Astronomy 10B List of Concepts– by Chapter
... o Stellar mass-loss on way to becoming a White Dwarf • Supernovas (ae) o Implosion/Explosion Iron core & end of fusion - What’s special about Iron o Energy given off, fraction as light, neutrinos, other o Nucleosynthesis: how elements heavier than Iron are made • Neutron Stars o Neutron degeneracy ...
... o Stellar mass-loss on way to becoming a White Dwarf • Supernovas (ae) o Implosion/Explosion Iron core & end of fusion - What’s special about Iron o Energy given off, fraction as light, neutrinos, other o Nucleosynthesis: how elements heavier than Iron are made • Neutron Stars o Neutron degeneracy ...
Astro 2 - Red Hook Central School District
... body – spherical in shape held by its own gravity ...
... body – spherical in shape held by its own gravity ...
solution - Evergreen Archives
... 13. What produces the rapid rotation rate of a young neutron star, or pulsar? The core of the dying star spins up because it collapses to a very small radius. Matter falling onto the neutron star from the debris of the supernova explosion causes the neutron star to spin up. Mass transfer from a com ...
... 13. What produces the rapid rotation rate of a young neutron star, or pulsar? The core of the dying star spins up because it collapses to a very small radius. Matter falling onto the neutron star from the debris of the supernova explosion causes the neutron star to spin up. Mass transfer from a com ...
Problem set 2
... and luminosity from the textbook, and between mass and radius (you can assume it’s linear, R ∼ M), compute Proxima’s effective temperature Tef f . Comparing with sun’s temperature, prove that the star appears much redder than the sun. Compute the effective temperatures of the other two stars (1.1 an ...
... and luminosity from the textbook, and between mass and radius (you can assume it’s linear, R ∼ M), compute Proxima’s effective temperature Tef f . Comparing with sun’s temperature, prove that the star appears much redder than the sun. Compute the effective temperatures of the other two stars (1.1 an ...
MT 2 Answers Version A
... Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and chec ...
... Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and chec ...
MT 2 Answers Version C
... O- and B-type stars have converted much more of their hydrogen into heavier elements. ...
... O- and B-type stars have converted much more of their hydrogen into heavier elements. ...
MT 2 Answers Version D
... dropped from the same height and allowed to fall to the ground. How do their accelerations compare? (a) ...
... dropped from the same height and allowed to fall to the ground. How do their accelerations compare? (a) ...
The Future Sun
... • Giants are dying stars; white dwarfs are dead stars • Why does the sun die? • What will the sun become when it dies? ...
... • Giants are dying stars; white dwarfs are dead stars • Why does the sun die? • What will the sun become when it dies? ...
SOLUTION SET
... 15. __________ are relatively compact dead cores of stars like our sun. A. White dwarfs B. Neutron stars C. Black holes D. Supernovae E. Planetary nebulae ...
... 15. __________ are relatively compact dead cores of stars like our sun. A. White dwarfs B. Neutron stars C. Black holes D. Supernovae E. Planetary nebulae ...
Earth Space Systems Semester 1 Exam Astronomy Vocabulary Astronomical Unit-
... fast spinning star called a Neutron star. The Neutron star can further develop into a Pulsar which is a pulsating spinning star. After a Supernova, some super massive stars collapse so much that they form an invisible Black Hole. A Black Hole’s gravitational inward pull is so great that its light an ...
... fast spinning star called a Neutron star. The Neutron star can further develop into a Pulsar which is a pulsating spinning star. After a Supernova, some super massive stars collapse so much that they form an invisible Black Hole. A Black Hole’s gravitational inward pull is so great that its light an ...
Evolution Cycle of Stars
... Sun their overall luminosity's are 1% of the Sun or less. • White dwarfs are the shrunken remains of normal stars, whose nuclear energy supplies have been used up. White dwarf consist of degenerate matter with a very high density due to gravitational effects, i.e. one spoonful has a mass of several ...
