The Death of Massive Stars
... Review – the fates of stars What happens after all the H is used up in the core? • Very Low-mass stars (0.4 Msun or less): Star cease fusing material in the core after all the Hydrogen is used up • Low-mass stars: Hydrogen shell burning, eventually leads to Helium flash in core, planetary nebula ph ...
... Review – the fates of stars What happens after all the H is used up in the core? • Very Low-mass stars (0.4 Msun or less): Star cease fusing material in the core after all the Hydrogen is used up • Low-mass stars: Hydrogen shell burning, eventually leads to Helium flash in core, planetary nebula ph ...
Stellar Evolution
... • A core with remaining mass of 1.4 to 3 M, composed of tightly packed neutrons. • These tiny stars are much smaller than planet Earth -- in fact, they are about the diameter of a large city (~20 km). • One cubic centimeter (like a sugar cube) of a neutron star, would have a mass of about 1011 kg! ...
... • A core with remaining mass of 1.4 to 3 M, composed of tightly packed neutrons. • These tiny stars are much smaller than planet Earth -- in fact, they are about the diameter of a large city (~20 km). • One cubic centimeter (like a sugar cube) of a neutron star, would have a mass of about 1011 kg! ...
30 The Nucleus - mrphysicsportal.net
... Beta particles were later identified as high speed electrons. Six millimeters of aluminum are needed to stop most 13 particles. Several centimeters of lead are required to stop 'Y rays, which proved to be high energy photons. Alpha particles and 'Y rays are emitted with a specific energy that depend ...
... Beta particles were later identified as high speed electrons. Six millimeters of aluminum are needed to stop most 13 particles. Several centimeters of lead are required to stop 'Y rays, which proved to be high energy photons. Alpha particles and 'Y rays are emitted with a specific energy that depend ...
A not so massive cluster hosting a very massive star
... We present the first physical characterization of the young open cluster VVV CL041. We spectroscopically observed the cluster main-sequence stellar population and a very-massive star candidate: WR62-2. CMFGEN modelling to our near-infrared spectra indicates that WR62-2 is a very luminous (106.4±0.2 ...
... We present the first physical characterization of the young open cluster VVV CL041. We spectroscopically observed the cluster main-sequence stellar population and a very-massive star candidate: WR62-2. CMFGEN modelling to our near-infrared spectra indicates that WR62-2 is a very luminous (106.4±0.2 ...
How is the Potential Energy Released
... behaviors, but much of the interesting physics/astrophysics is common to all • Understanding of accretion disks, accretion flows, X-ray induced winds, compact object evolution are all in an active state of ...
... behaviors, but much of the interesting physics/astrophysics is common to all • Understanding of accretion disks, accretion flows, X-ray induced winds, compact object evolution are all in an active state of ...
Chapter 13 Neutron Stars and Black Holes
... Bursts of X rays have been observed near the center of our Galaxy. A typical one appears at right, as imaged in the X-ray spectrum. ...
... Bursts of X rays have been observed near the center of our Galaxy. A typical one appears at right, as imaged in the X-ray spectrum. ...
Untitled
... BANG ! Scientists aren’t entirely sure what causes a star to explode. But they do know about two types of supernovas. One type of supernova requires two stars that ...
... BANG ! Scientists aren’t entirely sure what causes a star to explode. But they do know about two types of supernovas. One type of supernova requires two stars that ...
Physics I - Rose
... first find the radius of the circle using 2πr = l. EXECUTE: Solving for r gives r = l/2π = (8.50 cm)/2π = 1.353 cm The charge on this circle is Q = l = (175 nC/m)(0.0850 m) = 14.88 nC The electric field is E ...
