Chapter 25 Study guide Answer Key
... What color is the most massive type of main sequence star? The least massive? Blue = Most massive Red = Least ...
... What color is the most massive type of main sequence star? The least massive? Blue = Most massive Red = Least ...
Review3-2016
... Asteroid, meteorites and comets. What is the asteroid belt, how we believe it was formed and where it is located? What are the size distribution of the asteroids. Compare the size of the largest asteroid with the planet Pluto. What is the composition of a meteorite. What is the structure of a comet? ...
... Asteroid, meteorites and comets. What is the asteroid belt, how we believe it was formed and where it is located? What are the size distribution of the asteroids. Compare the size of the largest asteroid with the planet Pluto. What is the composition of a meteorite. What is the structure of a comet? ...
Structure of the Sun, our nearest star
... The luminosity of a star is powered by nuclear ____________ taking place in the center (core) of the star o The temperature and density are sufficient to allow nuclear fusion to occur. o Stars are primarily composed of hydrogen, with small amounts of helium. o They are so hot that the ______________ ...
... The luminosity of a star is powered by nuclear ____________ taking place in the center (core) of the star o The temperature and density are sufficient to allow nuclear fusion to occur. o Stars are primarily composed of hydrogen, with small amounts of helium. o They are so hot that the ______________ ...
How do stars form?
... Will a star form? • If mass is sufficient, gravity at the center of the sphere may be great enough to “squash” atoms together. • 4 H atoms are fused to form 1 He atom in a nuclear reaction (not chemical). • Nuclear reaction is nuclear fusion, which ...
... Will a star form? • If mass is sufficient, gravity at the center of the sphere may be great enough to “squash” atoms together. • 4 H atoms are fused to form 1 He atom in a nuclear reaction (not chemical). • Nuclear reaction is nuclear fusion, which ...
Review 1
... 11. Each element, e.g. H, He, C,..., has its own unique set of spectral lines. 12. Kirchhoff’s Laws: : 1. A hot opaque body produces continuous spectrum. : 2. A hot transparent gas produces an emission line spectrum. : 3. A cooler, transparent gas in front of a source of continuous spectrum produces ...
... 11. Each element, e.g. H, He, C,..., has its own unique set of spectral lines. 12. Kirchhoff’s Laws: : 1. A hot opaque body produces continuous spectrum. : 2. A hot transparent gas produces an emission line spectrum. : 3. A cooler, transparent gas in front of a source of continuous spectrum produces ...
Unit D Test Review Electromagnetic Spectrum: Which
... Stars: What is a main sequence star made of? (what elements) What holds a star together? What are the 3 Characteristics of stars? How does a star’s temperature relate to its luminosity? Using an HR diagram: ● identify the super giant, giant, main sequence and white dwarf stars ● relate colo ...
... Stars: What is a main sequence star made of? (what elements) What holds a star together? What are the 3 Characteristics of stars? How does a star’s temperature relate to its luminosity? Using an HR diagram: ● identify the super giant, giant, main sequence and white dwarf stars ● relate colo ...
Physical Science 1 Quiz 10 1 ID # or name:
... Please circle the letter or write the letter next to or under the question number. This quiz is due by 7:30 pm, Wed., May 28th. Please submit your quiz to me via email to one of the ...
... Please circle the letter or write the letter next to or under the question number. This quiz is due by 7:30 pm, Wed., May 28th. Please submit your quiz to me via email to one of the ...
STARS
... Make up about 90% of all studied stars Most stars spend a majority of their life as a main sequence star As main sequence stars temperature increases, their ...
... Make up about 90% of all studied stars Most stars spend a majority of their life as a main sequence star As main sequence stars temperature increases, their ...
Ch 28 Fact Sheet
... _________________ 16. Type of spectrum that glowing neon gas produces in a spectroscope. _________________ 17. Type of spectrum produced by the atmosphere of a planet. _________________ 18. Type of pitch (high or low) produced as a car approaches you. _________________ 19. Shift question 28 is an ex ...
... _________________ 16. Type of spectrum that glowing neon gas produces in a spectroscope. _________________ 17. Type of spectrum produced by the atmosphere of a planet. _________________ 18. Type of pitch (high or low) produced as a car approaches you. _________________ 19. Shift question 28 is an ex ...
Solving the Mystery of Massive Star Birth
... As the cloud gets smaller, it gets clumpy. The clumps may eventually become so compact that they begin to heat up, growing hotter and hotter, until eventually they begin “burning” at their core. When the temperature at the core reaches a scorching 10 million degrees, the clump officially becomes a new ...
... As the cloud gets smaller, it gets clumpy. The clumps may eventually become so compact that they begin to heat up, growing hotter and hotter, until eventually they begin “burning” at their core. When the temperature at the core reaches a scorching 10 million degrees, the clump officially becomes a new ...
AST 443
... 8. Calculate the average density of a red-giant core of 0.25 solar-mass and radius 15,000 km. Compare this with the average density of the giant’s envelope, if it has a 0.5 solar-mass and its radius is 0.5 A.U. Compare each with the central density of the Sun. ...
... 8. Calculate the average density of a red-giant core of 0.25 solar-mass and radius 15,000 km. Compare this with the average density of the giant’s envelope, if it has a 0.5 solar-mass and its radius is 0.5 A.U. Compare each with the central density of the Sun. ...
Name: Period : ______ The Universe – Life and Death of a Star How
... 23. When a Sun-like star begins to eject its outer layers of gas in “cosmic burps” it will send shells of gas illuminated by the hot central star and that will cause the __________________ nebula phenomenon. 24. When a star cools, it can become a bizarre stellar remnant known as a __________________ ...
... 23. When a Sun-like star begins to eject its outer layers of gas in “cosmic burps” it will send shells of gas illuminated by the hot central star and that will cause the __________________ nebula phenomenon. 24. When a star cools, it can become a bizarre stellar remnant known as a __________________ ...
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.