answers2004_05_BC - Particle Physics and Particle Astrophysics
... its days in the spectacular fashion adopted by Sanduleak −69 202. What will the Sun eventually evolve into? Sun is not massive enough to fuse elements heavier than helium (core never gets that hot), therefore it will not form an iron core (it is also not a close binary, so it will not produce a Ty ...
... its days in the spectacular fashion adopted by Sanduleak −69 202. What will the Sun eventually evolve into? Sun is not massive enough to fuse elements heavier than helium (core never gets that hot), therefore it will not form an iron core (it is also not a close binary, so it will not produce a Ty ...
H-R Diagram
... stop, the star will collapse. Gravity always wins. What's left at the end depends on how massive the star was to begin with. ...
... stop, the star will collapse. Gravity always wins. What's left at the end depends on how massive the star was to begin with. ...
stars - Chatt
... • These are stars thirty times bigger than our Sun. • Small, very dense object with an extremely strong gravitational pull. • Nothing can escape from it; not even light. ...
... • These are stars thirty times bigger than our Sun. • Small, very dense object with an extremely strong gravitational pull. • Nothing can escape from it; not even light. ...
File - Mr. Catt`s Class
... The Chandrasekhar Limit 1. Even though electron degeneracy supports the white dwarf against collapsing completely, there is a limit to the amount of pressure degenerate electrons can withstand. 2. This limit to the mass of a white dwarf above which it cannot be supported by electron degeneracy and ...
... The Chandrasekhar Limit 1. Even though electron degeneracy supports the white dwarf against collapsing completely, there is a limit to the amount of pressure degenerate electrons can withstand. 2. This limit to the mass of a white dwarf above which it cannot be supported by electron degeneracy and ...
CHAPTER 14
... 1. If accretion brings the mass of a white dwarf above the Chandrasekhar limit, electron degeneracy can no longer support the star, and it collapses. The collapse raises the core temperature and runaway carbon fusion begins, which ultimately leads to the star exploding completely. 2. Such an explod ...
... 1. If accretion brings the mass of a white dwarf above the Chandrasekhar limit, electron degeneracy can no longer support the star, and it collapses. The collapse raises the core temperature and runaway carbon fusion begins, which ultimately leads to the star exploding completely. 2. Such an explod ...
Astronomy
... A contracting cloud is called a protostar. Pressure and temperature increase. When the contracting gas and dust becomes so hot that nuclear fusion begins, a star is born!! ...
... A contracting cloud is called a protostar. Pressure and temperature increase. When the contracting gas and dust becomes so hot that nuclear fusion begins, a star is born!! ...
MASS – LUMINOSITY RELATION FOR MASSIVE STARS
... Near the stellar surface we have Mr ≈ M and Lr ≈ L, and adopting κ ≈ κe = const, we may integrate equation (s2.3) to obtain ...
... Near the stellar surface we have Mr ≈ M and Lr ≈ L, and adopting κ ≈ κe = const, we may integrate equation (s2.3) to obtain ...
April 10th
... • Carbon and silicon atoms form grains, which are pushed outward by radiation • Red Giant loses material (as much as 10-4 solar masses per year) ...
... • Carbon and silicon atoms form grains, which are pushed outward by radiation • Red Giant loses material (as much as 10-4 solar masses per year) ...
Red Giant Red Giant White Giant Red Giant White Giant White Giant
... Centauri, the closest star to the Sun, is a red giant. Mass: 1- 4 Solar Mass StarPower Points: 7 ...
... Centauri, the closest star to the Sun, is a red giant. Mass: 1- 4 Solar Mass StarPower Points: 7 ...
Astronomy The Night Sky. Vocabulary Terms to know for the
... 3. All stars begin as _______________________ when space dust has formed a sphere that becomes very hot, leading to ___________________: when _____________________ is turned into _________________ in its core. 4. The ________________________________________ (stars that are stable and have a lot of h ...