... first find the radius of the circle using 2πr = l. EXECUTE: Solving for r gives r = l/2π = (8.50 cm)/2π = 1.353 cm The charge on this circle is Q = l = (175 nC/m)(0.0850 m) = 14.88 nC The electric field is E ...
arXiv:hep-ph/9910471 25 Oct 1999
... matter (109 erg cm−3 or ∼ 0.1 eV per molecular bond). At a mass above 1.5 ng, for a typical nuclear density, the object becomes larger than an atom and the positron cloud that it has been developing sits mainly inside the strangelet itself (for stable strangelets that have grown this large, the sign ...
... matter (109 erg cm−3 or ∼ 0.1 eV per molecular bond). At a mass above 1.5 ng, for a typical nuclear density, the object becomes larger than an atom and the positron cloud that it has been developing sits mainly inside the strangelet itself (for stable strangelets that have grown this large, the sign ...
Core-collapse supernovae and their massive progenitors
... the SMC stars, typically 175 ± 100 km s–1 (Mokiem et al. 2006). Rotational velocities have not been significantly affected by stellar winds, and are significantly lower than 300 km s–1 presently adopted in evolutionary models of Meynet and Maeder (2000). Although the majority of high-mass stars unde ...
... the SMC stars, typically 175 ± 100 km s–1 (Mokiem et al. 2006). Rotational velocities have not been significantly affected by stellar winds, and are significantly lower than 300 km s–1 presently adopted in evolutionary models of Meynet and Maeder (2000). Although the majority of high-mass stars unde ...
University of Groningen Weak Interactions in Neutron Stars van
... The standard coolirig scenario of lFri79] is based upon a nonrelativistic quasiparticle approxiniation and the use of the one-pion exchange potential. For a low neutrino energy (1 MeV) the two-body neutrino emission processes are directly related to the nucleon-nucleon scattering according to the Lo ...
... The standard coolirig scenario of lFri79] is based upon a nonrelativistic quasiparticle approxiniation and the use of the one-pion exchange potential. For a low neutrino energy (1 MeV) the two-body neutrino emission processes are directly related to the nucleon-nucleon scattering according to the Lo ...
Modern physics topics 1 Physical data Constants: G = 6.67 x 10
... Emergency exit signs are sometimes powered by the decay of radioactive tritium, which has a half-life of 12.3 years and emits an electron with a kinetic energy of 0.0186 MeV. Light is emitted when the electron is captured by the surrounding plastic in the sign. Suppose that you want to construct a r ...
... Emergency exit signs are sometimes powered by the decay of radioactive tritium, which has a half-life of 12.3 years and emits an electron with a kinetic energy of 0.0186 MeV. Light is emitted when the electron is captured by the surrounding plastic in the sign. Suppose that you want to construct a r ...
Asteroseismology with the Whole Earth Telescope
... Luminosity = 0.05±0.12 Mo Magnetic field = 1300±300 G????? Differential Rotation – envelop rotating faster than core????? • Fontaine & Brassard • Temperature 22,900 K • Mass=0.625 Mo (C) 0.660 Mo (C/O)) • Log (Helium envelope mass) = -6.1 • Models depend on input physics – including convection param ...
... Luminosity = 0.05±0.12 Mo Magnetic field = 1300±300 G????? Differential Rotation – envelop rotating faster than core????? • Fontaine & Brassard • Temperature 22,900 K • Mass=0.625 Mo (C) 0.660 Mo (C/O)) • Log (Helium envelope mass) = -6.1 • Models depend on input physics – including convection param ...
stars - acpsd
... The ejection of stellar remnants is the low-mass star�supernova. On Earth, we measure the effects of this supernova in the increased luminosity. After a low-mass star�death (supernova), it often leaves behind material that forms new stellar bodies. This is the end of stars with low masses (less than ...
... The ejection of stellar remnants is the low-mass star�supernova. On Earth, we measure the effects of this supernova in the increased luminosity. After a low-mass star�death (supernova), it often leaves behind material that forms new stellar bodies. This is the end of stars with low masses (less than ...
Nuclear Powerhouse
... They rarely interact with ordinary matter Neutrinos travel extremely fast at almost the speed of light if their mass is tiny ...
