Chapter16
... emission line — A narrow, bright region of the spectrum. Emission lines are produced when electrons in atoms jump from one energy level to a lower energy level. energy level — Any of the many energy states that an atom may have. Different energy levels correspond to different distances of the electr ...
... emission line — A narrow, bright region of the spectrum. Emission lines are produced when electrons in atoms jump from one energy level to a lower energy level. energy level — Any of the many energy states that an atom may have. Different energy levels correspond to different distances of the electr ...
Supernova - Mid-Pacific Institute
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
Activity: Star Classification - d
... Part 1: Exploring with Classification Each group will receive 1 set of 27 stars. Every star has: a color, name, temperature, size, & luminosity value o The luminosity is compared to the sun's luminosity. If a star has a luminosity value of 5, then it is 5 times brighter than our sun. If a star h ...
... Part 1: Exploring with Classification Each group will receive 1 set of 27 stars. Every star has: a color, name, temperature, size, & luminosity value o The luminosity is compared to the sun's luminosity. If a star has a luminosity value of 5, then it is 5 times brighter than our sun. If a star h ...
G-stars - Gemini Astronomie
... The birth of a star: Every star develops from a cloud (giant molecular cloud GMC) consisting almost entirely of the elements hydrogen and helium with a small percentage of other elements as well as dust, mostly from the death of older stars. Due to the force of its own gravity, the cloud begins to c ...
... The birth of a star: Every star develops from a cloud (giant molecular cloud GMC) consisting almost entirely of the elements hydrogen and helium with a small percentage of other elements as well as dust, mostly from the death of older stars. Due to the force of its own gravity, the cloud begins to c ...
Sample Stellar Evolution TEST QUESTIONS
... 11. The Orion region contains young main sequence stars and an emission nebula. 12. The thermal motions of the atoms in a gas cloud can make it collapse to form a protostar. 13. The pressure of a gas generally depends on its temperature and its density. 14. Stars swell into giants when hydrogen is e ...
... 11. The Orion region contains young main sequence stars and an emission nebula. 12. The thermal motions of the atoms in a gas cloud can make it collapse to form a protostar. 13. The pressure of a gas generally depends on its temperature and its density. 14. Stars swell into giants when hydrogen is e ...
Astronomy Webquest _2 STARS
... time, the star will change into a ___________________________ and grow to more than 400 times its original size. As they expand, red giants engulf some of their close-orbiting planets. In the Sun's case, this will mean the fiery end of all the inner planets of our Solar System, which might also incl ...
... time, the star will change into a ___________________________ and grow to more than 400 times its original size. As they expand, red giants engulf some of their close-orbiting planets. In the Sun's case, this will mean the fiery end of all the inner planets of our Solar System, which might also incl ...
Ordinary Stars - Edgewood High School
... As the temperature of a star increases, the peak of its radiation is shifted toward shorter (blue) wavelengths Stefan-Boltzmann Law As the temperature of a star increases, the total energy output increases as the 4th power of the temperature ...
... As the temperature of a star increases, the peak of its radiation is shifted toward shorter (blue) wavelengths Stefan-Boltzmann Law As the temperature of a star increases, the total energy output increases as the 4th power of the temperature ...
0802 - thephysicsteacher.ie
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean 'water-forming'. Hydrogen atoms were made in the Big Bang, when the universe is be ...
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean 'water-forming'. Hydrogen atoms were made in the Big Bang, when the universe is be ...
Summary: The Structure and Evolution of Stars
... • Region A represents the main sequence in the cluster. All stars in this region are in the core hydrogen-burning phase, the longest evolutionary phase of a star. Stars at lower luminosity along the main sequence have lower masses (where roughly M ∝ L4 ). • Turning Point X: stars near the turning p ...
... • Region A represents the main sequence in the cluster. All stars in this region are in the core hydrogen-burning phase, the longest evolutionary phase of a star. Stars at lower luminosity along the main sequence have lower masses (where roughly M ∝ L4 ). • Turning Point X: stars near the turning p ...
