scholarly journals New test of supernova electron neutrino emission using Sudbury Neutrino Observatory sensitivity to the diffuse supernova neutrino background

2006 ◽  
Vol 73 (3) ◽  
Author(s):  
John F. Beacom ◽  
Louis E. Strigari
Keyword(s):  
Electron Neutrino ◽  
Neutrino Emission ◽  
Sudbury Neutrino Observatory ◽  
Supernova Neutrino ◽  
Neutrino Background

scholarly journals A Search for Neutrinos from the SolarhepReaction and the Diffuse Supernova Neutrino Background with the Sudbury Neutrino Observatory

2006 ◽  
Vol 653 (2) ◽  
pp. 1545-1551 ◽  
Author(s):  
B. Aharmim ◽  
S. N. Ahmed ◽  
A. E. Anthony ◽  
E. W. Beier ◽  
A. Bellerive ◽  
...  
Keyword(s):  
Sudbury Neutrino Observatory ◽  
Supernova Neutrino ◽  
Neutrino Background

scholarly journals The effect of collective flavor oscillations on the diffuse supernova neutrino background

2008 ◽  
Vol 2008 (09) ◽  
pp. 013 ◽  
Author(s):  
Sovan Chakraborty ◽  
Sandhya Choubey ◽  
Basudeb Dasgupta ◽  
Kamales Kar
Keyword(s):  
Flavor Oscillations ◽  
Supernova Neutrino ◽  
Neutrino Background

scholarly journals IMPACT OF ROTATION ON NEUTRINO EMISSION AND RELIC NEUTRINO BACKGROUND FROM POPULATION III STARS

2008 ◽  
Vol 690 (1) ◽  
pp. 913-922 ◽  
Author(s):  
Yudai Suwa ◽  
Tomoya Takiwaki ◽  
Kei Kotake ◽  
Katsuhiko Sato
Keyword(s):  
Neutrino Emission ◽  
Population Iii Stars ◽  
Neutrino Background ◽  
Population Iii

scholarly journals Can one measure the Cosmic Neutrino Background?

2017 ◽  
Vol 26 (01n02) ◽  
pp. 1740008 ◽  
Author(s):  
Amand Faessler ◽  
Rastislav Hodák ◽  
Sergey Kovalenko ◽  
Fedor Šimkovic
Keyword(s):  
Rest Mass ◽  
Big Bang ◽  
Electron Neutrino ◽  
Electron Neutrinos ◽  
Cosmic Neutrino Background ◽  
Cosmic Neutrino ◽  
The Moment ◽  
Katrin Experiment ◽  
The Big Bang ◽  
Neutrino Background

The Cosmic Microwave Background (CMB) yields information about our Universe at around 380,000 years after the Big Bang (BB). Due to the weak interaction of the neutrinos with matter, the Cosmic Neutrino Background (CNB) should give information about a much earlier time of our Universe, around one second after the BB. Probably, the most promising method to “see” the CNB is the capture of the electron neutrinos from the Background by Tritium, which then decays into 3He and an electron with the energy of the the [Formula: see text]-value [Formula: see text] 18.562[Formula: see text]keV plus the electron neutrino rest mass. The “KArlsruhe TRItium Neutrino” (KATRIN) experiment, which is in preparation, seems presently the most sensitive proposed method for measuring the electron antineutrino mass. At the same time, KATRIN can also look by the reaction [Formula: see text]. The capture of the Cosmic Background Neutrinos (CNB) should show in the electron spectrum as a peak by the electron neutrino rest mass above [Formula: see text]. Here, the possibility to see the CNB with KATRIN is studied. A detection of the CNB by KATRIN seems not to be possible at the moment. But KATRIN should be able to determine an upper limit for the local electron neutrino density of the CNB.

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