Tesla_WTC_Solution
31st January 2013, 17:35
edit @ friday: If you read the below posts very closely, you will see the evidence that a gamma detector is really a 1st stage nuclear bomb detector, and can sense gamma before the big boom and activate the big shields, I think-- !
Tell me if you like my theory that the particle detectors in Antarctica and Mediterranean sea are really nuclear bomb gamma ray detectors , LOL
_________________________________
I wanted to ask the Avalon community if they were familiar with the Icecube Neutrino Observatory that was built recently in Antarctica.
The idea is this (roughly): the ice provides a wonderful insulator, blocking lots of "harmful" or "interfering" radiation while allowing chargeless neutrinos to quickly pass through.
http://imageshack.us/a/img24/5356/icecubeu.png
Suspended in the ice in Antarctica are a number of ruggedized, spherical computers, installed via a sophisticated machine that boils liquid and makes a very precise (and deep!) hole in the ice.
http://upload.wikimedia.org/wikipedia/commons/thumb/6/6f/ICECUBE_dom_taklampa.jpg/220px-ICECUBE_dom_taklampa.jpg
This device is not alone in its generation. I read last year that such a contraption is being built in the Mediterranean sea on behalf of Israel and perhaps some partner nations.
Well, my question is this: if these things were really for what people say they are, detecting gamma from stars and black holes, etc., I don't think Israel would be wasting money on them. I think these things are precise remote nuclear detonation detectors.
http://upload.wikimedia.org/wikipedia/commons/thumb/7/79/Operation_Upshot-Knothole_-_Badger_001.jpg/250px-Operation_Upshot-Knothole_-_Badger_001.jpg
I would not be surprised if a nuclear bomb lets off many sorts of particles maybe even to include neutrinos. I don't know this for sure. But it seems that any particle detector worth its salt could detect the presence of a nuclear reaction, even across the globe.
http://upload.wikimedia.org/wikipedia/commons/thumb/f/f2/Advanced_Test_Reactor.jpg/250px-Advanced_Test_Reactor.jpg
I heard that the one down south focuses on the Northern Hemisphere.
The one in the Middle East, who knows. I have no idea what they are looking at or why.
I just wanted to give a heads up.
You know, there are people who can detect Cherenkov radiation emitted by such a reaction. Not everyone, and although I jokingly refer to it next to my avatar, I have no idea who is able to do this, except that I read, the particles result in a strobing blue light on the human retina.
http://hyperphysics.phy-astr.gsu.edu/hbase/relativ/imgrel/cerenkov.gif
So keep in mind, your own eyes and brains can detect the presence of certain types of unseen radiation. By seeing the path left (in the future and past!) by the atypically fast moving particle.
Neutrinos typically travel faster than other particles through a medium because they are unimpeded.
To be continued, I hope.
P.s. my air national guard unit was involved with missions to transport scientists related to these remote projects.
Thanks for reading. <3
http://en.wikipedia.org/wiki/IceCube_Neutrino_Observatory for more reading
The IceCube Neutrino Observatory (or simply IceCube) is a neutrino telescope constructed at the Amundsen-Scott South Pole Station in Antarctica.[1] Similar to its predecessor, the Antarctic Muon And Neutrino Detector Array (AMANDA), IceCube contains thousands of spherical optical sensors called Digital Optical Modules (DOMs), each with a photomultiplier tube (PMT)[2] and a single board data acquisition computer which sends digital data to the counting house on the surface above the array.[3] IceCube was completed on 18 December, 2010, New Zealand time.[4]
DOMs are deployed on "strings" of sixty modules each at depths ranging from 1,450 to 2,450 meters, into holes melted in the ice using a hot water drill. IceCube is designed to look for point sources of neutrinos in the TeV range to explore the highest-energy astrophysical processes.
The IceCube project is part of the University of Wisconsin–Madison projects developed and supervised by the same institution, while collaboration and funding is provided by numerous other universities and research institutions worldwide.[5] Construction of IceCube is only possible during the Antarctic austral summer from November to February, when permanent sunlight allows for 24 hour drilling. Construction began in 2005, when the first IceCube string was deployed and collected enough data to verify that the optical sensors worked correctly.[6] In the 2005–2006 season, an additional eight strings were deployed, making IceCube the largest neutrino telescope in the world.
