A model of low-mass neutron stars with a quark core
... Abstract—We consider an equation of state that leads to a first-order phase transition from the nucleon state to the quark state with a transition parameter λ > 3/2 (λ = ρQ /(ρN + P0 /c2 )) in superdense nuclear matter. Our calculations of integrated parameters for superdense stars using this equatio ...
... Abstract—We consider an equation of state that leads to a first-order phase transition from the nucleon state to the quark state with a transition parameter λ > 3/2 (λ = ρQ /(ρN + P0 /c2 )) in superdense nuclear matter. Our calculations of integrated parameters for superdense stars using this equatio ...
The Constant-Sound-Speed parameterization of the quark matter EoS
... sufficiently heavy neutron stars may really be “hybrid stars” with quark matter cores. Since little is known about the quark matter equation of state, we perform a model-independent study of the form of the mass-radius relation for hybrid stars, making only some generic assumptions about the quark m ...
... sufficiently heavy neutron stars may really be “hybrid stars” with quark matter cores. Since little is known about the quark matter equation of state, we perform a model-independent study of the form of the mass-radius relation for hybrid stars, making only some generic assumptions about the quark m ...
Energy in The Universe - Physics Department, Princeton University
... clear hangup. This hangup arises from the fact that hydrogen "bums" to form helium when it is heated and com pressed. The thermonuclear burning (actually fusion reactions between hy drogen nuclei) releases energy, which opposes any further compression. As a result any object such as a star that co ...
... clear hangup. This hangup arises from the fact that hydrogen "bums" to form helium when it is heated and com pressed. The thermonuclear burning (actually fusion reactions between hy drogen nuclei) releases energy, which opposes any further compression. As a result any object such as a star that co ...
GoldCreation
... Most main sequence stars are in the business of making helium from hydrogen. Other elements can be created through fusion (Chaisson & McMillan, 2002). However, this only works for elements as heavy as iron or less. That’s because creation of elements heavier than iron requires additional energy rath ...
... Most main sequence stars are in the business of making helium from hydrogen. Other elements can be created through fusion (Chaisson & McMillan, 2002). However, this only works for elements as heavy as iron or less. That’s because creation of elements heavier than iron requires additional energy rath ...
Type II supernovae (Inma Dominguez)
... After an initial phase, different for the different types of SNe, the LC is powered by the photons produced by the radioactive decay ...
... After an initial phase, different for the different types of SNe, the LC is powered by the photons produced by the radioactive decay ...
LAGUNA
... LENA: Diffuse SN Background optical measurements will determine the SNR with high accuracy with this input, the spectral slope of the DSN can be used to distinguish between different SN explosion scenarios ...
... LENA: Diffuse SN Background optical measurements will determine the SNR with high accuracy with this input, the spectral slope of the DSN can be used to distinguish between different SN explosion scenarios ...
Document
... Abundance in number of an atomic species Z is the ratio between the number of atoms of this species and that of another species, X, chosen as a reference nZ=N(Z)/N(X) In the study of stellar photospheres one refers generally to Hydrogen, as this is the most abundant element. The quantity nZ=N(Z)/N(H ...
... Abundance in number of an atomic species Z is the ratio between the number of atoms of this species and that of another species, X, chosen as a reference nZ=N(Z)/N(X) In the study of stellar photospheres one refers generally to Hydrogen, as this is the most abundant element. The quantity nZ=N(Z)/N(H ...
Neutron stars: compact objects with relativistic
... deep gravitational well of neutron stars. Fixing the model of relativistic gravity in this way, the equation of state determines the mass-radius relation of neutron stars [48, 49] as well as the moment of inertia [50]. Measuring the mass and radius of neutron stars by astrophysical methods can thus ...
... deep gravitational well of neutron stars. Fixing the model of relativistic gravity in this way, the equation of state determines the mass-radius relation of neutron stars [48, 49] as well as the moment of inertia [50]. Measuring the mass and radius of neutron stars by astrophysical methods can thus ...
Unit-2-PW-Summary-Notes
... 100 atoms thick, suggested that the atom must be mostly empty space! In order to produce the large deflections at C and D, the positively charged alpha particles must be encountering something of very large mass and a positive charge ...
... 100 atoms thick, suggested that the atom must be mostly empty space! In order to produce the large deflections at C and D, the positively charged alpha particles must be encountering something of very large mass and a positive charge ...
Particles and Waves Summary Notes
... 100 atoms thick, suggested that the atom must be mostly empty space! In order to produce the large deflections at C and D, the positively charged alpha particles must be encountering something of very large mass and a positive charge ...
... 100 atoms thick, suggested that the atom must be mostly empty space! In order to produce the large deflections at C and D, the positively charged alpha particles must be encountering something of very large mass and a positive charge ...
CHP 14
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
Neutron Stars and Black Holes
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
... c. the material will become hot enough that it will radiate most strongly at x-ray wavelengths. d. as the material slows down it converts thermal energy to gravitational potential energy. e. none of the above A rotating black hole a. will produce a pulsar. b. will have a stronger gravitational field ...
Measuring the Masses of Neutron Stars
... of a massive star (M ≥ 8 MA) with a central density that can be as high as 5 to 10 times the density of an atomic nucleus. Neutron stars can be detected as radio sources (radio pulsars) or, when they accrete matter coming from a companion star in a binary system, as X-ray sources. The global structu ...
... of a massive star (M ≥ 8 MA) with a central density that can be as high as 5 to 10 times the density of an atomic nucleus. Neutron stars can be detected as radio sources (radio pulsars) or, when they accrete matter coming from a companion star in a binary system, as X-ray sources. The global structu ...
Nuclear drip line
In nuclear physics, the boundaries for nuclear particle-stability are called drip lines. Atomic nuclei contain both protons and neutrons—the number of protons defines the identity of that element (ie, carbon always has 6 protons), but the number of neutrons within that element may vary (carbon-12 and its isotope carbon-13, for example). The number of isotopes each element may have is visually represented by plotting boxes, each of which represents a unique nuclear species, on a graph with the number of neutrons increasing on the abscissa (X axis) and number of protons increasing along the ordinate (Y axis). The resulting chart is commonly referred to as the table of nuclides, and is to nuclear physics what the periodic table of the elements is to chemistry.An arbitrary combination of protons and neutrons does not necessarily yield a stable nucleus. One can think of moving up and/or to the right across the nuclear chart by adding one type of nucleon (i.e. a proton or neutron, both called nucleons) to a given nucleus. However, adding nucleons one at a time to a given nucleus will eventually lead to a newly formed nucleus that immediately decays by emitting a proton (or neutron). Colloquially speaking, the nucleon has 'leaked' or 'dripped' out of the nucleus, hence giving rise to the term ""drip line"". Drip lines are defined for protons, neutrons, and alpha particles, and these all play important roles in nuclear physics. The nucleon drip lines are at the extreme of the proton-to-neutron ratio: at p:n ratios at or beyond the driplines, no stable nuclei can exist. The location of the neutron drip line is not well known for most of the nuclear chart, whereas the proton and alpha driplines have been measured for a wide range of elements. The nucleons drip out of such unstable nuclei for the same reason that water drips from a leaking faucet: in the water case, there is a lower potential available that is great enough to overcome surface tension and so produces a droplet; in the case of nuclei, the emission of a particle from a nucleus, against the strong nuclear force, leaves the total potential of the nucleus and the emitted particle in a lower state. Because nucleons are quantized, only integer values are plotted on the table of isotopes; this indicates that the drip line is not linear but instead looks like a step function up close.