Star Formation - University of Redlands
... Cold clouds can be tens of parsecs across. Thousands of times the mass of the Sun. Temperatures 10 – 100 K. In such a cloud: – Something makes a region denser than normal. – Force of gravity draws material to denser region. – Gravitational collapse begins. ...
... Cold clouds can be tens of parsecs across. Thousands of times the mass of the Sun. Temperatures 10 – 100 K. In such a cloud: – Something makes a region denser than normal. – Force of gravity draws material to denser region. – Gravitational collapse begins. ...
Lecture 11: The Internal Structure of Stars
... Tip the internal balance either way, and it will change the star’s outward appearance (most obviously, it will expand or contract) Internal Changes have External Consequences, which is helpful for figuring out what is going on inside of stars. ...
... Tip the internal balance either way, and it will change the star’s outward appearance (most obviously, it will expand or contract) Internal Changes have External Consequences, which is helpful for figuring out what is going on inside of stars. ...
EMR, Telescopes, Stars, Solar System study guide `14-15
... 9. The distance that light travels in a year is known as a _________________________. 10. The time it takes light from a star 100 light years away to reach Earth is ___________________. 11. Parallax is used to find the ____________________________ to nearby stars. 12. Astronomers use a _____________ ...
... 9. The distance that light travels in a year is known as a _________________________. 10. The time it takes light from a star 100 light years away to reach Earth is ___________________. 11. Parallax is used to find the ____________________________ to nearby stars. 12. Astronomers use a _____________ ...
Which property of a star would not change if we could observe it
... • It works the same with stars! • If we know the total energy output of a star (luminosity), and we can count the number of photons we receive from that star (brightness), we can calculate its distance ...
... • It works the same with stars! • If we know the total energy output of a star (luminosity), and we can count the number of photons we receive from that star (brightness), we can calculate its distance ...
Black Hole
... It is the tiniest star, having collapsed into a superdense state. It is thought to have formed when a large star exploded as a supernova. ...
... It is the tiniest star, having collapsed into a superdense state. It is thought to have formed when a large star exploded as a supernova. ...
The solar system rotates around the sun due to the sun`s
... T he light spectra emitted from supernovas show the light of the heavy elements. ...
... T he light spectra emitted from supernovas show the light of the heavy elements. ...
Chapter 19 Star Formation
... Stars go through a number of stages in the process of forming from an interstellar cloud: [You don’t have to memorize these numbers, but they do tell an important story, and you should understand the names of the objects on the right.] ...
... Stars go through a number of stages in the process of forming from an interstellar cloud: [You don’t have to memorize these numbers, but they do tell an important story, and you should understand the names of the objects on the right.] ...
Nuclear Probabilities - FacStaff Home Page for CBU
... In Beta- decay, a neutron emits an electron and antineutrino and becomes a proton. We can see this occur if we consider the neutron to consist of 2 down quarks and 1 up quark. The extra energy in the unstable isotope undergoing the decay is converted into a neutrino / anti-neutrino pair. One of the ...
... In Beta- decay, a neutron emits an electron and antineutrino and becomes a proton. We can see this occur if we consider the neutron to consist of 2 down quarks and 1 up quark. The extra energy in the unstable isotope undergoing the decay is converted into a neutrino / anti-neutrino pair. One of the ...
Beavercreek City Schools
... Lighter elements are more likely to undergo fusion because they have smaller nuclei that can fuse with another nuclei and remain stable. 2. What type of elements are more likely to undergo fission? Why? Heavier elements are more likely to undergo fission because they have larger unstable nuclei that ...
... Lighter elements are more likely to undergo fusion because they have smaller nuclei that can fuse with another nuclei and remain stable. 2. What type of elements are more likely to undergo fission? Why? Heavier elements are more likely to undergo fission because they have larger unstable nuclei that ...
UCSD Students` Presentation on Star Formation
... * How does star formation begin? When part of an interstellar medium collapses under it’s own weight *As the # of atoms increases in an accidental cluster, the gravitational attraction increases, and the clump becomes strong enough for the atoms not to disperse. The effect of heat is not stronger t ...
... * How does star formation begin? When part of an interstellar medium collapses under it’s own weight *As the # of atoms increases in an accidental cluster, the gravitational attraction increases, and the clump becomes strong enough for the atoms not to disperse. The effect of heat is not stronger t ...
powerpoint - Physics @ IUPUI
... up with a combination of gas pressure and radiation pressure (light has energy) • This was called “Hydrostatic Equilibrium” ...
... up with a combination of gas pressure and radiation pressure (light has energy) • This was called “Hydrostatic Equilibrium” ...
Student 1
... thought to be 10 billion years old and older than our galaxy. It must have been captured from elsewhere. Bernard’s star is travelling towards us at a very high speed. It will become closer to us than Proxima Centauri. Barnard’s star emits most of its radiation as infrared light and emits almost no u ...
... thought to be 10 billion years old and older than our galaxy. It must have been captured from elsewhere. Bernard’s star is travelling towards us at a very high speed. It will become closer to us than Proxima Centauri. Barnard’s star emits most of its radiation as infrared light and emits almost no u ...
THE MASS OF A STELLAR BLACK HOLE Andrea Massi
... Doppler discovered that sound waves from a moving source are compressed or expanded, i.e. their frequency changes. For example the Doppler effect causes a siren to sound higher when it is approaching us and lower when it is receding. ...
... Doppler discovered that sound waves from a moving source are compressed or expanded, i.e. their frequency changes. For example the Doppler effect causes a siren to sound higher when it is approaching us and lower when it is receding. ...
Astron 104 Laboratory #7 Nuclear Fusion and Stars
... which might already be familiar from high school chemistry. Use a periodic table to determine the element, mass, and charge for nuclei in the table below. For example, 8 protons and 8 neutrons is an oxygen nucleus with a mass of 16 units and a charge of ...
... which might already be familiar from high school chemistry. Use a periodic table to determine the element, mass, and charge for nuclei in the table below. For example, 8 protons and 8 neutrons is an oxygen nucleus with a mass of 16 units and a charge of ...
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.