I done the Experimental Research offered by the work for Nobel Laureates in Physics, University of California, Berkeley CA background - one Who is Emeritus Professor Russell Kulsrud {1} and V.L. Ginzburg {2} and the others are from Caltech and Chicago. I learned how to make a laboratory device that is used in our research laboratory purpose, the resistance heating device we call it furnace for Laboratory Works. Usually the samples are heating by Radiation Resistance Process we call it Black Body Radiation {3}, In this process we make the Laboratory Samples by pure and impure for electrical conduction. In impure samples samples are defect made {4} electrical charge conduction couple to the devices we choose it for research works in Advanced Research Laboratories. Detection of vacuum conditions by epoch {5} and Thanks for providing me an experience with <<elements>> these are importance in Thermonuclear Supernova conditions {6} to check their origin as nuclear content in the Universe. Further more on this Professor Sir Steven C. Cowley Princeton Plasma Physics Laboratory Princeton University and Harvard University advisory council.

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I learned in Theoretical Research how to make defects in atom for an electron motion in an atomic orbitals and the Dislocation Theory by Emeritus Professor Jean-Loup STRUDEL {1}. The man made Objects for Charge Coupling Oscillations and Resonance. The Electrons are the first fundamental particles to work in Research Laboratories to understand the final motion and force equivalent scalar properties in Lagrangian or Tensor made objects in Hamiltonian Mechanics.

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We have tried to develop as fully as possible all matters of physical interest, and to do so in such a way as to give the clearest possible picture of the phenomena and their interrelation by Professor Alexander A. Schekochihin, Rudolf Peierls Centre for Theoretical Physics, Oxford University. Accordingly, we discuss neither approximate methods of calculation in fluid mechanics, nor empirical theories devoid of physical significance. On the other hand, accounts are given of some topics by Pratt & Whitney Chair : Roddam Narasimha, California Institute of Technology, Pasadena.

                                                                                                                                    

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Can a uniformly moving electron emit Radiation? The Hamiltonian approach to Electrodynamics. Applications of Electrodynamics in Theoretical Physics and Astrophysics leaves the signature of Transition. All the transitions are not the spectral lines but even a single transition theoretically important. Gamma Ray Cosmology merely an answer to the question of interest for the quest of transitions at very high energies and also standard candles of highest distant objects.

 

Supernova explosions in other galaxies and collapse of galactic nuclei are the promising events in an Observational Cosmology and also important in an Extragalactic Astronomy. More physically energy density of final states of proton-nuclear components in a Scientific Research Laboratories - Rocket fires from Launching - Decays of Hyperons and some Mesons are evidence for an high intense and pure Electromagnetic Beam Research. 

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Dark Energy Components {7} of a Single Photon of Gamma Ray for Relativistic Effects and non-relativistic effects of a single photon momenta of Rocket fires for a Theoretical and  an Experimental Physics of outstanding and evergreen problems. Radiation reaction of Gamma Rays {8} in the Gravitational fields and probes of  Dark Energy like SNAP is a most powerful tool for today detection of Dark Energy.

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Quantum Structure of the Universe​ of a Zero Point Energy and its origin of the Electromagnetic Laws and how an anisotropic at an absolute temperature of a Zero Point Energy Equations for an approximation of  a new epoch of Oscillations and vibration detection of resonating techniques and probing at large scales.  
 

 

Finding the echo of Big bang {7},  Searching the probes for an Electrodynamics of Magnetic Monopole Physics and Problem of Baryon Acoustic Oscillations for proton nucleon content of matter wave radiation reaction and Cosmic Micro Wave Background Radiation as a probe for  studying the over all evolution of the Universe.

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References:

[1-(a)]. William Alfred Fowler, The Nobel Prize in Physics (1983), Affiliation at the time of the award: California Institute of Technology (Caltech), Pasadena, CA, USA. Prize motivation: “for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe”. Work: Stars in the universe form from clouds of gas and dust. When these clouds are pulled together by gravitational force, energy is released in the form of heat. And when a high enough temperature is reached, reactions among the atomic nuclei in the star’s interior begin. These reactions are what causes radiation from stars. In the 1950s William Fowler showed how these nuclear reactions also account for how various elements are formed. These processes have created the elements that make up our earth and other heavenly bodies in the universe.

