WHERE DO ELEMENTS COME FROM?
... • Prior to 10-6seconds, no matter, only energy • 10-6 seconds - quarks formed • By 1 second - all matter created – Tuniverse=1010 K – 7 protons for every 1 neutron – This results in 75% H and 25% He ...
... • Prior to 10-6seconds, no matter, only energy • 10-6 seconds - quarks formed • By 1 second - all matter created – Tuniverse=1010 K – 7 protons for every 1 neutron – This results in 75% H and 25% He ...
ISP 205: Visions of the Universe Fall 2001 Professor: ER Capriotti
... B. the Earth and sky as being roughly the same size. C. the Sun as the center of the universe. D. the creation as starting with a huge explosion. E. the stars as distant suns. 2. Most Greek astronomers believed that the Earth is immobile because they did not observe A. retrograde motion of the plane ...
... B. the Earth and sky as being roughly the same size. C. the Sun as the center of the universe. D. the creation as starting with a huge explosion. E. the stars as distant suns. 2. Most Greek astronomers believed that the Earth is immobile because they did not observe A. retrograde motion of the plane ...
Chapter 28 Stars and Their Characteristics
... Apparent Magnitude- Apparent Magnitude is a how bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as ...
... Apparent Magnitude- Apparent Magnitude is a how bright a star “appears” to be from Earth. The Apparent Magnitude of a star is affected by Absolute- Magnitude (Volume x Luminosity) and Distance from Observer. Betelgeuse, one of the brightest stars in the Universe, does not appear to be as bright as ...
escape velocity
... out….gravity wins the long-lasting battle • In less than 1 second, the entire star collapses in on itself, hits the iron core and bounces off to release an EXTREME amount of energy • As bright as an entire galaxy of 10 billion stars • Only high-massive stars go supernovae (must be at least 3x the ma ...
... out….gravity wins the long-lasting battle • In less than 1 second, the entire star collapses in on itself, hits the iron core and bounces off to release an EXTREME amount of energy • As bright as an entire galaxy of 10 billion stars • Only high-massive stars go supernovae (must be at least 3x the ma ...
2. Stellar Physics
... Define a star as an object that is: • Bound by self-gravity • Radiates energy that is primarily released by nuclear fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant ...
... Define a star as an object that is: • Bound by self-gravity • Radiates energy that is primarily released by nuclear fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant ...
PHYSICS OF THE SUN The Sun is a main
... Thus, we need 105510−26 ≈ 1029 kg of hydrogen to power the Sun over its lifetime so far. Since M⊙ ≈ 2 × 1030 kg, this is ∼ 1/20 of a solar mass. This is a plausible order of magnitude, since we know it’s just the core that undergoes nuclear fusion. ...
... Thus, we need 105510−26 ≈ 1029 kg of hydrogen to power the Sun over its lifetime so far. Since M⊙ ≈ 2 × 1030 kg, this is ∼ 1/20 of a solar mass. This is a plausible order of magnitude, since we know it’s just the core that undergoes nuclear fusion. ...
Star and Galaxies Chapter 13
... • Eventually Fe forms in the core, and Fe can’t fuse to produce energy • Core collapses violently and shock waves travel outwards • Outer portion of star explodes producing supernova • Neutron stars: if collapsed core of supernova is between 1.4 to 3 times as massive as the sun, it will shrink to ab ...
... • Eventually Fe forms in the core, and Fe can’t fuse to produce energy • Core collapses violently and shock waves travel outwards • Outer portion of star explodes producing supernova • Neutron stars: if collapsed core of supernova is between 1.4 to 3 times as massive as the sun, it will shrink to ab ...
Star and Galaxies Chapter 13 2013
... • Eventually Fe forms in the core, and Fe can’t fuse to produce energy • Core collapses violently and shock waves travel outwards • Outer portion of star explodes producing supernova • Neutron stars: if collapsed core of supernova is between 1.4 to 3 times as massive as the sun, it will shrink to ab ...
... • Eventually Fe forms in the core, and Fe can’t fuse to produce energy • Core collapses violently and shock waves travel outwards • Outer portion of star explodes producing supernova • Neutron stars: if collapsed core of supernova is between 1.4 to 3 times as massive as the sun, it will shrink to ab ...
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... The discovery of the mechanism of fasting and feasting process is the breakthrough that many were looking forward to and given important inputs for further theoretical understanding of these binaries. Says Dr Bhalerao: “This allows us to better understand how massive stars form, to study how binarie ...
... The discovery of the mechanism of fasting and feasting process is the breakthrough that many were looking forward to and given important inputs for further theoretical understanding of these binaries. Says Dr Bhalerao: “This allows us to better understand how massive stars form, to study how binarie ...
Where do Stars Form ?
... Disks of matter accreted onto the protostar (“accretion disks”) often lead to the formation of jets ...
... Disks of matter accreted onto the protostar (“accretion disks”) often lead to the formation of jets ...
NAME:______ANSWER KEY_______________________Period
... 1. What is the universe made up of? matter, energy, and space 2. What does light year measure? distance 3. Why do we use light year instead of kilometers? Kilometers would be way to big of a number 4. Change the following number 78,000,000 to scientific notation. 7.8 x 107 5. Write 1.90 x 108 in sta ...
... 1. What is the universe made up of? matter, energy, and space 2. What does light year measure? distance 3. Why do we use light year instead of kilometers? Kilometers would be way to big of a number 4. Change the following number 78,000,000 to scientific notation. 7.8 x 107 5. Write 1.90 x 108 in sta ...
Solutions 5
... In high-mass stars everything takes place more rapidly. Greater mass means greater gravity and the protostar process is accelerated. Greater mass leads to greater core pressures and temperatures, thus, a hotter more luminous star. The greater mass star consumes the available hydrogen at a much highe ...
... In high-mass stars everything takes place more rapidly. Greater mass means greater gravity and the protostar process is accelerated. Greater mass leads to greater core pressures and temperatures, thus, a hotter more luminous star. The greater mass star consumes the available hydrogen at a much highe ...
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.