Line 18 a3y3 Borexino Solar PEP Neutrino SSS Deuterium UFO 5g WOW SETI
View from inside the Borexino neutrino detector. Image Credit Borexino Collaboration
View of the Borexino Stainless Steel Sphere (SSS) from from the Water Tank
Line 18 a3y3 Borexino Solar PEP Neutrino SSS Deuterium UFO 5g WOW SETI
5g force ufo engine acceleration plasma formulas
part 138 of 100 videos there are more videos after this one i’ll post all then update the #.
Math Equation Wow Seti 1977 radio signal alien
14/
3/4/4/1/1/1/1/11=0.017
14/0.017=823.5294
Feb 19 2012 10 10 pm est
My thoughts
Key words found in lines of WOW SETI
Electron volts of energy
Nuclear reactions
High energy
Deuterium
hydrogen
uranium 235
Pep neutrino (now we know what is means)
Pep neutrinos work well in liquids.
Maybe this is the “type” of neutrinos we should use with the liquid argon gas.
vacuum propagation eigenstate
Homestake experiment
GALLEX
GNO
SAGE
gallium
radiochemical experiments
leptonic CP violation
CNO solar neutrino flux
Mikheyev-Smirnov-Wolfenstein
BS05(OP)
astronomical unit
Pp chain
Protons
Neutons
Positrons
Outer space
Nuclear reactions
refractive index of light
First Evidence of pep Solar Neutrinos by Direct Detection in Borexino, Phys. Rev. Lett. 108, 051302 (2012).DOI:10.1103/PhysRevLett.108.051302
Borexino Collaboration succeeds in spotting pep neutrinos emitted from the sun
February 9, 2012 by Bob Yirka
notes
Borexino Collaboration succeeds in spotting pep neutrinos emitted from the sun
February 9, 2012 by Bob Yirka
Enlarge
View of the Borexino “Stainless Steel Sphere” (SSS) from from the “Water Tank”
QUOTES:
(PhysOrg.com) — To learn more about how the sun works, scientists study particles that are emitted from it into space due to thermonuclear reactions that occur inside; by applying known physics principles, they can then deduce which sort of nuclear reactions are taking place.
As one example, researchers have been able to identify high energy proton to proton interactions that are described as pp neutrinos by detecting them when they reach Earth
Now, researchers deep beneath the ground in a mountain in Italy, working together in a group known as the Borexino Collaboration, have spotted the more elusive proton to electron to proton neutrino, a pep reaction that results in the formation of deuterium, a heavy form of hydrogen.
To detect them, the team, as they describe in their paper published in Physical Review Letters, the team had to develop a method of filtering out virtually all other neutrinos, including those from outer space.
To detect the presence of neutrinos, researchers build underground facilities to use the Earth’s natural filtering abilities to remove particle clutter. Then, they fill a big vat with a special kind of liquid that reacts with the type of neutrino they are looking for.
When one of the neutrinos strikes the liquid, a tiny flash or sparkle occurs. By measuring the number of sparkles that occur over a period of time the researchers can describe the amount of such neutrinos that are emitted by the sun, which helps to more fully understand the nuclear reactions that occur inside of it.
Pp neutrinos have been easy to count, they are plentiful and high energy, which makes it easy to detect them when hitting the liquid. Pep, neutrinos on the other hand are low energy and more elusive and up till now have been mostly a theoretical concept.
To detect their presence the team had to devise a means of filtering out virtually all other cosmic particles and then use a liquid that causes a sparkle when struck by a particle that has just 1.44 mega-electron-volts of energy, the distinctive signature of the pep neutrino.
The team succeeded on both counts and were able to detect 3.1 pepneutrino strikes per day, per 100 tons of liquid.
The new technique for cleaning and filtering out unwanted particles is ground breaking work and likely will be used by other scientists looking to measure other particles in other research efforts.
More information: First Evidence of pep Solar Neutrinos by Direct Detection in Borexino, Phys. Rev. Lett. 108, 051302 (2012).DOI:10.1103/PhysRevLett.108.051302
We observed, for the first time, solar neutrinos in the 1.0–1.5 MeV energy range. We determined the rate of pep solar neutrino interactions in Borexino to be 3.1±0.6stat±0.3syst counts/(day·100 ton).