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[1-(b)]. Subrahmanyan Chandrasekhar, The Nobel Prize in Physics (1983), Affiliation at the time of the award: University of Chicago, Chicago, IL, USA. Prize motivation: “for his theoretical studies of the physical processes of importance to the structure and evolution of the stars”. Work: Stars in the universe form from clouds of gas and dust. When these clouds are pulled together by gravitational force, energy is released in the form of heat. And when a high enough temperature is reached, reactions among the atomic nuclei in the star’s interior begin. Beginning in the 1930s, Subramanyan Chandrasekhar formulated theories for the development that stars subsequently undergo. He showed that when the hydrogen fuel of stars of a certain size begins to run out, it collapses into a compact, brilliant star known as a white dwarf.

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[2]. Hans Albrecht Bethe, The Nobel Prize in Physics (1967). Affiliation at the time of the award: Cornell University, Ithaca, NY, USA. Prize motivation: “for his contributions to the theory of nuclear reactions, especially his discoveries concerning the energy production in stars”. Work: The discovery of fission—the splitting of heavy nuclei—revealed the liberation of large quantities of energy; an effect now exploited in nuclear reactors. This energy is generated by differences in mass. Energy is also liberated when light nuclei combine to form heavier ones, i.e. fusion. In 1938, Hans Bethe proved that fusion produces the enormous energy emitted by stars. He proposed two different processes, both of which result in hydrogen nuclei fusing with helium nuclei.

[3-(a)]. George F. Smoot, The Nobel Prize in Physics (2006). Affiliation at the time of the award: University of California, Berkeley, CA, USA. Prize motivation: “for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation”. Work: Various types of particles and radiation travel through outer space, including cosmic background radiation, which has been carefully studied through measurements from the COBE satellite. George Smoot led a project that in 1992 was able to point out small variations in radiation in different directions. This provides a clue to how stars and other heavenly bodies have come into existence. The variations can be explained by a kind of quantum mechanical fluctuations that have caused matter in certain places to form clumps that then have grown because of gravitation.

[3-(b)]. John C. Matherher, Nobel Prize in Physics (2006).Affiliation at the time of the award: NASA Goddard Space Flight Center, Greenbelt, MD, USA. Prize motivation: “for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation”. Work: Various types of particles and radiation travel through outer space, including cosmic background radiation, which has been carefully studied through measurements from the COBE satellite. John Mather, a driving force in the project, had particular responsibility for a part that in 1989 indicated that cosmic background radiation’s spectrum corresponds to black-body radiation—radiation emitted by a dark, glowing body. The result provided evidence that the background radiation is a remnant from the creation of the universe in the Big Bang.

[4-(a)]. Albert Fert, The Nobel Prize in Physics (2007). Affiliation at the time of the award: Université Paris-Sud, Orsay, France; Unité Mixte de Physique CNRS/THALES, Orsay, France. Prize motivation: “for the discovery of Giant Magnetoresistance”. Work: When materials are reduced to just a few atomic layers—a few nanometers in thickness—their properties change. Independently of one another, Albert Fert and Peter Grünberg discovered the phenomenon Giant Magneto Resistance (GMR) in 1988. GMR involves small changes in magnetic fields creating major differences in electrical resistance. It has also had an impact on electronics, especially read heads, where information stored magnetically is converted to electric current. Thanks to GMR, hard drives have become much smaller.

 

[4-(b)]. Peter Grünberg, The Nobel Prize in Physics (2007). Affiliation at the time of the award: Forschungszentrum Jülich, Jülich, Germany. Prize motivation: “for the discovery of Giant Magnetoresistance” Work: When materials are reduced to just a few atomic layers—a few nanometers in thickness—their properties change. Independently of one another, Peter Grünberg and Albert Fert discovered the phenomenon Giant Magneto Resistance (GMR) in 1988. GMR involves small changes in magnetic fields creating major differences in electrical resistance. It has also had an impact on electronics, especially read heads, where information stored magnetically is converted to electric current. Thanks to GMR, hard drives have become much smaller. 

[5-(a)].Victor Franz Hess, The Nobel Prize in Physics (1936). Affiliation at the time of the award: Innsbruck University, Innsbruck, Austria. Prize motivation: “for his discovery of cosmic radiation”. Work: When radiation and atoms interact, charged atoms, ions, are often produced. In 1912 Victor Hess measured atmospheric ionization as function of altitude using balloons. Surprisingly, he found that ionization first decreased, but then increased again at higher altitudes. He concluded that the upper atmosphere is ionized by radiation from space. He proved that this radiation is not solar through experiments performed at night and during eclipses: cosmic rays had been discovered.

