The Swansong of Stars Orbiting Massive Black Holes
... heating, or gravitational wave emission. These processes are effective only when the star passes very close to the MBH. Inspiral starts when the star is scattered into a highly eccentric orbit, which brings it close to the MBH. Every orbit it dissipates some orbital energy. To dissipate all the ener ...
... heating, or gravitational wave emission. These processes are effective only when the star passes very close to the MBH. Inspiral starts when the star is scattered into a highly eccentric orbit, which brings it close to the MBH. Every orbit it dissipates some orbital energy. To dissipate all the ener ...
AP Physics 2: Algebra-Based 2016 Free
... The dots in the figure above represent two identical spheres, X and Y, that are fixed in place with their centers in the plane of the page. Both spheres are charged, and the charge on sphere Y is positive. The lines are isolines of electric potential, also in the plane of the page, with a potential ...
... The dots in the figure above represent two identical spheres, X and Y, that are fixed in place with their centers in the plane of the page. Both spheres are charged, and the charge on sphere Y is positive. The lines are isolines of electric potential, also in the plane of the page, with a potential ...
Lecture 9: Supernovae
... but ρ is so high in the collapsing core, the electrons are highly relativistic, and so occupy all energy states up to ∆E = 1.3 MeV = (mn − mp )c. Under these conditions, it is no longer energetically possible for free neutrons to undergo spontaneous decay. The reverse reaction ...
... but ρ is so high in the collapsing core, the electrons are highly relativistic, and so occupy all energy states up to ∆E = 1.3 MeV = (mn − mp )c. Under these conditions, it is no longer energetically possible for free neutrons to undergo spontaneous decay. The reverse reaction ...
The Sizes of Stars
... Identify the optical counterpart of an x-ray binary Observe the optical component of the binary Estimate the total mass of the system using Kepler’s and Newton’s laws Estimate the mass of the visible star from its ...
... Identify the optical counterpart of an x-ray binary Observe the optical component of the binary Estimate the total mass of the system using Kepler’s and Newton’s laws Estimate the mass of the visible star from its ...
Document
... What are black holes? How do we see black holes? What happens when black holes are in binaries? Supermassive Black Holes ...
... What are black holes? How do we see black holes? What happens when black holes are in binaries? Supermassive Black Holes ...
Black Holes and Neutron Stars
... What are black holes? How do we see black holes? What happens when black holes are in binaries? Supermassive Black Holes ...
... What are black holes? How do we see black holes? What happens when black holes are in binaries? Supermassive Black Holes ...
ppt document
... 2) If the final mass (after the supernova explosion) is more than 1.4 solar masses but less than about 3 solar masses, the core will stop collapsing when the atoms are so compacted that the electrons are shoved into the protons and the whole mass becomes neutrons that stick together by gravity. This ...
... 2) If the final mass (after the supernova explosion) is more than 1.4 solar masses but less than about 3 solar masses, the core will stop collapsing when the atoms are so compacted that the electrons are shoved into the protons and the whole mass becomes neutrons that stick together by gravity. This ...
The Lifecycle of the Stars
... *white dwarfs may only be the size of the earth, but it has the mass equal to half oh the sun. *it is the 6th stage in forming a star. Lifecycle of a star notes *also called a degenerate dwarf *it is a small star made up of electron-degenerate matter. http://en.wikipedia.org/wiki/White_dwarf Electro ...
... *white dwarfs may only be the size of the earth, but it has the mass equal to half oh the sun. *it is the 6th stage in forming a star. Lifecycle of a star notes *also called a degenerate dwarf *it is a small star made up of electron-degenerate matter. http://en.wikipedia.org/wiki/White_dwarf Electro ...
Low Mass
... winds, star expels all of its outer layers • Expelled material, rich in heavy elements such as carbon and silicon, forms planetary nebula. • ~60% of mass is lost in planetary nebula • The process of expelling material and forming the planetary nebula occurs over a period of thousands of years ...
... winds, star expels all of its outer layers • Expelled material, rich in heavy elements such as carbon and silicon, forms planetary nebula. • ~60% of mass is lost in planetary nebula • The process of expelling material and forming the planetary nebula occurs over a period of thousands of years ...
