Undergraduate Project in Physics Alon Grubshtein Guided by Prof. Eduardo Guendelman
... (Tritium is an unstable, ultra heavy hydrogen, consisting of one proton and two neutrons). It so happens, that there are no stable nuclei of masses 5 and 8, and as a result nuclear reactions rapidly diminish after making helium. Small amounts of other light elements are made, but it is not possible ...
... (Tritium is an unstable, ultra heavy hydrogen, consisting of one proton and two neutrons). It so happens, that there are no stable nuclei of masses 5 and 8, and as a result nuclear reactions rapidly diminish after making helium. Small amounts of other light elements are made, but it is not possible ...
UvA-DARE (Digital Academic Repository)
... withh B12 the magnetic field strength in units of 10 12 Gauss and P in units of 1 0 - 1 5 s/s. Ass pulsars grow older, their rotation slows down and their fields may decrease in strength. Eventuallyy the polar cap voltage falls below a certain value, the pulsar switches off: it 'dies'. A nn often us ...
... withh B12 the magnetic field strength in units of 10 12 Gauss and P in units of 1 0 - 1 5 s/s. Ass pulsars grow older, their rotation slows down and their fields may decrease in strength. Eventuallyy the polar cap voltage falls below a certain value, the pulsar switches off: it 'dies'. A nn often us ...
–1– Solutions to PH6820 Midterm 1. Define the following: molecular
... clouds. Typical kinetic temperatures range from 10-50 K. The average densities are around 50-100 cm−3 . They often show filamentary and clumpy morphologies. A molecular core is a self gravitating globule within a molecular cloud. The typical sizes (0.1 pc), masses (a few M⊙ ), temperatures (10 K) an ...
... clouds. Typical kinetic temperatures range from 10-50 K. The average densities are around 50-100 cm−3 . They often show filamentary and clumpy morphologies. A molecular core is a self gravitating globule within a molecular cloud. The typical sizes (0.1 pc), masses (a few M⊙ ), temperatures (10 K) an ...
Neutrino hot dark matter and hydrodynamics of structure formation
... • Lynden Bell: violent relaxation, faster than collisional • Relaxation in time-dependent potential: every object (individual particle, galaxy) exchanges energy with the whole cluster • Iff phase space density becomes uniform, then Fermi-Dirac distribution • X-ray radiation helps to maintain the vir ...
... • Lynden Bell: violent relaxation, faster than collisional • Relaxation in time-dependent potential: every object (individual particle, galaxy) exchanges energy with the whole cluster • Iff phase space density becomes uniform, then Fermi-Dirac distribution • X-ray radiation helps to maintain the vir ...
Sun, Moon, Earth,
... (not even light) can escape them. • We can find them because…. – Stars that are close to them are “pulled” by the gravity of the black hole. – Gases in the area are pulled in so fast (like a drain in a sink) that they spin around the black hole and we see the heat given off. ...
... (not even light) can escape them. • We can find them because…. – Stars that are close to them are “pulled” by the gravity of the black hole. – Gases in the area are pulled in so fast (like a drain in a sink) that they spin around the black hole and we see the heat given off. ...
Stellar Stability and the Chandrasekhar Limit
... oxygen.[3] This core has no further source of energy, and so will gradually radiate away its energy and cool down to extremely low temperatures. The core, no longer supported against gravitational collapse by fusion reactions, becomes extremely dense, with a typical mass of that of the sun contained ...
... oxygen.[3] This core has no further source of energy, and so will gradually radiate away its energy and cool down to extremely low temperatures. The core, no longer supported against gravitational collapse by fusion reactions, becomes extremely dense, with a typical mass of that of the sun contained ...
AST1100 Lecture Notes
... approximation in the absence of rotation, turbulence and magnetic fields. In reality however, all these factors do contribute and far more complicated considerations are needed in order to calculate the exact criterion. The collapsing cloud will initially be in free fall, a period when the photons g ...
... approximation in the absence of rotation, turbulence and magnetic fields. In reality however, all these factors do contribute and far more complicated considerations are needed in order to calculate the exact criterion. The collapsing cloud will initially be in free fall, a period when the photons g ...
Chapter 11 White Dwarfs and Neutron Stars
... 11.2.3 Ingredients of a White Dwarf Description An initial description of a white dwarf may be afforded by a theory for which 1. The stable configurations correspond to hydrostatic equilibrium ...
... 11.2.3 Ingredients of a White Dwarf Description An initial description of a white dwarf may be afforded by a theory for which 1. The stable configurations correspond to hydrostatic equilibrium ...
ASTRONOMY 301 EXAMPLES OF TEST
... (A) We would see completely different kinds of objects when we look at the night sky. (B) We would see only the most energetic objects – for example, supernovae – in the night sky. (C) We would see more or less the same objects that we see now, but hotter objects would be easier to see and colder ob ...