... Sun their overall luminosity's are 1% of the Sun or less. • White dwarfs are the shrunken remains of normal stars, whose nuclear energy supplies have been used up. White dwarf consist of degenerate matter with a very high density due to gravitational effects, i.e. one spoonful has a mass of several ...
Space Study Guide
... pressures within the core of stars, atoms collide at high enough speeds to overcome the usual electromagnetic repulsion of nuclei, allowing nuclear fusion to occur. All stars live by fusing hydrogen into helium. In the first step of the process, two hydrogen atoms fuse to form deuterium. In the next ...
... pressures within the core of stars, atoms collide at high enough speeds to overcome the usual electromagnetic repulsion of nuclei, allowing nuclear fusion to occur. All stars live by fusing hydrogen into helium. In the first step of the process, two hydrogen atoms fuse to form deuterium. In the next ...
The correct answers are written in bold, italic and underlined. The
... 12. Which physical process generates the force inside a pre-main-sequence star to stop the star from slowly condensing and shrinking by offsetting the force of gravity, thereby resulting in a stable main-sequence star? • No physical process can prevent this condensation until a black hole is produce ...
... 12. Which physical process generates the force inside a pre-main-sequence star to stop the star from slowly condensing and shrinking by offsetting the force of gravity, thereby resulting in a stable main-sequence star? • No physical process can prevent this condensation until a black hole is produce ...
PPT file
... Similar to our sun (stays like this for most of their life) These burn H fuel faster than low mass stars and last only about 10 billion years ...
... Similar to our sun (stays like this for most of their life) These burn H fuel faster than low mass stars and last only about 10 billion years ...
Type II supernova
A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star. A star must have at least 8 times, and no more than 40–50 times, the mass of the Sun (M☉) for this type of explosion. It is distinguished from other types of supernovae by the presence of hydrogen in its spectrum. Type II supernovae are mainly observed in the spiral arms of galaxies and in H II regions, but not in elliptical galaxies.Stars generate energy by the nuclear fusion of elements. Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans. The degeneracy pressure of electrons and the energy generated by these fusion reactions are sufficient to counter the force of gravity and prevent the star from collapsing, maintaining stellar equilibrium. The star fuses increasingly higher mass elements, starting with hydrogen and then helium, progressing up through the periodic table until a core of iron and nickel is produced. Fusion of iron or nickel produces no net energy output, so no further fusion can take place, leaving the nickel-iron core inert. Due to the lack of energy output allowing outward pressure, equilibrium is broken.When the mass of the inert core exceeds the Chandrasekhar limit of about 1.4 M☉, electron degeneracy alone is no longer sufficient to counter gravity and maintain stellar equilibrium. A cataclysmic implosion takes place within seconds, in which the outer core reaches an inward velocity of up to 23% of the speed of light and the inner core reaches temperatures of up to 100 billion kelvin. Neutrons and neutrinos are formed via reversed beta-decay, releasing about 1046 joules (100 foes) in a ten-second burst. The collapse is halted by neutron degeneracy, causing the implosion to rebound and bounce outward. The energy of this expanding shock wave is sufficient to accelerate the surrounding stellar material to escape velocity, forming a supernova explosion, while the shock wave and extremely high temperature and pressure briefly allow for theproduction of elements heavier than iron. Depending on initial size of the star, the remnants of the core form a neutron star or a black hole. Because of the underlying mechanism, the resulting nova is also described as a core-collapse supernova.There exist several categories of Type II supernova explosions, which are categorized based on the resulting light curve—a graph of luminosity versus time—following the explosion. Type II-L supernovae show a steady (linear) decline of the light curve following the explosion, whereas Type II-P display a period of slower decline (a plateau) in their light curve followed by a normal decay. Type Ib and Ic supernovae are a type of core-collapse supernova for a massive star that has shed its outer envelope of hydrogen and (for Type Ic) helium. As a result, they appear to be lacking in these elements.