12.1 Introduction
... limit, pressure support from the core can no longer hold the overlying stellar envelope. As a result, the core collapses on a Kelvin-Helmholtz timescale and the star evolves very rapidly relative to the nuclear timescale of main sequence evolution. This occurs at the points labelled 4 in Figure 12.1 ...
... limit, pressure support from the core can no longer hold the overlying stellar envelope. As a result, the core collapses on a Kelvin-Helmholtz timescale and the star evolves very rapidly relative to the nuclear timescale of main sequence evolution. This occurs at the points labelled 4 in Figure 12.1 ...
An Assessment: Think Pair Share
... How does the size of a star near the top left of the H-R diagram compare with a star of the same luminosity near the top right of the H-R diagram? ...
... How does the size of a star near the top left of the H-R diagram compare with a star of the same luminosity near the top right of the H-R diagram? ...
Introduction to the Earth
... White dwarfs- smaller than 1/10 the size of the sun Neutron stars - smallest stars - about 16 ...
... White dwarfs- smaller than 1/10 the size of the sun Neutron stars - smallest stars - about 16 ...
the Study Guide
... Supernovas: A super-brilliant burst of light caused by a collapsing star. When some stars die they reach a point where the energy they generate is not enough to counter act the force of their own gravity. They collapse in an instant, becoming supernovas. These are very rare. Only a few supernovas ha ...
... Supernovas: A super-brilliant burst of light caused by a collapsing star. When some stars die they reach a point where the energy they generate is not enough to counter act the force of their own gravity. They collapse in an instant, becoming supernovas. These are very rare. Only a few supernovas ha ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... 2. Consider a binary system consisting of a main sequence star and a white dwarf companion. Which star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cor ...
... 2. Consider a binary system consisting of a main sequence star and a white dwarf companion. Which star is older? Which star started its life with more mass? Given that we’ve talked about how far apart stars are in the galaxy, they almost never run into each other. (It’s a different matter in the cor ...
Measuring the Stars pages 813-820
... Lines of absorption show what elements are in a star, because of dark patches on the rainbow. ...
... Lines of absorption show what elements are in a star, because of dark patches on the rainbow. ...
Closed books and notes, 1 hour. Please PRINT
... (b) Experiments suggest that the Sun’s core must be cooler than previously thought, which reduces the rate of nuclear fusion and the number of neutrinos produced (c) Experiments suggest that electron neutrinos produced in the core can change into other types before reaching Earth, reducing the obser ...
... (b) Experiments suggest that the Sun’s core must be cooler than previously thought, which reduces the rate of nuclear fusion and the number of neutrinos produced (c) Experiments suggest that electron neutrinos produced in the core can change into other types before reaching Earth, reducing the obser ...
Montage of Jupiter and the Galilean satellites
... Indian astronomers. The color indicates what is happening to the electrons in different parts of the Crab Nebula. Red indicates the electrons are recombining with protons to form neutral hydrogen, while blue indicates the electrons are whirling around the magnetic field of the inner nebula. In the n ...
... Indian astronomers. The color indicates what is happening to the electrons in different parts of the Crab Nebula. Red indicates the electrons are recombining with protons to form neutral hydrogen, while blue indicates the electrons are whirling around the magnetic field of the inner nebula. In the n ...
Earth
... •Random non-uniformities in the expanding universe are not sufficient to allow the formation of galaxies. • In the presence of the rapid expansion, the gravitational attraction is too low for galaxies to form with any reasonable model of turbulence created by the expansion itself. •"..the question o ...
... •Random non-uniformities in the expanding universe are not sufficient to allow the formation of galaxies. • In the presence of the rapid expansion, the gravitational attraction is too low for galaxies to form with any reasonable model of turbulence created by the expansion itself. •"..the question o ...
blue_giant
... A blue giant is a massive star that has exhausted the hydrogen fuel in its core and left the main sequence. Blue giants have a surface temperature of around 30,000 K Typically, giant stars have radii between 10 and 100 solar radii and luminosities between 10 and 1,000 times that of the sun. ...
... A blue giant is a massive star that has exhausted the hydrogen fuel in its core and left the main sequence. Blue giants have a surface temperature of around 30,000 K Typically, giant stars have radii between 10 and 100 solar radii and luminosities between 10 and 1,000 times that of the sun. ...
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.