Chapter 10 Hertzsprung-Russel Diagrams and Distance to Stars
... Discovering whether this was true presented some obvious challenges. Since the distances to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than ...
... Discovering whether this was true presented some obvious challenges. Since the distances to the stars were unknown, one could not determine the intrinsic brightness of a star, but only its apparent brightness. As we’ve already said, a bright star that’s very far away would appear much fainter than ...
An introduction to the HR diagram File
... • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
... • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
The Magnitude scale
... The Magnitude scale Relative brightness on a backwards (!) log scale. Dates to Hipparchus. E.g., apparent relative luminosities of stars a & b are given by, ...
... The Magnitude scale Relative brightness on a backwards (!) log scale. Dates to Hipparchus. E.g., apparent relative luminosities of stars a & b are given by, ...
Stars and Constellations
... brightest stars as they appear on the dates and at the times listed. The line labeled ecliptic shows the apparent path of our Sun through the sky. 3. The horizontal and vertical lines on the chart roughly correspond to latitude and longitude lines on Earth. The horizontal lines are called declinatio ...
... brightest stars as they appear on the dates and at the times listed. The line labeled ecliptic shows the apparent path of our Sun through the sky. 3. The horizontal and vertical lines on the chart roughly correspond to latitude and longitude lines on Earth. The horizontal lines are called declinatio ...
Aspire: Star Life Cycle - Easy Peasy All-in
... 20. Choose a hypothesis and then continue. 21. Where would you expect to find other main sequence stars of the same size on this diagram? (2 Points) 22. Which description of the relationship is correct? (2 Points) 23. Write down the hypothesis that is correct. (2 Points) 24. Determine if the followi ...
... 20. Choose a hypothesis and then continue. 21. Where would you expect to find other main sequence stars of the same size on this diagram? (2 Points) 22. Which description of the relationship is correct? (2 Points) 23. Write down the hypothesis that is correct. (2 Points) 24. Determine if the followi ...
Astro 210 Lecture 4 Sept. 4, 2013 Announcements: • PS 1 available
... from star color → surface temperature T stellar luminosity depends on T but also on star’s radius R: since surface flux F = L/area = σT 4 L = 4πR2σT 4 so for fixed T (same color), L ∝ R2 → bigger stars → bigger emitting surface → higher L ...
... from star color → surface temperature T stellar luminosity depends on T but also on star’s radius R: since surface flux F = L/area = σT 4 L = 4πR2σT 4 so for fixed T (same color), L ∝ R2 → bigger stars → bigger emitting surface → higher L ...
The Hertzsprung-Russell Diagram
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
Stars: flux, luminosity, color, and temperature
... measure the light passing only through the detector. How bright a star looks to us is determined by its flux, not its luminosity. ...
... measure the light passing only through the detector. How bright a star looks to us is determined by its flux, not its luminosity. ...
Part 1—Stages of Human Life
... Arrange these images to match up with those for the life cycle of a human. Describe each stage of the star’s life cycle. ...
... Arrange these images to match up with those for the life cycle of a human. Describe each stage of the star’s life cycle. ...
Constants and Equations
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
... a) AM CVn stars are binary systems with an orbital period of less than 65 minutes. b) AM CVn stars may produce a type II supernova after the white dwarf reaches a critical mass. c) AM CVn stars are sources of gravitational waves. d) AM CVn stars are binary systems where a white dwarf accretes mass f ...
Exercise 4
... 12. d = 1/p = 1/0.0889 = 11.25 pc = 11.25 x 206265 = 2.32 x 106 AU 13. L = 4R2 T4 =A T4, thus L is directly proportional to surface area A. The graph is a straight line through origin. 14. Surface temperature is known from H-R diagram. Radius can be found from L = 4R2 T4. L Apparent brightness ...
... 12. d = 1/p = 1/0.0889 = 11.25 pc = 11.25 x 206265 = 2.32 x 106 AU 13. L = 4R2 T4 =A T4, thus L is directly proportional to surface area A. The graph is a straight line through origin. 14. Surface temperature is known from H-R diagram. Radius can be found from L = 4R2 T4. L Apparent brightness ...
Powerpoint Presentation (large file)
... are glowing, ionized clouds of gas • Emission nebulae are powered by ultraviolet light that they absorb from nearby hot stars • Reflection nebulae are produced when starlight is reflected from dust grains in the interstellar medium, producing a characteristic bluish ...
... are glowing, ionized clouds of gas • Emission nebulae are powered by ultraviolet light that they absorb from nearby hot stars • Reflection nebulae are produced when starlight is reflected from dust grains in the interstellar medium, producing a characteristic bluish ...
ASTRONOMY: WHAT DO YOU NEED TO KNOW
... compressed by the fast gases as the red giant collapses into a white dwarf Know the characteristics and lifespan characteristics of white dwarfs. Does not undergo nuclear fusion but rather contains degenerate matter; contains no gas but radiates energy into space which can take many billions of year ...
... compressed by the fast gases as the red giant collapses into a white dwarf Know the characteristics and lifespan characteristics of white dwarfs. Does not undergo nuclear fusion but rather contains degenerate matter; contains no gas but radiates energy into space which can take many billions of year ...
Death of massive stars
... A black hole is just a dead star with a massive gravitational field. At a reasonably large distance, its gravity is no greater than that of a normal object of similar mass. If the Sun became a black hole, the planets’ orbits would not change at all. ...
... A black hole is just a dead star with a massive gravitational field. At a reasonably large distance, its gravity is no greater than that of a normal object of similar mass. If the Sun became a black hole, the planets’ orbits would not change at all. ...
star
... • Very massive stars can explode in a supernova, which destroys the star. • Iron in the core does not fuse and the core collapses quickly under the force of gravity. • The normal space within atoms is eliminated, leaving a dense core of neutrons, or a neutron star. ...
... • Very massive stars can explode in a supernova, which destroys the star. • Iron in the core does not fuse and the core collapses quickly under the force of gravity. • The normal space within atoms is eliminated, leaving a dense core of neutrons, or a neutron star. ...
Chapter13
... D. Types of Supernovae E. Observations of Supernovae F. The Great Supernova of 1987 G. Local Supernovae and Life on Earth ...
... D. Types of Supernovae E. Observations of Supernovae F. The Great Supernova of 1987 G. Local Supernovae and Life on Earth ...
Objectives
... become hot enough to fuse heavier elements in their core • These shrink very rapidly and rebound with a tremendous shock wave which blows apart the entire shell of the star in an explosion called a… Supernova!!! Star field seen before supernova ...
... become hot enough to fuse heavier elements in their core • These shrink very rapidly and rebound with a tremendous shock wave which blows apart the entire shell of the star in an explosion called a… Supernova!!! Star field seen before supernova ...
