4 x What Powers the Sun? • Need to provide
... Stellar Evolution Here: Evolution through nuclear burning. Minitial > 2M Minitial < 2M ...
... Stellar Evolution Here: Evolution through nuclear burning. Minitial > 2M Minitial < 2M ...
Stellar Evolution - Harnett County High Schools Wiki
... When all the hydrogen in a star’s core is gone, star has a helium center and the outer layers have mostly hydrogen gas Some hydrogen will continue to undergo reactions in the outermost layer of the helium core; energy produced in this layer forces out layers of the star to expand and cool The star h ...
... When all the hydrogen in a star’s core is gone, star has a helium center and the outer layers have mostly hydrogen gas Some hydrogen will continue to undergo reactions in the outermost layer of the helium core; energy produced in this layer forces out layers of the star to expand and cool The star h ...
Stars_and_Galaxies
... Neutron star or Black hole: neutron star is the collapsed core of the supernova; a black hole forms when the remaining core is 3 times more massive than the Sun ...
... Neutron star or Black hole: neutron star is the collapsed core of the supernova; a black hole forms when the remaining core is 3 times more massive than the Sun ...
P1_Physics_Summary_Topic_3
... Compare and contrast theories about the beginning of our universe including steady state theory and big bang theory What are the different ways we can explore space? (Include information about SETI) ...
... Compare and contrast theories about the beginning of our universe including steady state theory and big bang theory What are the different ways we can explore space? (Include information about SETI) ...
ppt - Wladimir Lyra
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
Jeopardy
... The gravitational force between objects in our solar system depend on what 2 things? ...
... The gravitational force between objects in our solar system depend on what 2 things? ...
Twinkle, Twinkle Little Star
... gas and dust in my Solar Nursery and begins to Shine! When the cool masses of dust and gas combine, a star has a temperature of 1,800,000 degrees F! http://www.virginmedia.com/images/ ...
... gas and dust in my Solar Nursery and begins to Shine! When the cool masses of dust and gas combine, a star has a temperature of 1,800,000 degrees F! http://www.virginmedia.com/images/ ...
Review 2
... Internal structure of our Sun and its chemical composition. What is the convection zone on the Sun and what are the granules and supergranules? What is the temperature in the Sun’s core? What is the photosphere, chromosphere and corona? What is their temperature and what causes their color? What is ...
... Internal structure of our Sun and its chemical composition. What is the convection zone on the Sun and what are the granules and supergranules? What is the temperature in the Sun’s core? What is the photosphere, chromosphere and corona? What is their temperature and what causes their color? What is ...
Chapter 5 Mid-term Study Guide
... Part A 1–8. Number the steps to show the sequence of a star’s life. Write the correct number on the line before each step. ______ A small star becomes a white dwarf, and a large star becomes a neutron star or black hole. ______ The star collapses again and then explodes as a nova or supernova. _____ ...
... Part A 1–8. Number the steps to show the sequence of a star’s life. Write the correct number on the line before each step. ______ A small star becomes a white dwarf, and a large star becomes a neutron star or black hole. ______ The star collapses again and then explodes as a nova or supernova. _____ ...
Document
... II. Arrange the sentences in the correct order, according to the text on page 14. a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars a ...
... II. Arrange the sentences in the correct order, according to the text on page 14. a. The latter has a diameter of almost two billion miles. b. If you counted one star a second it would take you more than thirty thousand years to count 100 billion. c. But, during your lifetime, as always, new stars a ...
Planets in Strange Places
... The stars, called R 66 and R 126, are respectively 30 and 70 times the mass of the Sun, “about as massive as stars can get,” said Joel Kastner, professor of imaging science at the Rochester Institute of Technology in New York. R 126 is so luminous that if it were placed 10 parsecs (32.6 light-years) ...
... The stars, called R 66 and R 126, are respectively 30 and 70 times the mass of the Sun, “about as massive as stars can get,” said Joel Kastner, professor of imaging science at the Rochester Institute of Technology in New York. R 126 is so luminous that if it were placed 10 parsecs (32.6 light-years) ...
![Lectures 10 & 11 powerpoint (stellar formation) [movie below]](http://s1.studyres.com/store/data/008083226_1-fec717da713794a7feea61d4eec0ceb1-300x300.png)
Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... all layers above, everywhere in the star. This is why we find stable stars on such a narrow strip (main sequence) in the Hertzsprung-Russell diagram. ...
... all layers above, everywhere in the star. This is why we find stable stars on such a narrow strip (main sequence) in the Hertzsprung-Russell diagram. ...
formation of stars
... Background: An average cloud is about 25 lightyears in diameter and may contain enough material to form many stars. A force from outside the cloud [shockwave from a supernova] causes the cloud to begin to condense into stars by triggering the force of gravity that exists between the gas atoms and du ...
... Background: An average cloud is about 25 lightyears in diameter and may contain enough material to form many stars. A force from outside the cloud [shockwave from a supernova] causes the cloud to begin to condense into stars by triggering the force of gravity that exists between the gas atoms and du ...
Outline2a
... Eventually, the proto-star will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
... Eventually, the proto-star will fuse hydrogen in its core. This energy will greatly increase the radiation pressure that the photons create on their surroundings. A stellar wind will begin to blow material away. ...
Stellar Evolution after the Main Sequence
... • While the force of gravity has not been stopped, the gravitational collapse has been halted • The star will remain in this state for several billion years or more, depending on its mass ...
... • While the force of gravity has not been stopped, the gravitational collapse has been halted • The star will remain in this state for several billion years or more, depending on its mass ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
... The star reaches the peak of the red giant branch in the HR-diagram at the time when the core becomes dense and hot enough to start converting helium to carbon through the triple-alphaprocess, 3 4 He→12 C. This results in that the core starts to expand again and the outer hydrogen burning shell decr ...
... The star reaches the peak of the red giant branch in the HR-diagram at the time when the core becomes dense and hot enough to start converting helium to carbon through the triple-alphaprocess, 3 4 He→12 C. This results in that the core starts to expand again and the outer hydrogen burning shell decr ...
Day 2
... Finally, the rate of fusion becomes high enough to establish gravitational equilibrium. At this point, fusion becomes self-sustaining and the star settles into its hydrogen burning, main sequence life. The main sequence phase is the longest phase of a star's life, about 10 billion years for a star w ...
... Finally, the rate of fusion becomes high enough to establish gravitational equilibrium. At this point, fusion becomes self-sustaining and the star settles into its hydrogen burning, main sequence life. The main sequence phase is the longest phase of a star's life, about 10 billion years for a star w ...
Slide 1
... • But may determine the age of a stellar cluster, formed at the same time and composition, from the evolution of stars in the cluster with different masses isochrones • High mass stars evolve off the MS (“turn off”) before low mass stars ...
... • But may determine the age of a stellar cluster, formed at the same time and composition, from the evolution of stars in the cluster with different masses isochrones • High mass stars evolve off the MS (“turn off”) before low mass stars ...
Star Properties and Stellar Evolution
... different distances be compared? Use their brightness if they were all an equal distance from Earth = 32 ly. Absolute Magnitude ...
... different distances be compared? Use their brightness if they were all an equal distance from Earth = 32 ly. Absolute Magnitude ...
22 October: The Formation of Stars
... • When we see massive main sequence stars (spectral class O), we know they are young. • With fairly simple observations, we can find groups of O and B stars (OB associations) ...
... • When we see massive main sequence stars (spectral class O), we know they are young. • With fairly simple observations, we can find groups of O and B stars (OB associations) ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.