scholarly journals Updated results from the RICE experiment and future prospects for ultra-high energy neutrino detection at the south pole

2012 ◽  
Vol 85 (6) ◽  
Author(s):  
I. Kravchenko ◽  
S. Hussain ◽  
D. Seckel ◽  
D. Besson ◽  
E. Fensholt ◽  
...  
Keyword(s):  
High Energy ◽  
South Pole ◽  
Ultra High Energy ◽  
Future Prospects ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Detection ◽  
Energy Neutrino

ULTRA HIGH ENERGY NEUTRINO TELESCOPES

2006 ◽  
Vol 21 (08n09) ◽  
pp. 1914-1924
Author(s):  
PER OLOF HULTH
Keyword(s):  
Lake Baikal ◽  
High Energy ◽  
Atmospheric Neutrinos ◽  
South Pole ◽  
Ultra High Energy ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Neutrino Astronomy

The Neutrino Telescopes NT-200 in Lake Baikal, Russia and AMANDA at the South Pole, Antarctica have now opened the field of High Energy Neutrino Astronomy. Several other Neutrino telescopes are in the process of being constructed or very near realization. Several thousands of atmospheric neutrinos have been observed with energies up to several 100 TeV but so far no evidence for extraterrestrial neutrinos has been found.

scholarly journals On the age vs depth and optical clarity of deep ice at the South Pole

1995 ◽  
Vol 41 (139) ◽  
pp. 445-454
Author(s):  
Keyword(s):  
Visible Light ◽  
High Energy ◽  
Dust Concentration ◽  
Cherenkov Light ◽  
South Pole ◽  
The South ◽  
High Energy Neutrino ◽  
Arrival Times ◽  
Energy Neutrino ◽  
Crystal Boundaries

AbstractThe first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800-1000 m in ice at the South Pole, During the 1995-96 season, as many as six more strings will be deployed at greater depths. Provided absorption, scattering and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of Cherenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the interval 1600-2100 m will be suitably transparent for a future 1 km3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 k year BP.

STUDY OF ACOUSTIC ULTRA-HIGH ENERGY NEUTRINO DETECTION PHASE II

2006 ◽  
Vol 21 (supp01) ◽  
pp. 217-220 ◽  
Author(s):  
N. KURAHASHI
Keyword(s):  
Fiber Optic ◽  
High Energy ◽  
Second Phase ◽  
Ultra High Energy ◽  
Fiber Optic Cable ◽  
Future Plan ◽  
High Energy Neutrino ◽  
Neutrino Detection ◽  
Energy Neutrino ◽  
Hydrophone Array

The Study of Acoustic Ultra-high energy Neutrino Detection has started its second phase (SAUND II). Although the general location of the hydrophones has not changed, SAUND II uses a new hydrophone array that uses a fiber-optic cable to connect to shore. Changes associated with the new hydrophone array as well as a new DAQ system that incorporates multiprocessor computing and accurate GPS timestamping are reported. Initial data of lightbulb calibration conducted in March 2005, and a future plan for a more accurate calibration are also presented.

scholarly journals Evolving Antennas for Ultra-High Energy Neutrino Detection

2021 ◽  
Author(s):  
Julie Anne Rolla ◽  
Dean Arakaki ◽  
Maximilian Clowdus ◽  
Amy Connolly ◽  
Ryan Debolt ◽  
...  
Keyword(s):  
High Energy ◽  
Ultra High Energy ◽  
High Energy Neutrino ◽  
Neutrino Detection ◽  
Energy Neutrino
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