... They rarely interact with ordinary matter Neutrinos travel extremely fast at almost the speed of light if their mass is tiny ...
Modeling High-Mass X-ray Binary Formation in the Chandra Era Tim Linden
... At each step in stellar evolution, calculate if there are important binary interactions, these generally happen on a faster timescale than stellar evolution ...
... At each step in stellar evolution, calculate if there are important binary interactions, these generally happen on a faster timescale than stellar evolution ...
Stellar Evolu1on Stars spend most of their lives on the main
... degenerate C+O core, a helium fusing shell, and a hydrogen fusing shell, all within a volume just larger than that of the Earth. This is surrounded by a hydrogen-‐rich envelope ...
... degenerate C+O core, a helium fusing shell, and a hydrogen fusing shell, all within a volume just larger than that of the Earth. This is surrounded by a hydrogen-‐rich envelope ...
revealing star formation processes in the nearby universe
... • UV & FIR light are subject to assumptions about extinction and reprocessing of light • Radio recombination lines provide a direct measure of the ionized gas ...
... • UV & FIR light are subject to assumptions about extinction and reprocessing of light • Radio recombination lines provide a direct measure of the ionized gas ...
Life Cycle of Stars
... combine to form heavier elements. (For example, Hydrogen fuses to form Helium.) This process releases energy. When hydrogen beings to run low, the star becomes a red giant. The outer shell of the star expands (up to 100 times the size of the original star) and cools. A supernova is a tremendous expl ...
... combine to form heavier elements. (For example, Hydrogen fuses to form Helium.) This process releases energy. When hydrogen beings to run low, the star becomes a red giant. The outer shell of the star expands (up to 100 times the size of the original star) and cools. A supernova is a tremendous expl ...
Phantom Tracks
... particles interact strongly with matter, in fact, just a few centimeters of air are enough to absorb them. Beta particles were later identified as high-speed electrons. Moving faster and having less charge allows beta particles a greater penetrating ability. Figure 30–3 illustrates the difference in ...
... particles interact strongly with matter, in fact, just a few centimeters of air are enough to absorb them. Beta particles were later identified as high-speed electrons. Moving faster and having less charge allows beta particles a greater penetrating ability. Figure 30–3 illustrates the difference in ...
Chapter 30: The Nucleus
... particles interact strongly with matter, in fact, just a few centimeters of air are enough to absorb them. Beta particles were later identified as high-speed electrons. Moving faster and having less charge allows beta particles a greater penetrating ability. Figure 30–3 illustrates the difference in ...
... particles interact strongly with matter, in fact, just a few centimeters of air are enough to absorb them. Beta particles were later identified as high-speed electrons. Moving faster and having less charge allows beta particles a greater penetrating ability. Figure 30–3 illustrates the difference in ...
PowerPoint Presentation - The Sun as a Power House
... Fusion would be simpler if four protons would collide simultaneously to make one helium nucleus Simpler, but less likely rare for four objects to collide simultaneously with high enough energy chance of this happening are very, very small rate too slow to power the Sun proton-proton chain: each step ...
... Fusion would be simpler if four protons would collide simultaneously to make one helium nucleus Simpler, but less likely rare for four objects to collide simultaneously with high enough energy chance of this happening are very, very small rate too slow to power the Sun proton-proton chain: each step ...
Lectures 14 & 15 powerpoint (neutron stars & black holes)
... 4.3 and 3.9 Earth masses! Further analysis revealed a third planet with a mass of about that of our moon! And there is evidence that a fourth planet about 100 Earth masses orbits this pulsar with a much larger separation. Q: How can a NS have planets?!? (Recall that NS are created by supernovae, and ...
... 4.3 and 3.9 Earth masses! Further analysis revealed a third planet with a mass of about that of our moon! And there is evidence that a fourth planet about 100 Earth masses orbits this pulsar with a much larger separation. Q: How can a NS have planets?!? (Recall that NS are created by supernovae, and ...
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.