 

[5-(b)]. Carl David Anderson, The Nobel Prize in Physics (1936). Affiliation at the time of the award: California Institute of Technology (Caltech), Pasadena, CA, USA. Prize motivation: “for his discovery of the positron”. Work: In developing quantum mechanical theory, Dirac predicted that all matter has a kind of mirror image—antimatter. A particle and its antiparticle, if charged, should have opposite charges. By studying the tracks of cosmic ray particles in a cloud chamber, in 1932 Carl Anderson discovered a positively-charged particle with a mass seemingly equal to that of an electron. Anderson’s particle was the first antiparticle proven by experiment and was named a “positron”.

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[5-(c)]. ​Paul Adrien Maurice Dirac, The Nobel Prize in Physics (1933). Affiliation at the time of the award: University of Cambridge, Cambridge, United Kingdom. Prize motivation: “for the discovery of new productive forms of atomic theory”. Work: During the intense period of 1925-26 quantum theories were proposed that accurately described the energy levels of electrons in atoms. These equations needed to be adapted to Einstein’s theory of relativity, however. In 1928 Paul Dirac formulated a fully relativistic quantum theory. The equation gave solutions that he interpreted as being caused by a particle equivalent to the electron, but with a positive charge. This particle, the positron, was later confirmed through experiments.

 

[5-(d)]. Erwin Schrödinger, The Nobel Prize in Physics (1933). Affiliation at the time of the award: Berlin University, Berlin, Germany. Prize motivation: “for the discovery of new productive forms of atomic theory”. Work: In Niels Bohr’s theory of the atom, electrons absorb and emit radiation of fixed wavelengths when jumping between fixed orbits around a nucleus. The theory provided a good description of the spectrum created by the hydrogen atom, but needed to be developed to suit more complicated atoms and molecules. Assuming that matter (e.g., electrons) could be regarded as both particles and waves, in 1926 Erwin Schrödinger formulated a wave equation that accurately calculated the energy levels of electrons in atoms.

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​[5-(e)]. John Hasbrouck Van Vleck, The Nobel Prize in Physics (1977). Affiliation at the time of the award: Harvard University, Cambridge, MA, USA. Prize motivation: “for their fundamental theoretical investigations of the electronic structure of magnetic and disordered systems”. Work: The electrical and magnetic properties of different materials are determined by how the electrons move about in relation to the atomic nucleus. When an atom from a foreign substance is inserted into a crystalline structure, the crystal’s properties can be altered. During the 1930s John Van Vleck developed theories about how electrical fields in a crystal affect a foreign atom and how such an atom can be bound to nearby atoms through its electrons. He also showed how the interaction between the electron’s movements can create local magnetic moments in crystals.

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​[5-(f)]. Sir Nevill Francis Mott, The Nobel Prize in Physics (1977). Affiliation at the time of the award: University of Cambridge, Cambridge, United Kingdom. Prize motivation: “for their fundamental theoretical investigations of the electronic structure of magnetic and disordered systems”. Work: The electrical and magnetic properties of different materials, which are significant in electronics and other areas, are determined by the movements of electrons in relation to atomic nuclei and to one another. By observing the interaction between electrons, Nevill Mott explained in 1949 how certain crystals can alternate between being electrical conductors and insulators. He also has contributed to the development of new concepts for a deeper understanding of solid materials that do not have a regular crystalline structure but constitute disordered systems.

​[5-(g)]. Philip Warren Anderson, The Nobel Prize in Physics (1977​). Affiliation at the time of the award: Bell  Telephone Laboratories, Murray Hill, NJ, USA. Prize motivation: “for their fundamental theoretical investigations of the electronic structure of magnetic and disordered systems”. Work: Solid materials often have a regular crystalline structure and composition, but sometimes they constitute disordered systems. These could be alloys with a regular structure but a more random composition. Other solid materials, such as glass, lack a regular structure. In 1958 Philip Anderson showed the conditions under which an electron can move about freely within a disordered system and when it is more or less bound to a specific place. This and other works have contributed to a deeper understanding of electrical phenomena in disordered systems.

 

[5-(h)]. Julian Schwinger, The Nobel Prize in Physics (1965). Affiliation at the time of the award: Harvard University, Cambridge, MA, USA. Prize motivation: “for their fundamental work in quantum electrodynamics, with deep-ploughing consequences for the physics of elementary particles”. Work: Following the establishment of the theory of relativity and quantum mechanics, an initial relativistic theory was formulated for the interaction between charged particles and electromagnetic fields. However, partly because the electron’s magnetic moment proved to be somewhat larger than expected, the theory had to be reformulated. Julian Schwinger solved this problem in 1948 through “renormalization” and thereby contributed to a new quantum electrodynamics.