The IceCube Neutrino Observatory is made up of several sub-detectors in addition to the main in-ice array.
AMANDA, the Antarctic Muon And Neutrino Detector Array, was the first part built, and it served as a proof-of-concept for IceCube. AMANDA was turned off in April 2009.[citation needed]
The IceTop array is a series of Cherenkov detectors on the surface of the glacier, two detectors approximately above each IceCube string. IceTop is used as a cosmic ray shower detector, for cosmic ray composition studies and coincident event tests: if a muon is observed going through IceTop, it cannot be from a neutrino interacting in the ice.
The Deep Core Low-Energy Extension is a densely instrumented region of the IceCube array which extends the observable energies below 100 GeV. The Deep Core strings are deployed at the center (in the surface plane) of the larger array, deep in the clearest ice at the bottom of the array (between 1760 and 2450 m deep). There are no Deep Core DOMs between 1850 m and 2107 m depth, as the ice is not as clear in those layers.
Look closely:
Experimental goals
[edit]Point sources of high energy neutrinos
A point source of neutrinos could help explain the mystery of the origin of the highest energy cosmic rays. These cosmic rays have energies high enough that they cannot be contained by galactic magnetic fields (their gyroradii are larger than the radius of the galaxy), so they are believed to come from extra-galactic sources. Astrophysical events which are cataclysmic enough to create such high energy particles would probably also create high energy neutrinos, which could travel to the Earth with very little deflection, because neutrinos interact so rarely. IceCube could observe these neutrinos: its observable energy range is about 100 GeV to several PeV. The more energetic an event is, the larger volume IceCube may detect it in; in this sense, IceCube is more similar to Cherenkov telescopes like the Pierre Auger Observatory (an array of Cherenkov detecting tanks) than it is to other neutrino experiments, such as Super-K (with inward-facing PMTs fixing the fiducial volume).
IceCube is sensitive to point sources more in the northern hemisphere than the southern. It can observe astrophysical neutrino signals from any direction, but in the southern hemisphere these neutrinos are swamped by the downgoing cosmic-ray muon background. Thus, early IceCube point source searches focus on the northern hemisphere, and the extension to southern hemisphere point sources takes extra work.[11]
Although IceCube is expected to detect very few neutrinos (relative to the number of photons detected by more traditional telescopes), it should have very high resolution with the ones that it does find. Over several years of operation, it could produce a flux map of the northern hemisphere similar to existing maps like that of the cosmic microwave background, or gamma ray telescopes, which use particle terminology more like IceCube. Likewise, KM3NeT could complete the map for the southern hemisphere.
IceCube scientists detected their first neutrinos on January 29, 2006.[12]
Gamma ray bursts coincident with neutrinos
When protons collide with one another or with photons, the result is usually pions. Charged pions decay into muons and muon neutrinos whereas neutral pions decay into gamma rays. Potentially, the neutrino flux and the gamma ray flux may coincide in certain sources such as gamma ray bursts and supernova remnants, indicating the elusive nature of their origin. Data from IceCube is being used in conjunction with gamma-ray satellites like Swift or Fermi for this goal. IceCube has not observed any neutrinos in coincidence with GRBs, but is able to use this search to constrain neutrino flux to values less than those predicted by the current models.[13]
Indirect dark matter searches
Weakly interacting massive particle (WIMP) dark matter could be gravitationally captured by massive objects like the Sun and accumulate in the core of the Sun. With a high enough density of these particles, they would annihilate with each other at a significant rate. The decay products of this annihilation could decay into neutrinos, which could be observed by IceCube as an excess of neutrinos from the direction of the Sun. This technique of looking for the decay products of WIMP annihilation is called indirect, as opposed to direct searches which look for dark matter interacting within a contained, instrumented volume. Solar WIMP searches are more sensitive to spin-dependent WIMP models than many direct searches, because the Sun is made of lighter elements than direct search detectors (e.g. xenon or germanium). IceCube has set better limits with the 22 string detector (about 1⁄4 of the full detector) than the AMANDA limits.[14]
Neutrino oscillations
IceCube can observe neutrino oscillations from atmospheric cosmic ray showers, over a baseline across the Earth. It is most sensitive at ~25 GeV, the energy range which Deep Core will be able to see. IceCube can constrain θ23. Deep Core will have the full 6 strings deployed by the end of the 2009–2010 austral summer. As more data is collected and IceCube can refine this measurement, it may be possible to observe a shift in the oscillation peak that determines the neutrino mass hierarchy. This mechanism for determining the mass hierarchy would only work if θ13 is sufficiently large (close to present limits).
