here
... As we compress the highly ionised gas further, there comes a point where the electrons in the gas are squeezed together so closely that they start to behave like in condensed matter. The Pauli exclusion principle disallows them to occupy the same quantum state, and therefore, each electron must occu ...
... As we compress the highly ionised gas further, there comes a point where the electrons in the gas are squeezed together so closely that they start to behave like in condensed matter. The Pauli exclusion principle disallows them to occupy the same quantum state, and therefore, each electron must occu ...
Comparing Earth, Sun and Jupiter
... a. If pulsars were binary stars, what would be the size of the semimajor axis? a3 P M ...
... a. If pulsars were binary stars, what would be the size of the semimajor axis? a3 P M ...
Coursework 7 File
... Permittivity of free space 0 = 8.85 × 10−12 F m−1 Proton charge e = 1.6 × 10−19 C. Exercise class question - not to be handed in 1. The atoms in a gas of temperature T have kinetic energies Eke = 32 kT on average. Assuming that this is the typical energy associated with collisions between hydrogen ...
... Permittivity of free space 0 = 8.85 × 10−12 F m−1 Proton charge e = 1.6 × 10−19 C. Exercise class question - not to be handed in 1. The atoms in a gas of temperature T have kinetic energies Eke = 32 kT on average. Assuming that this is the typical energy associated with collisions between hydrogen ...
Stars
... Apparent magnitude: brightness as seen from Earth Absolute magnitude: brightness if it were a standard distance from Earth ...
... Apparent magnitude: brightness as seen from Earth Absolute magnitude: brightness if it were a standard distance from Earth ...
Star Life Cycles
... all of its nuclear fuel and has collapsed to a very small size; such a star is near its final stage of life. White dwarfs eventually become black dwarfs, which is a white dwarf that has cooled down enough that it no longer emits light. Interesting Fact: The universe is not old enough to have a ...
... all of its nuclear fuel and has collapsed to a very small size; such a star is near its final stage of life. White dwarfs eventually become black dwarfs, which is a white dwarf that has cooled down enough that it no longer emits light. Interesting Fact: The universe is not old enough to have a ...
Stars and Galaxies - Earth Science: Astronomy
... b. Core contracts and heats up causing outer layers to expand and cool c. Star becomes a giant as it expands and outer layers cool d. Helium nuclei fuse to form core of carbon ...
... b. Core contracts and heats up causing outer layers to expand and cool c. Star becomes a giant as it expands and outer layers cool d. Helium nuclei fuse to form core of carbon ...
Astronomy Learning Objectives and Study Questions for Chapter 12
... (given an appropriate graph) and combine this with its apparent magnitude and the distance-magnitude equation to determine how far it is from Earth. 7. Briefly describe the conditions necessary for mass transfer to occur in a binary star system. 1. Prototstars become pre-main-sequence stars when the ...
... (given an appropriate graph) and combine this with its apparent magnitude and the distance-magnitude equation to determine how far it is from Earth. 7. Briefly describe the conditions necessary for mass transfer to occur in a binary star system. 1. Prototstars become pre-main-sequence stars when the ...
chapter 18
... An incredibly dense star so massive that light cannot escape from its surface is called a _______________. a) red giant b) black hole c) white dwarf d) pulsar ...
... An incredibly dense star so massive that light cannot escape from its surface is called a _______________. a) red giant b) black hole c) white dwarf d) pulsar ...
STARS
... • Most stars are between 1 billion and 10 billion years old. Some stars may even be close to 13.7 billion years old—the observed age of the universe. The oldest star yet discovered, HE 1523-0901, is an estimated 13.2 billion years old. • The more massive the star, the shorter its lifespan, primarily ...
... • Most stars are between 1 billion and 10 billion years old. Some stars may even be close to 13.7 billion years old—the observed age of the universe. The oldest star yet discovered, HE 1523-0901, is an estimated 13.2 billion years old. • The more massive the star, the shorter its lifespan, primarily ...
HOMEWORK 5 SOLUTIONS CHAPTER 9 4.A A red giant star will
... the Earth’s orbit will not change. Since the Sun is so far away, it appears to the Earth to be a point source. The black hole will also appear to be a point source so the orbit will not change. CHAPTER 11 1.C The halo is home to old, metal-poor stars. Globular clusters contain some of the oldest sta ...
... the Earth’s orbit will not change. Since the Sun is so far away, it appears to the Earth to be a point source. The black hole will also appear to be a point source so the orbit will not change. CHAPTER 11 1.C The halo is home to old, metal-poor stars. Globular clusters contain some of the oldest sta ...
Ch 28 Vocab cnp
... The brightness of a star The measure of how bright a star would be if it were located 10 parsecs from Earth A group of millions, or even billions of stars held together by gravity A unit of measurement used to describe distances between celestial objects, equal to 3.258 light-years A large cloud of ...
... The brightness of a star The measure of how bright a star would be if it were located 10 parsecs from Earth A group of millions, or even billions of stars held together by gravity A unit of measurement used to describe distances between celestial objects, equal to 3.258 light-years A large cloud of ...
Study Guide_galaxies, Tools, and Stars Test
... 6. Name and describe the 3 types of galaxies. 7. Where is our solar system located in the Milky Way galaxy? 8. What is a light year? 9. What contains all the matter and energy that exists? 10. Name two types of optical telescopes. 11. What do radio telescopes receive and where do they come from? 12. ...
... 6. Name and describe the 3 types of galaxies. 7. Where is our solar system located in the Milky Way galaxy? 8. What is a light year? 9. What contains all the matter and energy that exists? 10. Name two types of optical telescopes. 11. What do radio telescopes receive and where do they come from? 12. ...
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.