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[6-(a)]. Saul Perlmutter, The Nobel Prize in Physics (2011). Affiliation at the time of the award: Lawrence Berkeley National Laboratory, Berkeley, CA, USA; University of California, Berkeley, CA, USA. Prize motivation: “for the discovery of the accelerating expansion of the Universe through observations of distant supernovae”. Work: The universe’s stars and galaxies are moving away from one another; the universe is expanding. Up until recently, the majority of astrophysicists believed that this expansion would eventually wane, due to the effect of opposing gravitational forces. Saul Perlmutter, Brian Schmidt, and Adam Riess studied exploding stars, called supernovae. Because the light emitted by stars appears weaker from a larger distance and takes on a reddish hue as it moves further from the observer, the researchers were able to determine how the supernovae moved. In 1998 they reached a surprising result: the universe is expanding at an ever-increasing rate.

 

[6-(b)]. Brian P. Schmidt, The Nobel Prize in Physics (2011). Affiliation at the time of the award: Australian National University, Weston Creek, Australia. Prize motivation: “for the discovery of the accelerating expansion of the Universe through observations of distant supernovae”. Work: The universe’s stars and galaxies are moving away from one another; the universe is expanding. Up until recently, the majority of astrophysicists believed that this expansion would eventually wane, due to the effect of opposing gravitational forces. Saul Perlmutter, Brian Schmidt, and Adam Riess studied exploding stars, called supernovae. Because the light emitted by stars appears weaker from a larger distance and takes on a reddish hue as it moves further from the observer, the researchers were able to determine how the supernovae moved. In 1998 they reached a surprising result: the universe is expanding at an ever-increasing rate.

 

[6-(c)]. Adam G. Riess, The Nobel Prize in Physics (2011). Affiliation at the time of the award: Johns Hopkins University, Baltimore, MD, USA; Space Telescope Science Institute, Baltimore, MD, USA. Prize motivation: “for the discovery of the accelerating expansion of the Universe through observations of distant supernovae”. Work: The universe’s stars and galaxies are moving away from one another; the universe is expanding. Up until recently, the majority of astrophysicists believed that this expansion would eventually wane, due to the effect of opposing gravitational forces. Saul Perlmutter, Brian Schmidt, and Adam Riess studied exploding stars, called supernovae. Because the light emitted by stars appears weaker from a larger distance and takes on a reddish hue as it moves further from the observer, the researchers were able to determine how the supernovae moved. In 1998 they reached a surprising result: the universe is expanding at an ever-increasing rate.

 

 

[7-(a)]. Luis Walter Alvarez, The Nobel Prize in Physics (1968). Affiliation at the time of the award: University of California, Berkeley, CA, USA. Prize motivation: “for his decisive contributions to elementary particle physics, in particular the discovery of a large number of resonance states, made possible through his development of the technique of using hydrogen bubble chamber and data analysis”. Work: Opportunities to investigate our world’s smallest components were revolutionized by C.T.R. Wilson’s invention of the cloud chamber and Donald Glaser’s invention of the bubble chamber. In these devices electrically charged particles leave trails behind them. In the latter part of the 1950s, Luis Alvarez further developed the bubble chamber by using liquid hydrogen. He also developed new measurement systems and computer-based methods for analyzing large quantities of data. This has led to the discovery of a number of previously unknown particles.

 

[7-(b)]. Murray Gell-Mann, The Nobel Prize in Physics (1969). Affiliation at the time of the award: California Institute of Technology (Caltech), Pasadena, CA, USA. Prize motivation: “for his contributions and discoveries concerning the classification of elementary particles and their interactions”. Work: During the 1950s and 1960s, new accelerators and apparatuses helped identify many new elementary particles. In theoretical works from the same period, Murray Gell-Mann classified particles and their interactions. He proposed that observed particles are in fact composite, that is, comprised of smaller building blocks called quarks. According to this theory, as-yet-undiscovered particles should exist. When these were later found in experiments, the theory was accepted.

