THE INNER CORE OF A NEUTRON STAR Part 1
... Abstract: Neutron stars are formed by super compaction that result from the gravitational collapse of a massive star after a supernova. Neutron star composition makes it so heavy that its density is at least twice the mass of Earth’s Sun. Current thinking subscribes to the possibility that a neutron ...
... Abstract: Neutron stars are formed by super compaction that result from the gravitational collapse of a massive star after a supernova. Neutron star composition makes it so heavy that its density is at least twice the mass of Earth’s Sun. Current thinking subscribes to the possibility that a neutron ...
reach for the stars
... Section Id: Answer the following questions about open and globular clusters. (10 pts total) 1. Stars in clusters are bound together by what? (1 pt) Gravity 2. Which type of cluster is often found in the halo of galaxies? (1 pt) Globular clusters 3. Where is the other type of cluster usually found? ...
... Section Id: Answer the following questions about open and globular clusters. (10 pts total) 1. Stars in clusters are bound together by what? (1 pt) Gravity 2. Which type of cluster is often found in the halo of galaxies? (1 pt) Globular clusters 3. Where is the other type of cluster usually found? ...
Multi-physics simulations using a hierarchical interchangeable
... is used for the integration of the equations of motion of the stars, the second module is used for the gravitational coupling between the gas-particles and the stars. The combined solver consists of an integrator for the coupled gas/gravitational dynamics systems and a feedback prescription for mech ...
... is used for the integration of the equations of motion of the stars, the second module is used for the gravitational coupling between the gas-particles and the stars. The combined solver consists of an integrator for the coupled gas/gravitational dynamics systems and a feedback prescription for mech ...
Variation of Elements in Nature
... He/3He. When the helium-4 nuclei interact with interstellar hydrogen, part of it is converted into helium-3 (and also helium-2). The ratio of 3He/4He thus will increase with the amount of matter travelled. From the measurement of this ratio it has been estimated that cosmic ray nuclei have travelled ...
... He/3He. When the helium-4 nuclei interact with interstellar hydrogen, part of it is converted into helium-3 (and also helium-2). The ratio of 3He/4He thus will increase with the amount of matter travelled. From the measurement of this ratio it has been estimated that cosmic ray nuclei have travelled ...
14.1 Introduction - University of Cambridge
... ure 13.11) following the ejection of the star’s outer layers in the planetary nebula stage. In either case, without an internal source of energy, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy. ...
... ure 13.11) following the ejection of the star’s outer layers in the planetary nebula stage. In either case, without an internal source of energy, white dwarfs simply cool off at an essentially constant radius as they slowly deplete their supply of thermal energy. ...
14 The Interstellar Medium and Star Formation
... 106 K, and nuclear fusion begins. The protostar has become a star, but it is not in equilibrium. The star continues to contract and increase in temperature until it is in equilibrium. This is stage 7: The star has reached the main sequence and will remain there as long as it has hydrogen to ...
... 106 K, and nuclear fusion begins. The protostar has become a star, but it is not in equilibrium. The star continues to contract and increase in temperature until it is in equilibrium. This is stage 7: The star has reached the main sequence and will remain there as long as it has hydrogen to ...
ASTR 300 Stars and Stellar Systems Spring 2011
... of a neutron star? What happens to the rest of the mass of the original star? The maximum mass of a neutron star is thought to be between 2 and 3 solar masses – surely below 3 M⊙ . A 13 M⊙ star explodes as a core-collapse supernova in forming the neutron star, so 13 - 3 = 10 M⊙ of material are expel ...
... of a neutron star? What happens to the rest of the mass of the original star? The maximum mass of a neutron star is thought to be between 2 and 3 solar masses – surely below 3 M⊙ . A 13 M⊙ star explodes as a core-collapse supernova in forming the neutron star, so 13 - 3 = 10 M⊙ of material are expel ...
Exploring Stars - Discovery Education
... 1. Talk about the life of a star. A good way to introduce this topic is to show Exploring Stars. After watching the program, talk about the different types of stars found in the universe. What are stars? What are they made of? How is a red star different from a blue star? Discuss and review the life ...