Assuming the pep neutrino flux predicted by the standard solar model, we obtained a constraint on the CNO solar neutrino interaction rate of <7.9 counts/(day·100 ton) (95% C.L.).
The absence of the solar neutrino signal is disfavored at 99.97% C.L., while the absence of the pep signal is disfavored at 98% C.L.
The necessary sensitivity was achieved by adopting data analysis techniques for the rejection of cosmogenic 11C, the dominant background in the 1–2 MeV region.
Assuming the Mikheyev-Smirnov-Wolfenstein large mixing angle solution to solar neutrino oscillations, these values correspond to solar neutrino fluxes of (1.6±0.3)×108 cm-2 s-1 and <7.7×108 cm-2 s-1 (95% C.L.), respectively, in agreement with both the high and low metallicity standard solar models.
These results represent the first direct evidence of the pep neutrino signal and the strongest constraint of the CNO solar neutrino flux to date.
Physics Synopsis
© 2011 PhysOrg.com
Pasted from http://www.physorg.com/news/2012-02-borexino-collaboration-pep-neutrinos-emitted.html
Hydrogen Deuterium Tritium Nuclei Schmatic-ja-textpath.svg (with names in Japanese)
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Hydrogen Deuterium Tritium Nuclei Schmatic-ja-textpath.svg (with names in Japanese)
Feb 19 2012 10 10 pm est
My thoughts
Key words found in lines of WOW SETI
Electron volts of energy
Nuclear reactions
High energy
Deuterium
hydrogen
uranium 235
Pep neutrino (now we know what is means)
Pep neutrinos work well in liquids.
Maybe this is the “type” of neutrinos we should use with the liquid argon gas.
Google
Mikheyev-Smirnov-Wolfenstein
Pasted from http://www.physorg.com/news/2012-02-borexino-collaboration-pep-neutrinos-emitted.html
quote
The Mikheyev–Smirnov–Wolfenstein effect (often referred to as matter effect) is a particle physics process which can act to modify neutrino oscillations in matter.
1978 work by Americanphysicist Lincoln Wolfenstein and 1986 work by Soviet physicists Stanislav Mikheyev and Alexei Smirnov led to an understanding of this effect. Later in 1986, Stephen Parke of Fermilab provided the first full analytic treatment of this effect.
Pasted from http://en.wikipedia.org/wiki/Mikheyev%E2%80%93Smirnov%E2%80%93Wolfenstein_effect
quote
Explanation
The presence of electrons in matter changes the energy levels of the propagation eigenstates of neutrinos due to charged current coherent forward scattering of the electron neutrinos (i.e., weak interactions).
The coherent forward scattering is analogous to the electromagnetic process leading to the refractive index of light in a medium.
This means that neutrinos in matter have a different effective mass than neutrinos in vacuum, and since neutrino oscillations depend upon the squared mass difference of the neutrinos, neutrino oscillations may be different in matter than they are in vacuum.
With antineutrinos, the conceptual point is the same but the effective charge that the weak interaction couples to (called weak isospin) has an opposite sign.
The effect is important at the very large electron densities of the Sun where electron neutrinos are produced. The high-energy neutrinos seen, for example, in SNO (Sudbury Neutrino Observatory) and in Super-Kamiokande, are produced as the higher mass eigenstate in matter ν2m, and remain as such as the density of solar material changes.
(When neutrinos go through the MSW resonance the neutrinos have the maximal probability to change their nature, but it happens that this probability is negligibly small—this is sometimes called propagation in the adiabatic regime).
Thus, the neutrinos of high energy leaving the sun are in a vacuum propagation eigenstate, ν2, that has a reduced overlap with the electron neutrino νe = ν1 cosθ + ν2 sinθ seen by charged current reactions in the detectors.
This is consistent with the experimental observations of low energy Solar neutrinos by the Homestake experiment (the first experiment to reveal the solar neutrino problem), followed by GALLEX, GNO, and SAGE (collectively, gallium radiochemical experiments), and, more recently, the Borexino experiment. These experiments provided further evidence of the MSW effect.
These results are further supported by the reactor experiment KamLAND, that alone is able to provide also a measurement of the parameters of oscillation that is consistent with all other measurements.
