Assembly techniques for ultra-low mass drift chambers

2014 ◽  
Vol 248-250 ◽  
pp. 124-126 ◽  
Author(s):  
R. Assiro ◽  
M. Cascella ◽  
F. Grancagnolo ◽  
A. L'Erario ◽  
A. Miccoli ◽  
...  
Keyword(s):  
Author(s):  
R. Assiro ◽  
L. Cappelli ◽  
M. Cascella ◽  
L. De Lorenzis ◽  
F. Grancagnolo ◽  
...  
Keyword(s):  

Author(s):  
C Garabatos ◽  
W Karig ◽  
C Müntz ◽  
A Steigerwald ◽  
J Stroth ◽  
...  
Keyword(s):  

Author(s):  
Alessandro MAssimo Baldini ◽  
Toshinori Mori

The possible existence of the \mu \rightarrow {e} \gammaμ→eγ decay predicted by many new physics scenarios is investigated by stopping positive muons in a very thin target and measuring emitted photons and positrons with the best possible resolutions. Photons are measured by a 2.7 ton ultra pure liquid xenon detector while positron trajectories are measured in a specially designed gradient magnetic field by low-mass drift chambers and precisely timed by scintillation counters. A first phase of the experiment (MEG) ended in 2016, and excluded the existence of the decay with branching ratios larger than 4.2 \times 10^{-13}4.2×10−13 (90% C.L.). This provides approximately 30~times stronger constraints on a variety of new physics models than previous experiments. In the second phase (MEG II), most of the detectors have been upgraded by adopting up-to-date technologies to improve the search sensitivity by another order of magnitude down to \mathcal{O}(10^{-14})𝒪(10−14). MEG II will perform a search for physics beyond the Standard Model complementary to high energy collider experiments with compatible or even higher sensitivity.


Author(s):  
H Bokemeyer ◽  
J.l Boyard ◽  
V Chepurnov ◽  
S Chernenko ◽  
H Daues ◽  
...  
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1988 ◽  
Vol 102 ◽  
pp. 47-50
Author(s):  
K. Masai ◽  
S. Hayakawa ◽  
F. Nagase

AbstractEmission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Txof continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ∼ 100 eV formed above the accretion disk. This mechanism is attained for Tx≲ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx> 10 keV is likely due to fluorescence outside the He II ionization front.


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