... 1. Talk about the life of a star. A good way to introduce this topic is to show Exploring Stars. After watching the program, talk about the different types of stars found in the universe. What are stars? What are they made of? How is a red star different from a blue star? Discuss and review the life ...
Skinner Chapter 3
... d. the process whereby elements heavier than carbon are created. 12. Which one of the following statements is false? a. Our Sun is in its hydrogen burning stage of evolution. b. The main sequence lifetime of our Sun will last at least 4 billion more years. c. After our Sun has exhausted its nuclear ...
... d. the process whereby elements heavier than carbon are created. 12. Which one of the following statements is false? a. Our Sun is in its hydrogen burning stage of evolution. b. The main sequence lifetime of our Sun will last at least 4 billion more years. c. After our Sun has exhausted its nuclear ...
Be Stars
... Stars are formed by a process in which gas clouds, condense and collapse in on them selves because of gravity. Building up pressure causes a rise in temperature in the developing star. Nuclear fusion begins if the core´s temperature gets to about 14 000 000 degrees Kelvin. ...
... Stars are formed by a process in which gas clouds, condense and collapse in on them selves because of gravity. Building up pressure causes a rise in temperature in the developing star. Nuclear fusion begins if the core´s temperature gets to about 14 000 000 degrees Kelvin. ...
nebula - Harding University
... Sometimes a white dwarf may be one of a binary star system. As material (hydrogen) from its companion leaks onto the surface of the white dwarf, the pressure and temperature build up until the outer hydrogen shell ignites and causes an explosion – producing one class of nova. This type of nova m ...
... Sometimes a white dwarf may be one of a binary star system. As material (hydrogen) from its companion leaks onto the surface of the white dwarf, the pressure and temperature build up until the outer hydrogen shell ignites and causes an explosion – producing one class of nova. This type of nova m ...
What is a Hertzsprung
... • As it expands, the ionized helium cools, and becomes less ionized and therefore more transparent, allowing the radiation to escape cooling the star and slowing the fusion rate. • Then the expansion stops, and reverses due to the star's gravitational attraction. • The process then repeats. ...
... • As it expands, the ionized helium cools, and becomes less ionized and therefore more transparent, allowing the radiation to escape cooling the star and slowing the fusion rate. • Then the expansion stops, and reverses due to the star's gravitational attraction. • The process then repeats. ...
lecture11
... Two otherwise identical stars are rotating at different rates. Star A is rotating slower than Star B. How do Star A’s spectral lines appear with respect to Star B’s lines? Star A’s lines are narrower than Star B’s lines. Star B’s lines are narrower than Star A’s lines. There is no difference in th ...
... Two otherwise identical stars are rotating at different rates. Star A is rotating slower than Star B. How do Star A’s spectral lines appear with respect to Star B’s lines? Star A’s lines are narrower than Star B’s lines. Star B’s lines are narrower than Star A’s lines. There is no difference in th ...
18._Sun_student
... a) 4 hydrogen nuclei form 1 helium nucleus plus energy. b) 2 hydrogen nuclei form 1 helium nucleus plus energy. c) 6 hydrogen nuclei form 1 helium nucleus, 1 carbon nucleus plus energy. d) 3 hydrogen nuclei form 1 helium nucleus plus energy. e) 4 hydrogen nuclei form 1 helium nucleus, 1 carbon nucle ...
... a) 4 hydrogen nuclei form 1 helium nucleus plus energy. b) 2 hydrogen nuclei form 1 helium nucleus plus energy. c) 6 hydrogen nuclei form 1 helium nucleus, 1 carbon nucleus plus energy. d) 3 hydrogen nuclei form 1 helium nucleus plus energy. e) 4 hydrogen nuclei form 1 helium nucleus, 1 carbon nucle ...
1 Stars
... For most of a star’s life, hydrogen atoms fuse to form helium atoms. A star like this is a main sequence star. The hotter a main sequence star is, the brighter it is. A star remains on the main sequence as long as it is fusing hydrogen to form helium. Our Sun has been a main sequence star for about ...
... For most of a star’s life, hydrogen atoms fuse to form helium atoms. A star like this is a main sequence star. The hotter a main sequence star is, the brighter it is. A star remains on the main sequence as long as it is fusing hydrogen to form helium. Our Sun has been a main sequence star for about ...
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.