... (A) We would see completely different kinds of objects when we look at the night sky. (B) We would see only the most energetic objects – for example, supernovae – in the night sky. (C) We would see more or less the same objects that we see now, but hotter objects would be easier to see and colder ob ...
SGR and AXP – are they magnetars?
... scenario of the off-center explosion Numerical investigation is needed ...
... scenario of the off-center explosion Numerical investigation is needed ...
nuclear
... persistent X-ray emission (arising from accretion) constrains the burst energetics - the -value • Compactness of the neutron star means that accretion liberates roughly 50% of the rest-mass energy of the accreted material • Nuclear burning is much less efficient, at around 1%; expected ratio is the ...
... persistent X-ray emission (arising from accretion) constrains the burst energetics - the -value • Compactness of the neutron star means that accretion liberates roughly 50% of the rest-mass energy of the accreted material • Nuclear burning is much less efficient, at around 1%; expected ratio is the ...
If neutron star is born with a strong magnetic field
... along what is known as the spin-up line and approaches a few milliseconds. ...
... along what is known as the spin-up line and approaches a few milliseconds. ...
Computer Modeling the Line of Sight Column Densities of Polars
... Polars are a type of CV that has a strong magnetic field around 100 million times earths magnetic field. The plasma is not allowed to form an accretion disc because it follows the magnetic field lines. The stream takes a more direct path toward the white dwarf. The high speeds of the impacting parti ...
... Polars are a type of CV that has a strong magnetic field around 100 million times earths magnetic field. The plasma is not allowed to form an accretion disc because it follows the magnetic field lines. The stream takes a more direct path toward the white dwarf. The high speeds of the impacting parti ...
Chapter 21 Jeopardy
... The Hertzsprung-Russell Diagram for 1600 Stars found in the upper right-hand corner of the HR diagram are known as the ____________________ ...
... The Hertzsprung-Russell Diagram for 1600 Stars found in the upper right-hand corner of the HR diagram are known as the ____________________ ...
JeopardyCh21StarsGalaxiesUniverse
... The Hertzsprung-Russell Diagram for 1600 Stars found in the upper right-hand corner of the HR diagram are known as the ____________________ ...
... The Hertzsprung-Russell Diagram for 1600 Stars found in the upper right-hand corner of the HR diagram are known as the ____________________ ...
absolute brightness: The apparent brightness a star would have if it
... proton or an electron. The electric field determines the electric force exerted by the particle on all other charged particles in the universe; the strength of the electric field decreases with increasing distance from the charge according to an inverse-square law. electromagnetic radiation: Consist ...
... proton or an electron. The electric field determines the electric force exerted by the particle on all other charged particles in the universe; the strength of the electric field decreases with increasing distance from the charge according to an inverse-square law. electromagnetic radiation: Consist ...
Constraining decaying dark matter with neutron stars
... If this was indeed the scenario, a possibly catastrophic NS to quark star transition could occur when the macroscopic deconfinement proceeds via detonation modes to rapidly consume the star [36]. The GRB signal emitted has been estimated in [14] and subsequent emission in cosmic ray channels is also ...
... If this was indeed the scenario, a possibly catastrophic NS to quark star transition could occur when the macroscopic deconfinement proceeds via detonation modes to rapidly consume the star [36]. The GRB signal emitted has been estimated in [14] and subsequent emission in cosmic ray channels is also ...
absolute brightness: The apparent brightness a star would have if it
... proton or an electron. The electric field determines the electric force exerted by the particle on all other charged particles in the universe; the strength of the electric field decreases with increasing distance from the charge according to an inverse-square law. electromagnetic radiation: Consist ...
... proton or an electron. The electric field determines the electric force exerted by the particle on all other charged particles in the universe; the strength of the electric field decreases with increasing distance from the charge according to an inverse-square law. electromagnetic radiation: Consist ...
Document
... lifetime = E available = 1. 3 x 1051 ergs ~ 3 x 1017s ~ 10 billion yrs E loss rate 4 x 1033 ergs/s ...
... lifetime = E available = 1. 3 x 1051 ergs ~ 3 x 1017s ~ 10 billion yrs E loss rate 4 x 1033 ergs/s ...
ECLIPSE, Volume 1, Number 3, March - April 2017
... Why are black holes so hard to find? Black holes are often created when a lot of matter is compressed into a small space, which can happen when stars are dying and collapse in on themselves. This means the gravitational pull is so strong, light cannot escape. When no light can get out, that means th ...
... Why are black holes so hard to find? Black holes are often created when a lot of matter is compressed into a small space, which can happen when stars are dying and collapse in on themselves. This means the gravitational pull is so strong, light cannot escape. When no light can get out, that means th ...
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.