DOC - Cool Cosmos
... The way stars live and die makes a lot of sense if you consider what a star really is. Simply put, a star is a large amount of gas and dust that is collapsing under the force of gravity. At first, this crush of gravity makes the inside of the star hot enough to ignite a nuclear explosion. This explo ...
... The way stars live and die makes a lot of sense if you consider what a star really is. Simply put, a star is a large amount of gas and dust that is collapsing under the force of gravity. At first, this crush of gravity makes the inside of the star hot enough to ignite a nuclear explosion. This explo ...
QUIZ 1 - AY5-S13 . . . . . . . . . . . . . . . . . YOUR NAME
... T The two gases would show different emission-line spectra F Both would show continuous spectra, with the helium-gas spectrum peaking at a shorter wavelength 6. What color would a yellow banana slug appear if illuminated with white light? Yellow ...
... T The two gases would show different emission-line spectra F Both would show continuous spectra, with the helium-gas spectrum peaking at a shorter wavelength 6. What color would a yellow banana slug appear if illuminated with white light? Yellow ...
Red Giants - Uplift North Hills Prep
... concluding that the composition of the Sun is different from that of the Earth in her papers, as it contradicted the accepted wisdom at the time. However, he changed his mind four years later after deriving the same result by different means. After Payne was proven correct, Russell briefly credited ...
... concluding that the composition of the Sun is different from that of the Earth in her papers, as it contradicted the accepted wisdom at the time. However, he changed his mind four years later after deriving the same result by different means. After Payne was proven correct, Russell briefly credited ...
Stellar Formation 1) Solar Wind/Sunspots 2) Interstellar Medium 3) Protostars
... In dense molecular clouds gravity eventually wins ...
... In dense molecular clouds gravity eventually wins ...
(AU): Average distance from Earth to Sun
... • Gas & dust held together by gravity. • Birthplace of stars. ...
... • Gas & dust held together by gravity. • Birthplace of stars. ...
Name - MIT
... A) A 100 kg mass moving at 1 km/s. B) A 20 kg mass moving at 2 km/s. C) A 2 kg mass moving at 5 km/s. D) A 10 kg mass moving at 4 km/s. E) A 5 kg mass moving at 2 km/s. 7) The Homestake Gold Mine experiment was designed to detect neutrinos. What insight can be gained from such an experiment? A) The ...
... A) A 100 kg mass moving at 1 km/s. B) A 20 kg mass moving at 2 km/s. C) A 2 kg mass moving at 5 km/s. D) A 10 kg mass moving at 4 km/s. E) A 5 kg mass moving at 2 km/s. 7) The Homestake Gold Mine experiment was designed to detect neutrinos. What insight can be gained from such an experiment? A) The ...
M = 5.5 - The Millstone
... Case 1 Stars = 1 Solar Mass -> Red Giant -> White dwarf Stars such as our Sun move off the main sequence and enter the red giant branch (RGB), when the core hydrogen is exhausted. With no thermonuclear fusion in the core, the star contracts . An outer shell of hydrogen continues to burn and the radi ...
... Case 1 Stars = 1 Solar Mass -> Red Giant -> White dwarf Stars such as our Sun move off the main sequence and enter the red giant branch (RGB), when the core hydrogen is exhausted. With no thermonuclear fusion in the core, the star contracts . An outer shell of hydrogen continues to burn and the radi ...
Cosmology 20B Homework 2 solutions
... A supernova will retain a black hole if its core remains more massive than 2 to 3 solar masses. 8. What two forces are competing when a star is in “hydrostatic equilibrium”? Gravity pulling in and pressure pushing out compete when a star is in hydrostatic equilibrium. 9. (Will be graded) Hint: use t ...
... A supernova will retain a black hole if its core remains more massive than 2 to 3 solar masses. 8. What two forces are competing when a star is in “hydrostatic equilibrium”? Gravity pulling in and pressure pushing out compete when a star is in hydrostatic equilibrium. 9. (Will be graded) Hint: use t ...
KEY Unit 10‐11 Test Review: Characteristics of the Universe
... get their energy by eating other organisms and/or plants. B) Compare Predator Vs Prey. Can a Predator can ever become a prey. Why or why not? Predator is a HunteR and eats the prey. Prey is the hunted who gets eaten. A predator can become a prey. In the food web below, the salamander is a predator t ...
... get their energy by eating other organisms and/or plants. B) Compare Predator Vs Prey. Can a Predator can ever become a prey. Why or why not? Predator is a HunteR and eats the prey. Prey is the hunted who gets eaten. A predator can become a prey. In the food web below, the salamander is a predator t ...
07-01TheColsmologicalDistanceLadder
... Cepheid Variables: How to measure the distance to a galaxy using Cepheid variable stars: 1. Find the Cepheid, measure its spectrum 2. Measure a couple periods, and its apparent magnitude m 3. Look up its absolute magnitude 4. Use M = m - 5 log10(d/10) to find d ...
... Cepheid Variables: How to measure the distance to a galaxy using Cepheid variable stars: 1. Find the Cepheid, measure its spectrum 2. Measure a couple periods, and its apparent magnitude m 3. Look up its absolute magnitude 4. Use M = m - 5 log10(d/10) to find d ...
TTh HW06 key
... 2. By how much does the mass of the Sun decrease each second because of the energy it radiates (its luminosity)? (See the discussion in Box 18-1 of Freedman and Kaufmann, Universe, 7th ed.) A) 4.2 × 109 kg B) 3.9 × 1026 kg C) 2.0 × 107 kg D) 6.0 × 1011 kg ...
... 2. By how much does the mass of the Sun decrease each second because of the energy it radiates (its luminosity)? (See the discussion in Box 18-1 of Freedman and Kaufmann, Universe, 7th ed.) A) 4.2 × 109 kg B) 3.9 × 1026 kg C) 2.0 × 107 kg D) 6.0 × 1011 kg ...
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.