Galactic supernovae
Despite the fact that individual neutrinos expected from supernovae have energies well below the IceCube energy cutoff, IceCube could detect a local supernova. It would appear as a detector-wide, brief, correlated rise in noise rates. The supernova would have to be relatively close (within our galaxy) to get enough neutrinos before the 1/r2 distance dependence took over. IceCube is a member of the Supernova Early Warning System (SNEWS).[15]
String theory
The described detection strategy, along with its South Pole position, could allow the detector to provide the first robust experimental evidence of extra dimensions predicted in string theory. Many extensions of the Standard Model of particle physics, including string theory, propose a sterile neutrino; in string theory this is made from a closed string. These could leak into extra dimensions before returning, making them appear to travel faster than the speed of light. An experiment to test this may be possible in the near future.[16] Furthermore, if high energy neutrinos create microscopic black holes (as predicted by some aspects of string theory) it would create a shower of particles; resulting in an increase of "down" neutrinos while reducing "up" neutrinos.[17] There is no group within the IceCube collaboration working on tachyons, travel through extra dimensions, or observations of microscopic black holes.
Results
The IceCube collaboration has published flux limits for neutrinos from point sources,[18] Gamma-ray bursts,[19] and neutralino annihilation in the Sun, with implications for WIMP-proton cross sections.[20]
A shadowing effect from the Moon has been observed.[21][22] Cosmic ray protons are blocked by the Moon, creating a deficit of cosmic ray shower muons in the direction of the Moon. A small (under 1%) but robust anisotropy has been observed in cosmic ray muons.[23]
Tell me if you like my theory that the particle detectors in Antarctica and Mediterranean sea are really nuclear bomb gamma ray detectors , LOL
_________________________________
I wanted to ask the Avalon community if they were familiar with the Icecube Neutrino Observatory that was built recently in Antarctica.
The idea is this (roughly): the ice provides a wonderful insulator, blocking lots of "harmful" or "interfering" radiation while allowing chargeless neutrinos to quickly pass through.
http://imageshack.us/a/img24/5356/icecubeu.png
Suspended in the ice in Antarctica are a number of ruggedized, spherical computers, installed via a sophisticated machine that boils liquid and makes a very precise (and deep!) hole in the ice.
http://upload.wikimedia.org/wikipedia/commons/thumb/6/6f/ICECUBE_dom_taklampa.jpg/220px-ICECUBE_dom_taklampa.jpg
This device is not alone in its generation. I read last year that such a contraption is being built in the Mediterranean sea on behalf of Israel and perhaps some partner nations.
Well, my question is this: if these things were really for what people say they are, detecting gamma from stars and black holes, etc., I don't think Israel would be wasting money on them. I think these things are precise remote nuclear detonation detectors.
http://upload.wikimedia.org/wikipedia/commons/thumb/7/79/Operation_Upshot-Knothole_-_Badger_001.jpg/250px-Operation_Upshot-Knothole_-_Badger_001.jpg
I would not be surprised if a nuclear bomb lets off many sorts of particles maybe even to include neutrinos. I don't know this for sure. But it seems that any particle detector worth its salt could detect the presence of a nuclear reaction, even across the globe.
http://upload.wikimedia.org/wikipedia/commons/thumb/f/f2/Advanced_Test_Reactor.jpg/250px-Advanced_Test_Reactor.jpg
I heard that the one down south focuses on the Northern Hemisphere.
The one in the Middle East, who knows. I have no idea what they are looking at or why.
I just wanted to give a heads up.
