star), but some stars actually do vary. While some stars owe their variation to their rotation (like rotating neutron stars, called pulsars) ...
Life Cycle of Stars
... At each step write a short explanation of what is happening during that stage. Fill the entire poster with you cycle. You may want to sketch it out in your notebook before you start on the poster paper. Due at end of period at back table. Make sure your name is on it. ...
... At each step write a short explanation of what is happening during that stage. Fill the entire poster with you cycle. You may want to sketch it out in your notebook before you start on the poster paper. Due at end of period at back table. Make sure your name is on it. ...
Lecture notes -- pdf file - University of Iowa Astrophysics
... Beta Canum Venaticorum .. 27 light years (a star like the Sun) • Lambda Serpentis … 38 light years (***) • 72 Herculis … 47 light years (***) • 18 Scorpii … 46 light years (the “Solar Twin”) ...
... Beta Canum Venaticorum .. 27 light years (a star like the Sun) • Lambda Serpentis … 38 light years (***) • 72 Herculis … 47 light years (***) • 18 Scorpii … 46 light years (the “Solar Twin”) ...
The Milky Way - Houston Community College System
... difficult. To discover the properties of stars, astronomers have used their telescopes and spectrographs in clever ways to learn the secrets hidden in starlight. The result is a family portrait of the stars. In this chapter you will find answers to five important questions about stars: • How far awa ...
... difficult. To discover the properties of stars, astronomers have used their telescopes and spectrographs in clever ways to learn the secrets hidden in starlight. The result is a family portrait of the stars. In this chapter you will find answers to five important questions about stars: • How far awa ...
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.