super kamiokande
Skip this Video
Download Presentation

Loading in 2 Seconds...

play fullscreen
1 / 28

SUPER -KAMIOKANDE - PowerPoint PPT Presentation

  • Uploaded on

SUPER -KAMIOKANDE. Kamiokande = Kamioka Nucleon Decay Experiment. Topics of Discussion. Detector Super-Kamiokande Solar neutrinos Results . Properties of Super-K. A Large Water Cherenkov Detector for Cosmic Particles Size: Cylinder of 41.4m (Height) x 39,9m (Diameter)

I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
Download Presentation

PowerPoint Slideshow about 'SUPER -KAMIOKANDE' - delano

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
super kamiokande


Kamiokande = Kamioka Nucleon Decay Experiment

topics of discussion
Topics of Discussion
  • Detector Super-Kamiokande
  • Solar neutrinos
  • Results
properties of super k
Properties of Super-K
  • A Large Water Cherenkov Detector for Cosmic Particles
  • Size: Cylinder of 41.4m (Height) x 39,9m (Diameter)
  • Weight: 50,000 tons of pure Water
  • Number of Photomultipier Tubes: 11,200
how does s k detect
How does S-K detect?

The PMTs collect the pale blue light called Cherenkov light which is emitted by particles travelling faster as light in the water

cherenkov radiation



Compare : shock wave of supersonic airplanes

c0 = speed of light in vacuum

Cherenkov radiation

See for a nice illustration

The picture above shows an incoming 1063 MeV neutrino which strikes a free proton at rest and produces a 1032 MeV muon. Different colors are related to time, blue shows the muon, green the electron of the muon decay.
advantages of s k
Advantages of S-K
  • The direction the neutrino came from can be determined
  • The time of the neutrino’s arrival can be determined
  • The energy of the electron gives a rough estimate of the neutrino energy
time of neutrino s arrival
Time of neutrino’s arrival
  • It is possible to search for day/night or seasonal variations
direction of neutrino
Direction of neutrino
  • One can provide solid evidence that the neutrinos are actually coming from the sun
estimate of neutrino energy
Estimate of neutrino Energy

It is possible to distinguish neutrinos from different reaction chains in the sun

So, where and how are neutrinos produced?

solar fusion 1
Solar fusion 1
  • Basic process in sun and most stars – fusion of hydrogen(protons) into helium

First step is combination of two protons

11H + 11H 21H + e+ +e






solar fusion 2
Solar fusion 2

The cross-section for this process is very small at average proton energies in the core of the sun, however there is a huge number of protons available to react.

Deuterons so produced fuse with protons:

21H + 11H 32H + 

solar fusion 3
Solar fusion 3
  • In our sun 3He is most likely to react with another 3He nucleus.

32He + 32He 42He + 2 11H + 

  • The complete process is given by:

4 11H 42He +2 e+ +2 e +

  • This process is known as the proton-proton cycle or the ‘PPI chain’.
solar fusion 4
Solar fusion 4
  • PPII : 32He + 42He  74Be + 

74Be + e-73Li + e

73Li + 11H 2 42He

  • PPIII: 32He + 42He  74Be + 

74Be + 11H  84Be + e+ + e

84Be  2 42He

solar neutrinos
Solar neutrinos
  • Neutrinos are ‘ghost ‘-particles which merely interact, they are the only known type of particle that can escape from the sun’s core bringing direct information about the solar interior
solar neutrinos 2
Solar neutrinos 2
  • Neutrinos are difficult to detect and measure
  • Neutrinos produced in different branches carry away different amounts of energy and momentum – detector design has to take account
solar neutrinos at s k
Solar neutrinos at S-K
  • Super Kamiokande uses elastic scattering of neutrinos from electrons
  • Cherenkov radiation emitted by the electron is detected


All five blue bars, according to various experiments, show significantly less values than the model predictions: the discrepancy is approximately a factor oftwo
additional result of s k
Additional Result of S-K
  • S-K observes a significant difference between the numbers of neutrinos coming up through the ground as went down on the other side
  • A possible explanation is neutrino conversion takes place in matter – called Mikheyev-Smirnov-Wolfenstein effect
additional result of s k26
Additional Result of S-K
  • Super-K has found evidence of the transformation of muon type neutrinos to something else, probabely tau type neutrinos (neutrino oscillations).
  • This is taken as strong evidence that neutrinos have a small, but finite mass.
what this means
What This Means
  • Neutrino oscillations is today the most promising of the proposed solutions to the solar neutrino problem
Solar neutrino research was undertaken to test stellar evolution
  • Unexpectedly one found evidence for new neutrino physics
  • More experiments are needed to understand neutrino oscillation phenomena