You know, there are people who can detect Cherenkov radiation emitted by such a reaction. Not everyone, and although I jokingly refer to it next to my avatar, I have no idea who is able to do this, except that I read, the particles result in a strobing blue light on the human retina.
http://hyperphysics.phy-astr.gsu.edu/hbase/relativ/imgrel/cerenkov.gif
So keep in mind, your own eyes and brains can detect the presence of certain types of unseen radiation. By seeing the path left (in the future and past!) by the atypically fast moving particle.
Neutrinos typically travel faster than other particles through a medium because they are unimpeded.
To be continued, I hope.
P.s. my air national guard unit was involved with missions to transport scientists related to these remote projects.
Thanks for reading. <3
http://en.wikipedia.org/wiki/IceCube_Neutrino_Observatory for more reading
The IceCube Neutrino Observatory (or simply IceCube) is a neutrino telescope constructed at the Amundsen-Scott South Pole Station in Antarctica.[1] Similar to its predecessor, the Antarctic Muon And Neutrino Detector Array (AMANDA), IceCube contains thousands of spherical optical sensors called Digital Optical Modules (DOMs), each with a photomultiplier tube (PMT)[2] and a single board data acquisition computer which sends digital data to the counting house on the surface above the array.[3] IceCube was completed on 18 December, 2010, New Zealand time.[4]
DOMs are deployed on "strings" of sixty modules each at depths ranging from 1,450 to 2,450 meters, into holes melted in the ice using a hot water drill. IceCube is designed to look for point sources of neutrinos in the TeV range to explore the highest-energy astrophysical processes.
The IceCube project is part of the University of Wisconsin–Madison projects developed and supervised by the same institution, while collaboration and funding is provided by numerous other universities and research institutions worldwide.[5] Construction of IceCube is only possible during the Antarctic austral summer from November to February, when permanent sunlight allows for 24 hour drilling. Construction began in 2005, when the first IceCube string was deployed and collected enough data to verify that the optical sensors worked correctly.[6] In the 2005–2006 season, an additional eight strings were deployed, making IceCube the largest neutrino telescope in the world.
The IceCube Neutrino Observatory is made up of several sub-detectors in addition to the main in-ice array.
AMANDA, the Antarctic Muon And Neutrino Detector Array, was the first part built, and it served as a proof-of-concept for IceCube. AMANDA was turned off in April 2009.[citation needed]
The IceTop array is a series of Cherenkov detectors on the surface of the glacier, two detectors approximately above each IceCube string. IceTop is used as a cosmic ray shower detector, for cosmic ray composition studies and coincident event tests: if a muon is observed going through IceTop, it cannot be from a neutrino interacting in the ice.
The Deep Core Low-Energy Extension is a densely instrumented region of the IceCube array which extends the observable energies below 100 GeV. The Deep Core strings are deployed at the center (in the surface plane) of the larger array, deep in the clearest ice at the bottom of the array (between 1760 and 2450 m deep). There are no Deep Core DOMs between 1850 m and 2107 m depth, as the ice is not as clear in those layers.
Look closely:
Experimental goals
[edit]Point sources of high energy neutrinos
A point source of neutrinos could help explain the mystery of the origin of the highest energy cosmic rays. These cosmic rays have energies high enough that they cannot be contained by galactic magnetic fields (their gyroradii are larger than the radius of the galaxy), so they are believed to come from extra-galactic sources. Astrophysical events which are cataclysmic enough to create such high energy particles would probably also create high energy neutrinos, which could travel to the Earth with very little deflection, because neutrinos interact so rarely. IceCube could observe these neutrinos: its observable energy range is about 100 GeV to several PeV. The more energetic an event is, the larger volume IceCube may detect it in; in this sense, IceCube is more similar to Cherenkov telescopes like the Pierre Auger Observatory (an array of Cherenkov detecting tanks) than it is to other neutrino experiments, such as Super-K (with inward-facing PMTs fixing the fiducial volume).