The transition between the low energy regime (the MSW effect is negligible) and the high energy regime (the oscillation probability is determind by matter effects) lies in the region of about 2 MeV for the Solar neutrinos.
The MSW effect can also modify neutrino oscillations in the Earth, and future search for new oscillations and/or leptonic CP violation may make use of this property.
Pasted from http://en.wikipedia.org/wiki/Mikheyev%E2%80%93Smirnov%E2%80%93Wolfenstein_effect
A technician works on equipment that feeds a particle beam into the MINOS neutrino oscillation experiment.
A technician works on equipment that feeds a particle beam into the MINOS neutrino oscillation experiment.
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On June 14,2011 the Japanese Tokai-to-Kamioka experiment reported the significant detection of muon-to-electron neutrino changes. On June 24, the Main Injector Neutrino Oscillation Search (MINOS) experiment at Fermilab reported the same. While the ranges of their data varied, the basic claims were the same.
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Refractive Indices
When light travels at an angle between two materials, light bends according to their refractive indices. In order to reflect, light must be on the wider side of the critical angle.
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Refractive Indices diagram light travels at an angle between two materials light bends
quote
Neutrino production
Neutrino flux at Earth predicted by the Standard Solar Model of 2005. The neutrinos produced in the pp chain are shown in black, neutrinos produced by the CNO cycle are shown in blue.
The solar neutrino spectrum predicted by the BS05(OP) standard solar model. The neutrino fluxes from continuum sources are given in units of number cm−2 s−1 MeV−1 at one astronomical unit, and the line fluxes are given in number cm−2s−1.
Hydrogen is fused into helium through several different interactions in the sun. The vast majority of neutrinos are produced through thepp chain, a process in which four protons are combined to produce two protons, two neutrons, two positrons, and two electron neutrinos. Neutrinos are also produced by the CNO cycle, but that process is considerably less important in our sun than in other stars.
Most of the neutrinos produced in the sun come from the first step of the pp chain but their energy is so low (<0.425 MeV)[13]
they are very difficult to detect. A rare side branch of the pp chain produces the "boron-8" neutrinos with a maximum energy of roughly 15 MeV, and these are the easiest neutrinos to detect.
A very rare interaction in the pp chain produces the "hep" neutrinos, the highest energy neutrinos predicted to be produced by our sun. They are predicted to have a maximum energy of about 18 MeV.
All of the interactions described above produce neutrinos with a spectrum of energies. The electron capture of 7Be produces neutrinos at either roughly 0.862 MeV (~90%) or 0.384 MeV (~10%).[13]
[edit]Neutrino detection
The weakness of the neutrino's interactions with other particles means that most neutrinos produced in the core of the sun can pass all the way through the sun without being absorbed.
It is possible, therefore, to observe the core of the sun directly by detecting these neutrinos.
Pasted from http://en.wikipedia.org/wiki/Standard_Solar_Model
quote
Nuclear structure of
Boron 8
(half life = 770 ms). Move mouse over image for B8 nucleus decay form.
Blue toruses = 8 protons
Red toruses = 3 nuclear electrons
Atomic number of B (5) = protons (8) – nuclear electrons (3)
Boron 8 transform by electron capture (from light !) of B8 nucleus decay form and Be8 nucleus generated (half life = 67 as).
Click on image for Be8 nucleus.
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Nuclear structure of boron 8 half life 770 ms decay blue toruses 8 protons red toruses 3 nuclear electrons atomic number b5 8
Line 18 a3h Starshine Retroreflectors SLR NRL SNL Faraday Effect Milky Way WOW SETI
Line 18 a3h Starshine Retroreflectors SLR NRL SNL Faraday Effect Milky Way WOW SETI
part 112 of 100 videos there are more videos after this one i’ll post all then update the #.
Math Equation Wow Seti 1977 radio signal alien
14/
3/4/4/1/1/1/1/11=0.017
14/0.017=823.5294
Sky Hook SpaceDEV STARSYS retroreflectors Laser ranging NRL
STARSHINE-2 and -3 in relation to:
retroreflectors
Laser ranging
NRL Naval Research Laboratory
Sandia National Laboratories.
A retroreflector (sometimes called a retroflector or cataphote) is a device or surface that reflects light back to its source with a minimum scattering of light.
