Abstract
The chamber for direct detection of WIMP with mass < 10 Gev/c2 and axions, emitted from the Sun was developed. The chamber is filled with gas mixture H2 +3ppm TMAE (1,5,10 bar), or D2 + 3ppm TMAE. These gas fillings allow to suppress the electron background. For detecting of events is used the system GEM+pin-anode with coefficient multiplication about 105. In experiment it is necessary to search the early or daily modulation effects.
Highlights
From astronomical observations it is obvious, that the Dark Matter of the Universe exists
J.Va’vra [1] have supposed, that yearly modulation effect in experiments [2] is explained by low mass WIMP scattering on protons of H2O molecules which contamination in detector NaI [2].In work [5] it is shown, that the lightest neutralino is the best WIMP Dark Matter candidates
The addition in detecting gas the TMAE with low ionization potential increases the sensitivity to low mass WIMP in range < 0,5 GeV/c2
Summary
From astronomical observations it is obvious, that the Dark Matter of the Universe exists. Because the WIMP masses > 10 GeV in laboratory experiments are not discovered, it is necessary to search the WIMP with masses ≤ 10 GeV. J.Va’vra [1] have supposed, that yearly modulation effect in experiments [2] is explained by low mass WIMP scattering on protons of H2O molecules which contamination in detector NaI [2].In work [5] it is shown, that the lightest neutralino is the best WIMP Dark Matter candidates
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