... 3. All stars begin as _______________________ when space dust has formed a sphere that becomes very hot, leading to ___________________: when _____________________ is turned into _________________ in its core. 4. The ________________________________________ (stars that are stable and have a lot of h ...
Stars
... • Begin their lives as giant clouds of dust and gas called nebulae • Gravity may cause the nebula to ...
... • Begin their lives as giant clouds of dust and gas called nebulae • Gravity may cause the nebula to ...
Stars and Moon Summative Review
... Identify the phases of the moon. How does the gravitational pull of the moon affect the Earth? (the side closest and the side farthest) What does a waxing moon indicate? Identify the cause of tides on Earth. Describe the effect that the elliptical orbit of the moon has on the Earth. ...
... Identify the phases of the moon. How does the gravitational pull of the moon affect the Earth? (the side closest and the side farthest) What does a waxing moon indicate? Identify the cause of tides on Earth. Describe the effect that the elliptical orbit of the moon has on the Earth. ...
Stars
... Three types of galaxies--all have billions of stars. Spiral Galaxy Our Milky Way is one. Has bulge at center and spiral arms. Our Sun is close to the edge of galaxy. ...
... Three types of galaxies--all have billions of stars. Spiral Galaxy Our Milky Way is one. Has bulge at center and spiral arms. Our Sun is close to the edge of galaxy. ...
Star formation jeopardy
... The stars are in old age (Red Giants) and there are hundreds of thousands to millions of stars in a cluster. ...
... The stars are in old age (Red Giants) and there are hundreds of thousands to millions of stars in a cluster. ...
The coolest White Dwarf— older than the age of the universe?
... steadily loses its outer gasses and ends its life as a ball of compact degenerate electron gas or a White Dwarf (WD). It may begin this stage with a very high temperature, say 50,000 K and it steadily cools over time following a well-known cooling rate. Eventually this object will cool so much that ...
... steadily loses its outer gasses and ends its life as a ball of compact degenerate electron gas or a White Dwarf (WD). It may begin this stage with a very high temperature, say 50,000 K and it steadily cools over time following a well-known cooling rate. Eventually this object will cool so much that ...
Mars Project
... a nebula. (A big cloud of gas and dust spread out in space.) in the dense part of the nebula the gas and dust becomes so dense and hot that a star is born. ...
... a nebula. (A big cloud of gas and dust spread out in space.) in the dense part of the nebula the gas and dust becomes so dense and hot that a star is born. ...
Reading Preview
... A star’s ________ gives clues about the star’s temperature. The coolest stars appear ________. The hottest stars appear ________. Very large stars are called ________ stars or ____________ stars. Our sun is a medium sized ________. Most stars are ________ than the sun. White dwarf stars are abou ...
... A star’s ________ gives clues about the star’s temperature. The coolest stars appear ________. The hottest stars appear ________. Very large stars are called ________ stars or ____________ stars. Our sun is a medium sized ________. Most stars are ________ than the sun. White dwarf stars are abou ...
Stellar Evolution and the HR Diagram – Study Guide
... O Star: nebula blue star Super red giant Super nova Black Hole A Star: nebula whitestar Super red giant Super nova Neutron Star G Star: nebula yellow star Red giant Planetary Nebula White Dwarf ...
... O Star: nebula blue star Super red giant Super nova Black Hole A Star: nebula whitestar Super red giant Super nova Neutron Star G Star: nebula yellow star Red giant Planetary Nebula White Dwarf ...
Name_______________________Period_________Date
... 1. Describe the life cycle of a medium size star. (Our sun) 10 % of a stars inner most mass react in nuclear fusion When H in core is gone, some left in outer layers Outer layers expand and cool; star becomes a Red Giant Red giants have low surface gravity, outer layers are driven away Cor ...
... 1. Describe the life cycle of a medium size star. (Our sun) 10 % of a stars inner most mass react in nuclear fusion When H in core is gone, some left in outer layers Outer layers expand and cool; star becomes a Red Giant Red giants have low surface gravity, outer layers are driven away Cor ...
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.