A laser rangefinder is a device which uses a laser beam to determine the distance to an object.
SLR Supports Sensing of Surface Elevations: Satellite Laser Ranging (SLR) provides direct, clear measurements of surface heights of sea level and land surfaces, using satellites and SLR stations on the ground that cross-check each other.
Accurate SLR measurements provide changes in the global mean sea level to a few millimeters per year. Credit: NASA
notes
Wow Seti 1977 radio signal alien
14/
3/4/4/1/1/1/1/11=0.017
14/0.017=823.5294
Google 823.5294
STARSHINE-2 and -3 in relation to:
retroreflectors
Laser ranging
NRL Naval Research Laboratory
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A depiction of an accelerometer designed at Sandia National Laboratories.
Starshine 2 and 3 Satellite Facts
The STARSHINE (STARSHINE stands for Student Tracked Atmospheric Research Satellite Heuristic International Networking Experiment)
A gold corner cube retroreflector
Uses Distance measurement
by optical delay line
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A retroreflector (sometimes called a retroflector or cataphote) is a device or surface that reflects light back to its source with a minimum scattering of light.
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A gold corner cube retroreflector
Laser Ranging
A laser rangefinder is a device which uses a laser beam to determine the distance to an object. The most common form of laser rangefinder operates on the time of flight principle by sending a laser pulse in a narrow beam towards the object and measuring the time taken by the pulse to be reflected off the target and returned to the sender. Due to the high speed of light, this technique is not appropriate for high precision sub-millimeter measurements, where triangulation and other techniques are often used.
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NRL Naval Research Laboratory
Scientists at NRL are part of an international team that has pooled their radio observations into a database, producing the highest precision map to date of the magnetic field within our own Milky Way galaxy.
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SLR Supports Sensing of Surface Elevations: Satellite Laser Ranging (SLR) provides direct, clear measurements of surface heights of sea level and land surfaces, using satellites and SLR stations on the ground that cross-check each other.
Accurate SLR measurements provide changes in the global mean sea level to a few millimeters per year. Credit: NASA
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SLR Supports Sensing of Surface Elevations Satellite Laser Ranging (SLR)
The sky map of the Faraday effect caused by the magnetic fields of the Milky Way
Fig. 1: The sky map of the Faraday effect caused by the magnetic fields of the Milky Way. Red and blue colors indicate regions of the sky where the magnetic field points toward and away from the observer, respectively.
The band of the Milky Way (the plane of the Galactic disk) extends horizontally in this panoramic view. The center of the Milky Way lies in the middle of the image.
The North celestial pole is at the top left and the South Pole is at the bottom right. (Image Credit: Max Planck Institute for Astrophysics)
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Satellite Laser Ranging (SLR) network.
Satellites in the SLR: This graphic shows the constellation of satellites supported by the Satellite Laser Ranging (SLR) network.
Data spanning 28 years from 8 satellites are used for measuring the large-scale mass movements on the Earth and global solid Earth dynamics.
Click on image to enlarge. Credit: NASA
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WIMP dark matter event recoil energy wow seti graph
Line 18 a3y2 Dark Matter Neutrinos ARGON Xenon U235 Formula UFO 5g WOW SETI
quote
The ArDM experiment
Search for Dark Matter in the Universe with liquid Argon
CIEMAT – ETH/Zurich – Univ Granada – Univ Sheffield – Soltan Institute Warszawa – Univ Zurich
Astronomical observations give strong evidence for the existence of non-luminous and non-baryonic matter, presumably composed of a new type of elementary particle.
A leading candidate is the Weakly Interacting Massive Particle (WIMP). If they exist, WIMPs should form a cold thermal relic gas, which could be detected via elastic collisions with nuclei of ordinary matter.
The detection of these WIMPs is based on the capability of measuring the recoils of target nuclei with kinetic energy in the range of 10-100 keV. The signal is therefore quite elusive and is expected to be a rare event given the weak coupling between WIMPs and ordinary matter.
A better understanding of the DAMA result or alternatively the coverage of large fractions of the remaining theoretical parameter space of theories accommodating WIMPs
(e.g. supersymmetric extensions of the Standard Model) can only be achieved at the cost of improved detector technologies that are compatible with large target masses. Current experimental results from CDMS, ZEPLIN, and EDELWEISS exclude cross-sections above a few
10–42 cm2.
