by harry » Wed Jun 21, 2006 7:52 am
Hello All
Not confused
A neutron star is formed after a supenova.
Compact star Encyclopedia II - Compact star - Exotic stars
Compact star: Encyclopedia II - Compact star - Exotic stars
Compact star - Exotic stars
Neutron stars also have a maximum mass, called the Tolman-Oppenheimer-Volkoff limit. It is currently thought to be about 3 times the mass of the Sun. The exact value depends on the forces between neutrons at high density that in addition to the degenerate neutron-pressure could add to the overall pressure. If more mass accretes onto a neutron star, eventually this mass limit is reached, and new equilibriums may be found.
Compact star - Strange stars
It is possible that the neutrons will decompose into their constituent quarks. The star will shrink further, but it may survive in this new state indefinitely if no extra mass is added. It has become the largest nucleon in the universe.
Compact star - Preon stars
If quarks and leptons are not the fundamental elementary particles but are themselves composed of preons, then even denser objects, preon stars, would not be unthinkable. Our star may collapse to one ten-thousandth of its size, bringing its radius to one meter or less. Its density will exceed 1020 g/cm³, and may approach 1030 g/cm³.
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http://web.umr.edu/~om/report_to_fcr/report_to_fcr1.htm
Quote:
The Sun’s radiant energy and protons in the solar wind (SW) come from the collapsed supernova core, a neutron star (NS), on which the Sun formed. The cradle (Figs. 9-12) indicates that the energy of each neutron in the Sun’s central NS exceeds that of a free neutron by @ 10-22 MeV (Figs. 13-15) Solar luminosity and the flux of solar-wind protons are generated by a series of reactions (Fig. 16): a) escape of neutrons from the central NS, b) decay of free neutrons or their capture by other nuclides, c) fusion and upward migration of H+ through material that accreted on the NS, and d) escape of H+ in the SW. An example might be:
a) The escape of neutrons from the NS, <1n> –> 1n + 10-22 MeV
b) The decay of free neutrons, 1n –> 1H+ + e- + nanti + 0.78 MeV
c) Fusion of hydrogen, 4 1H+ + 2 e- –> 4He++ + 2 n + 26.73 MeV
d) Some H+ reaches the surface and departs in the solar wind
Reactions like a) and b) produce part of the Sun’s radiant energy and perhaps the luminosity of isolated neutron stars25. Note that reaction a) alone may release more energy per nucleon than is released by the sum of reactions b) and c), the decay or capture of neutrons plus H-fusion. The well-established Solar Neutrino Puzzle26 confirms that reaction c) generates only part of the Sun’s total luminosity. Most 1H+ from b) is consumed by H-fusion, but the anomalous abundance of H (See Fig.
shows that 1H+ also leaks from the interior, selectively carrying lighter nuclides to the solar surface (See Fig. 6) before departing in the solar wind at an emission rate of about 2.7 x 1043 1H/yr. Homochirality in living creatures26 was likely initiated by circularly polarized light (CPL) from the Sun’s early NS. Their fate and climate changes of planets27 may depend on the half-life of this massive nucleus at the Sun’s core.
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The sun evolved 5 billion years ago from a neutron core. Its composition at this moment is in question. I would assume after 5 billion years the neutron core would have undergone some changes.
The neutron core balance gives the sun a very high density, preventing over heating and keeping the sun from expanding into a red giant.
Just a hydrogen core is not enough to compact to a density high enough.
Neutrons have a neutral charge and can compact close together.
If the core was of Iron composition it would be unstable and its life span would be less than a thousand years.
Its amazing that many scientists do not see what I see.
I will keep on working on this,,,,,,,,,,,,,,,,,,,,,,smile,,,,,and if I'm wrong so be it.
Hello All
Not confused
A neutron star is formed after a supenova.
Compact star Encyclopedia II - Compact star - Exotic stars
Compact star: Encyclopedia II - Compact star - Exotic stars
[quote]Compact star - Exotic stars
Neutron stars also have a maximum mass, called the Tolman-Oppenheimer-Volkoff limit. It is currently thought to be about 3 times the mass of the Sun. The exact value depends on the forces between neutrons at high density that in addition to the degenerate neutron-pressure could add to the overall pressure. If more mass accretes onto a neutron star, eventually this mass limit is reached, and new equilibriums may be found.
Compact star - Strange stars
It is possible that the neutrons will decompose into their constituent quarks. The star will shrink further, but it may survive in this new state indefinitely if no extra mass is added. It has become the largest nucleon in the universe.
Compact star - Preon stars
If quarks and leptons are not the fundamental elementary particles but are themselves composed of preons, then even denser objects, preon stars, would not be unthinkable. Our star may collapse to one ten-thousandth of its size, bringing its radius to one meter or less. Its density will exceed 1020 g/cm³, and may approach 1030 g/cm³.[/quote]
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http://web.umr.edu/~om/report_to_fcr/report_to_fcr1.htm
Quote:
The Sun’s radiant energy and protons in the solar wind (SW) come from the collapsed supernova core, a neutron star (NS), on which the Sun formed. The cradle (Figs. 9-12) indicates that the energy of each neutron in the Sun’s central NS exceeds that of a free neutron by @ 10-22 MeV (Figs. 13-15) Solar luminosity and the flux of solar-wind protons are generated by a series of reactions (Fig. 16): a) escape of neutrons from the central NS, b) decay of free neutrons or their capture by other nuclides, c) fusion and upward migration of H+ through material that accreted on the NS, and d) escape of H+ in the SW. An example might be:
a) The escape of neutrons from the NS, <1n> –> 1n + 10-22 MeV
b) The decay of free neutrons, 1n –> 1H+ + e- + nanti + 0.78 MeV
c) Fusion of hydrogen, 4 1H+ + 2 e- –> 4He++ + 2 n + 26.73 MeV
d) Some H+ reaches the surface and departs in the solar wind
Reactions like a) and b) produce part of the Sun’s radiant energy and perhaps the luminosity of isolated neutron stars25. Note that reaction a) alone may release more energy per nucleon than is released by the sum of reactions b) and c), the decay or capture of neutrons plus H-fusion. The well-established Solar Neutrino Puzzle26 confirms that reaction c) generates only part of the Sun’s total luminosity. Most 1H+ from b) is consumed by H-fusion, but the anomalous abundance of H (See Fig.
shows that 1H+ also leaks from the interior, selectively carrying lighter nuclides to the solar surface (See Fig. 6) before departing in the solar wind at an emission rate of about 2.7 x 1043 1H/yr. Homochirality in living creatures26 was likely initiated by circularly polarized light (CPL) from the Sun’s early NS. Their fate and climate changes of planets27 may depend on the half-life of this massive nucleus at the Sun’s core.
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The sun evolved 5 billion years ago from a neutron core. Its composition at this moment is in question. I would assume after 5 billion years the neutron core would have undergone some changes.
The neutron core balance gives the sun a very high density, preventing over heating and keeping the sun from expanding into a red giant.
Just a hydrogen core is not enough to compact to a density high enough.
Neutrons have a neutral charge and can compact close together.
If the core was of Iron composition it would be unstable and its life span would be less than a thousand years.
Its amazing that many scientists do not see what I see.
I will keep on working on this,,,,,,,,,,,,,,,,,,,,,,smile,,,,,and if I'm wrong so be it.