IceCube is sensitive to point sources more in the northern hemisphere than the southern. It can observe astrophysical neutrino signals from any direction, but in the southern hemisphere these neutrinos are swamped by the downgoing cosmic-ray muon background. Thus, early IceCube point source searches focus on the northern hemisphere, and the extension to southern hemisphere point sources takes extra work.[11]
Although IceCube is expected to detect very few neutrinos (relative to the number of photons detected by more traditional telescopes), it should have very high resolution with the ones that it does find. Over several years of operation, it could produce a flux map of the northern hemisphere similar to existing maps like that of the cosmic microwave background, or gamma ray telescopes, which use particle terminology more like IceCube. Likewise, KM3NeT could complete the map for the southern hemisphere.
IceCube scientists detected their first neutrinos on January 29, 2006.[12]
Gamma ray bursts coincident with neutrinos
When protons collide with one another or with photons, the result is usually pions. Charged pions decay into muons and muon neutrinos whereas neutral pions decay into gamma rays. Potentially, the neutrino flux and the gamma ray flux may coincide in certain sources such as gamma ray bursts and supernova remnants, indicating the elusive nature of their origin. Data from IceCube is being used in conjunction with gamma-ray satellites like Swift or Fermi for this goal. IceCube has not observed any neutrinos in coincidence with GRBs, but is able to use this search to constrain neutrino flux to values less than those predicted by the current models.[13]
Indirect dark matter searches
Weakly interacting massive particle (WIMP) dark matter could be gravitationally captured by massive objects like the Sun and accumulate in the core of the Sun. With a high enough density of these particles, they would annihilate with each other at a significant rate. The decay products of this annihilation could decay into neutrinos, which could be observed by IceCube as an excess of neutrinos from the direction of the Sun. This technique of looking for the decay products of WIMP annihilation is called indirect, as opposed to direct searches which look for dark matter interacting within a contained, instrumented volume. Solar WIMP searches are more sensitive to spin-dependent WIMP models than many direct searches, because the Sun is made of lighter elements than direct search detectors (e.g. xenon or germanium). IceCube has set better limits with the 22 string detector (about 1⁄4 of the full detector) than the AMANDA limits.[14]
Neutrino oscillations
IceCube can observe neutrino oscillations from atmospheric cosmic ray showers, over a baseline across the Earth. It is most sensitive at ~25 GeV, the energy range which Deep Core will be able to see. IceCube can constrain θ23. Deep Core will have the full 6 strings deployed by the end of the 2009–2010 austral summer. As more data is collected and IceCube can refine this measurement, it may be possible to observe a shift in the oscillation peak that determines the neutrino mass hierarchy. This mechanism for determining the mass hierarchy would only work if θ13 is sufficiently large (close to present limits).
Galactic supernovae
Despite the fact that individual neutrinos expected from supernovae have energies well below the IceCube energy cutoff, IceCube could detect a local supernova. It would appear as a detector-wide, brief, correlated rise in noise rates. The supernova would have to be relatively close (within our galaxy) to get enough neutrinos before the 1/r2 distance dependence took over. IceCube is a member of the Supernova Early Warning System (SNEWS).[15]
String theory
The described detection strategy, along with its South Pole position, could allow the detector to provide the first robust experimental evidence of extra dimensions predicted in string theory. Many extensions of the Standard Model of particle physics, including string theory, propose a sterile neutrino; in string theory this is made from a closed string. These could leak into extra dimensions before returning, making them appear to travel faster than the speed of light. An experiment to test this may be possible in the near future.[16] Furthermore, if high energy neutrinos create microscopic black holes (as predicted by some aspects of string theory) it would create a shower of particles; resulting in an increase of "down" neutrinos while reducing "up" neutrinos.[17] There is no group within the IceCube collaboration working on tachyons, travel through extra dimensions, or observations of microscopic black holes.
Results
The IceCube collaboration has published flux limits for neutrinos from point sources,[18] Gamma-ray bursts,[19] and neutralino annihilation in the Sun, with implications for WIMP-proton cross sections.[20]
A shadowing effect from the Moon has been observed.[21][22] Cosmic ray protons are blocked by the Moon, creating a deficit of cosmic ray shower muons in the direction of the Moon. A small (under 1%) but robust anisotropy has been observed in cosmic ray muons.[23]