Noble liquid detectors using Xenon or Argon can efficiently act as targets for Weakly Interacting Massive Particles (WIMP) detection.
Xenon or Argon provide a high event rate because of their high density and high atomic number and large target masses are readily conceivable.
They have high scintillation and ionization yields because of their low ionization potentials.
Both scintillation and ionization are measurable and can be used to very effectively discriminate between nuclear recoils and gamma/electron backgrounds.
The use of noble liquid gases to detect WIMP dark matter is currently the subject of intense R&D carried out by a number of groups worldwide.
In these detectors, one relies on the simultaneous detection of the ionization charge and of the scintillation light produced during a nuclear recoil event.
A main subject for any such detector is the method of the readout for the ionization and scintillation.
Currently, the XENON ZEPLINand WARP designs rely exclusively on photomultipliers (PMTs) for their readout. The possibility to directly detect the ionization charge is less well developed although it might provide alternative and potentially large benefits.
Given the low energy thresholds necessary to efficiently detect WIMP signals, this method however requires the charge to be amplified before it is read out.
While amplification is not possible in the liquid Argon phase, it can be achieved in the vapor in equilibrium on top of the liquid, although operation in this context precludes the inclusion of common avalanche quenchers, since they will condense in the liquid phase.
Pasted from http://neutrino.ethz.ch/ArDM/
Feb 19 2012 916 pm est
My thoughts
Looking at this quote:
While amplification is not possible in the liquid Argon phase, it can be achieved in the vapor in equilibrium on top of the liquid, although operation in this context precludes the inclusion of common avalanche quenchers, since they will condense in the liquid phase.
My thoughts continued
Earlier I mentioned that you spray the ice cold neutrons and particles that have collided with a mist of water at a different temperature a bit warmer so that it will show up?
Key words in this Quote:
Xenon or Argon provide a high event rate because of their high density and high atomic number and large target masses are readily conceivable.
So I googled XENON to see what types of particles it has.
quote
Xenon is a chemical element with the symbol Xe and atomic number 54. The element name is pronounced
/ˈzɛnɒn/ zen-on or/ˈziːnɒn/ zee-non. A colorless, heavy, odorless noble gas, xenon occurs in the Earth’s atmosphere in trace amounts.[6]
Although generally unreactive, xenon can undergo a few chemical reactions such as the formation of xenon hexafluoroplatinate, the first noble gas compound to be synthesized.[7][8][9]
Naturally occurring xenon consists of nine stable isotopes. There are also over 40 unstable isotopes that undergo radioactive decay.
The isotope ratios of xenon are an important tool for studying the early history of the Solar System.
[10] Radioactive xenon-135 is produced from iodine-135 as a result of nuclear fission, and it acts as the most significant neutron absorber in nuclear reactors.[11]
he first excimer laser design used a xenondimer molecule (Xe2) as its lasing medium,[15] and the earliest laser designs used xenon flash lamps as pumps.[16]
Xenon is also being used to search for hypothetical weakly interacting massive particles[17] and as the propellant for ion thrusters inspacecraft.[18]
Pasted from http://en.wikipedia.org/wiki/Xenon
Feb 19 2012 921 pm est 952 pm est (reading material)
My Thoughts.
Xenon is a bi product of fission of Uranium 235.
I have another formula idea for you now:
U 235 comes up in an earlier line of data and we were going to use that in the process of exciting the neutrinos + liquid Argon Gas + Laser Beam + turbine Invention + Sputtering Gun Invention + Leptons
Quotes from Xenon data:
Naturally occurring xenon consists of nine stable isotopes.
Radioactive xenon-135 is produced from iodine-135 as a result of nuclear fission, and it acts as the most significant neutron absorber in nuclear reactors.[11]
Quote
The noble gases are a group of chemical elements with very similar properties: under standard conditions, they are all odorless, colorless, monatomic gases, with very low chemical reactivity. The six noble gases that occur naturally are helium (He), neon (Ne), argon (Ar), krypton (Kr), xenon (Xe), and the radioactiveradon (Rn).
Pasted from http://en.wikipedia.org/wiki/Noble_gas
