Stars Study Guide KEY
... *7. Which stars live the longest, high-mass or low-mass? Low Mass Stars live longer. Why? They have less self-gravity which means they burn through their fuel slower. 8. What will happen to our star, the Sun, at the end of its life? The sun will expand in the Red Giant phase, then will release its o ...
... *7. Which stars live the longest, high-mass or low-mass? Low Mass Stars live longer. Why? They have less self-gravity which means they burn through their fuel slower. 8. What will happen to our star, the Sun, at the end of its life? The sun will expand in the Red Giant phase, then will release its o ...
The H-R Diagram
... The Herzsprung Russel Diagram (HRD) is a systematic way of arranging stellar data. It plots the Absolute Magnitude (MV) or Luminosity (L/L¤) versus the Spectral Type, Surface Temperature or Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally t ...
... The Herzsprung Russel Diagram (HRD) is a systematic way of arranging stellar data. It plots the Absolute Magnitude (MV) or Luminosity (L/L¤) versus the Spectral Type, Surface Temperature or Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally t ...
ASTR101 Unit 10 Assessment Answer Key 1. Mass, luminosity, size
... 1. Mass, luminosity, size, surface temperature, and age. Ordinary stars range in mass from about 60 solar masses to about 1/12 solar mass, in luminosity from about 1,000,000 to 1/10,000 solar luminosities, in radius from about 1,000 to 1/10 solar radii, in surface temperature from about 35,000 to 3, ...
... 1. Mass, luminosity, size, surface temperature, and age. Ordinary stars range in mass from about 60 solar masses to about 1/12 solar mass, in luminosity from about 1,000,000 to 1/10,000 solar luminosities, in radius from about 1,000 to 1/10 solar radii, in surface temperature from about 35,000 to 3, ...
That is an irrelevant question, Ms Gajda, there was no
... 16. Out of which material do stars begin to form? Hydrogen/gas and dust found in nebulae 17. What are the nuclear reactions that take place in a star’s centre? The collision and fusion of hydrogen nuclei – produce helium 18. What causes a main sequence star to become a red giant? The nuclear reactio ...
... 16. Out of which material do stars begin to form? Hydrogen/gas and dust found in nebulae 17. What are the nuclear reactions that take place in a star’s centre? The collision and fusion of hydrogen nuclei – produce helium 18. What causes a main sequence star to become a red giant? The nuclear reactio ...
Kepler`s Law - New Mexico Tech
... The Sun’s Lifecycle • The Sun was formed about 4.57 billion years ago when a hydrogen molecular cloud collapsed. • It is about halfway through its main-sequence evolution, during this time, nuclear fusion reactions in its core fuse hydrogen into helium. • It will spend approx. 10 billion years as a ...
... The Sun’s Lifecycle • The Sun was formed about 4.57 billion years ago when a hydrogen molecular cloud collapsed. • It is about halfway through its main-sequence evolution, during this time, nuclear fusion reactions in its core fuse hydrogen into helium. • It will spend approx. 10 billion years as a ...
Solar System from Web
... The Sun’s Lifecycle • The Sun was formed about 4.57 billion years ago when a hydrogen molecular cloud collapsed. • It is about halfway through its main-sequence evolution, during this time, nuclear fusion reactions in its core fuse hydrogen into helium. • It will spend approx. 10 billion years as a ...
... The Sun’s Lifecycle • The Sun was formed about 4.57 billion years ago when a hydrogen molecular cloud collapsed. • It is about halfway through its main-sequence evolution, during this time, nuclear fusion reactions in its core fuse hydrogen into helium. • It will spend approx. 10 billion years as a ...
Lecture21
... If a degenerate core (or white dwarf) exceeds the Chandrasekhar mass limit (1.4MSun) it must collapse until neutron degeneracy pressure takes over. M 1.4M Sun R 10km ...
... If a degenerate core (or white dwarf) exceeds the Chandrasekhar mass limit (1.4MSun) it must collapse until neutron degeneracy pressure takes over. M 1.4M Sun R 10km ...
The Ultraluminous X-ray Source in Holmberg IX and its Environment
... mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX X-1, located at a distance of 3.6 Mpc in a dwarf galaxy companion of M81. Miller ...
... mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX X-1, located at a distance of 3.6 Mpc in a dwarf galaxy companion of M81. Miller ...
Astronomy Campus Assessment
... scientific data that showed that light from a distant galaxy is red-shifted. How would you evaluate the data? A. It indicates that the expansion of the universe has stopped, and so it does not support the Big Bang theory. B. It indicates that the galaxy is moving away from Earth, and so it supports ...
... scientific data that showed that light from a distant galaxy is red-shifted. How would you evaluate the data? A. It indicates that the expansion of the universe has stopped, and so it does not support the Big Bang theory. B. It indicates that the galaxy is moving away from Earth, and so it supports ...
Document
... Low Luminosity Since they are white they are comparatively hot Fusion is no longer taking place, and a white dwarf is just a hot remnant that is cooling down They are usually composed of oxygen and carbon in an ...
... Low Luminosity Since they are white they are comparatively hot Fusion is no longer taking place, and a white dwarf is just a hot remnant that is cooling down They are usually composed of oxygen and carbon in an ...
Stellar Evolution – Test Review Answers
... Nearly in the middle of both the temperature and luminosity scales relative to other stars. This puts it around the middle of the main sequence. 17. Where are giant stars, supergiant stars and white dwarfs found on the H-R diagram, relative to the main sequence? Giant and supergiant stars lie above ...
... Nearly in the middle of both the temperature and luminosity scales relative to other stars. This puts it around the middle of the main sequence. 17. Where are giant stars, supergiant stars and white dwarfs found on the H-R diagram, relative to the main sequence? Giant and supergiant stars lie above ...
Brighter than the average star?
... Many popular astronomy books start by explaining how small and unimportant our Solar System is. The famous ‘Hitchhiker’s Guide to the Galaxy’ begins by describing our own star with the words “Far out in the uncharted backwaters of the unfashionable end of the Western Spiral arm of the galaxy lies a ...
... Many popular astronomy books start by explaining how small and unimportant our Solar System is. The famous ‘Hitchhiker’s Guide to the Galaxy’ begins by describing our own star with the words “Far out in the uncharted backwaters of the unfashionable end of the Western Spiral arm of the galaxy lies a ...
Sample multiple choice questions for Exam 2
... 37. The final stellar remnant of a one solar mass star is a a) white dwarf. b) neutron star. c) pulsar. d) black hole. e) main sequence star. 38. Neutron stars are thought to form from a) 1 Msun stars. b) 5 Msun stars. c) 10 Msun stars. d) 50 Msun stars. e) all stars; mass has nothing to do with it. ...
... 37. The final stellar remnant of a one solar mass star is a a) white dwarf. b) neutron star. c) pulsar. d) black hole. e) main sequence star. 38. Neutron stars are thought to form from a) 1 Msun stars. b) 5 Msun stars. c) 10 Msun stars. d) 50 Msun stars. e) all stars; mass has nothing to do with it. ...
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.