Balloon Model of the Life Cycle of Stars
... When there is enough, or if it is compressed by other nearby events, gravity pulls the gas together into a dense ball. Gravity increases the heat and pressure so much that hydrogen in the gas begins to fuse into helium. A star is born. (We ignore planetary formation from the same cloud.) The color, ...
... When there is enough, or if it is compressed by other nearby events, gravity pulls the gas together into a dense ball. Gravity increases the heat and pressure so much that hydrogen in the gas begins to fuse into helium. A star is born. (We ignore planetary formation from the same cloud.) The color, ...
07-01TheColsmologicalDistanceLadder
... 1. Binary system: • A sub-Chandrasekhar white dwarf • A less dense companion star 2. Gravity strips material off companion star 3. Dwarf gets more and more massive 4. Mass exceeds Chandrasekhar limit (1.4 Msun) 5. Kablooey 6. Kablooey has a certain absolute magnitude 7. Kablooey is very very bright. ...
... 1. Binary system: • A sub-Chandrasekhar white dwarf • A less dense companion star 2. Gravity strips material off companion star 3. Dwarf gets more and more massive 4. Mass exceeds Chandrasekhar limit (1.4 Msun) 5. Kablooey 6. Kablooey has a certain absolute magnitude 7. Kablooey is very very bright. ...
TAP 534- 3: Annihilation and pair production: bubble chamber pictures
... enters a bubble chamber. The photons leave no track, so that the particles appear to come from nowhere. How many of these events can you identify? ...
... enters a bubble chamber. The photons leave no track, so that the particles appear to come from nowhere. How many of these events can you identify? ...
Conceptual Physics
... These stars manufactured most of the carbon atoms in our bodies. These stars manufactured virtually all the elements out of which we and our planet are made. These stars generate the energy that makes life on Earth possible. ...
... These stars manufactured most of the carbon atoms in our bodies. These stars manufactured virtually all the elements out of which we and our planet are made. These stars generate the energy that makes life on Earth possible. ...
Talk
... The temperature rise increases the pressure, expanding the gas just enough to cool the gas back down and stabilize the rate of fusion Thermal equilibrium is maintained ...
... The temperature rise increases the pressure, expanding the gas just enough to cool the gas back down and stabilize the rate of fusion Thermal equilibrium is maintained ...
Kern- und Teilchenphysik I Lecture 7: Nuclear fusion
... If we the star is much smaller than the Sun, has no enough mass to ignite other nuclear reactions (the Coulomb barrier is larger) it will become a white dwarf If the star is heavier enough the star stats burning 4He with the chain ...
... If we the star is much smaller than the Sun, has no enough mass to ignite other nuclear reactions (the Coulomb barrier is larger) it will become a white dwarf If the star is heavier enough the star stats burning 4He with the chain ...
Chapter 18 The Bizarre Stellar Graveyard What is a white dwarf
... • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, th ...
... • Quantum mechanics says that electrons must move faster as they are squeezed into a very small space • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, th ...
Lecture 19: Low
... • Continue with life of a lowlow-mass star (like the Sun) after exhausting H in core -- post MS • Red giant (RG I) phase, with H shell burning • Helium flash goes off in shrinking degenerate core: horizontal branch star with He core burning • Double shell burning (H and He) yields red supergiant (RG ...
... • Continue with life of a lowlow-mass star (like the Sun) after exhausting H in core -- post MS • Red giant (RG I) phase, with H shell burning • Helium flash goes off in shrinking degenerate core: horizontal branch star with He core burning • Double shell burning (H and He) yields red supergiant (RG ...
Last time we left off at hydrogen and helium, because that`s all that
... When one has used up the hydrogen in the core of a star, then if the star is massive enough it contracts, heats up, and starts to fuse helium to carbon. Note that in the early universe, we said that this didn’t happen because there is no stable element that has eight nucleons. In a star, this is sti ...
... When one has used up the hydrogen in the core of a star, then if the star is massive enough it contracts, heats up, and starts to fuse helium to carbon. Note that in the early universe, we said that this didn’t happen because there is no stable element that has eight nucleons. In a star, this is sti ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.