 

[7-(c)]. Richard P.  Feynman, The Nobel Prize in Physics (1965). Affiliation at the time of the award: California Institute of Technology (Caltech), Pasadena, CA, USA. Prize motivation: “for their fundamental work in quantum electrodynamics, with deep-ploughing consequences for the physics of elementary particles”. Work: Following the establishment of the theory of relativity and quantum mechanics, an initial relativistic theory was formulated for the interaction between charged particles and electromagnetic fields. This needed to be reformulated, however. In 1948 in particular, Richard Feynman contributed to creating a new quantum electrodynamics by introducing Feynman diagrams: graphic representations of various interactions between different particles. These diagrams facilitate the calculation of interaction probabilities.

 

 [7-(d)].

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L - Mode,  C - Mode, O -Mode, H - Mode, X - Mode, Spherical Torus - Mode,

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WALL BOUND / BOUNDARY LAYER THEORY/ ASYMPTOTIC FREEDOM

 

(nuclear content of the universe filled with   quark gulon plasmas) 

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​References:

 

Frank Wilczek, The Nobel Prize in Physics (2004). Affiliation at the time of the award: Massachusetts Institute of Technology (MIT), Cambridge, MA, USA. Prize motivation: “for the discovery of asymptotic freedom in the theory of the strong interaction”. Work:The atomic nucleus is held together by a powerful, strong interaction that binds together the protons and neutrons that comprise the nucleus. The strong interaction also holds together the quarks that make up protons and neutrons. This interaction is so strong that no free quarks have ever been observed. However, in 1973 Frank Wilczek, David Gross, and David Politzer came up with a theory postulating that when quarks come really close to one another, the attraction abates and they behave like free particles. This is called asymptotic freedom.

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H. David Politzer,The Nobel Prize in Physics (2004).Affiliation at the time of the award: California Institute of Technology (Caltech), Pasadena, CA, USA. Prize motivation: “for the discovery of asymptotic freedom in the theory of the strong interaction”. Work: The atomic nucleus is held together by a powerful,strong interaction that binds together the protons and neutrons that comprise the nucleus. The strong interaction also holds together the quarks that make up protons and neutrons. This interaction is so strong that no free quarks have ever been observed. However, in 1973 David Politzer, David Gross, and Frank Wilczek came up with a theory postulating that when quarks come really close to one another, the attraction abates and they behave like free particles. This is called asymptotic freedom.

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David J. Gross, The Nobel Prize in Physics (2004). Affiliation at the time of the award: University of California, Kavli Institute for Theoretical Physics, Santa Barbara, CA, USA. Prize motivation: “for the discovery of asymptotic freedom in the theory of the strong interaction”. Work: The atomic nucleus is held together by a powerful, strong interaction that binds together the protons and neutrons that comprise the nucleus. The strong interaction also holds together the quarks that make up protons and neutrons. This interaction is so strong that no free quarks have ever been observed. However, in 1973 David Gross, David Politzer, and Frank Wilczek came up with a theory postulating that when quarks come really close to one another, the attraction abates and they behave like free particles. This is called asymptotic freedom.

 

 

​Plasma Fluids/ Heavy Ions/ Astrophysical Plasmas/ Laboratory Plasmas/ Fusion Plasmas: 

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Hannes Olof Gösta Alfvén, The Nobel Prize in Physics (1970). Affiliation at the time of the award: Royal Institute of Technology, Stockholm, Sweden. Prize motivation: “for fundamental work and discoveries in magnetohydro-dynamics with fruitful applications in different parts of plasma physics”. Work: The phenomenon of aurora borealis occurs when bursts of charged particles from the sun collide with the earth’s magnetic field. These jets of particles are an example of a special state of matter—plasma. Plasma is a gas comprised of electrons and ions (electrically charged atoms) that forms at high temperatures.From the late 1930s onward,Hannes Alfvén developed a theory about aurora borealis, which led to magneto-hydrodynamics; the theory of the relationships between a plasma’s movements, electric currents and fields, and magnetic fields.

 

 

 

Louis Eugène Félix Néel, The Nobel Prize in Physics (1970).Affiliation at the time of the award: University of Grenoble, Grenoble, France. Prize motivation: “for fundamental work and discoveries concerning antiferromagnetism and ferrimagnetism which have led to important applications in solid state physics”. Work: Magnetism takes different forms, some stemming from the magnetic moments of atoms of different materials. In ferromagnetic material the magnetic moments are oriented in the same direction. In 1932 Louis Néel described the antiferromagnetism phenomenon, where nearby magnetic moments in a material are oriented in opposite directions. In 1947 he also described the ferrimagnetism phenomenon, where the magnetic moments are aligned in opposite directions but of different magnitudes. The findings became an important factor in the development of computer memory and other applications.

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