Search for solar axions via axion-photon coupling with the Majorana Demonstrator

Arnquist, I. J.; Avignone, F. T.; Barabash, A. S.; Barton, C. J.; Bhimani, K. H.; Blalock, E.; Bos, B.; Busch, M.; Buuck, M.; Caldwell, T. S.; Chan, Y-D.; Christofferson, C. D.; Chu, P. -H.; Clark, M. L.; Cuesta, C.; Detwiler, J. A.; Efremenko, Yu.; Ejiri, H.; Elliott, S. R.; Giovanetti, G. K.; Green, M. P.; Gruszko, J.; Guinn, I. S.; Guiseppe, V. E.; Haufe, C. R.; Henning, R.; Aguilar, D. Hervas; Hoppe, E. W.; Hostiuc, A.; Kidd, M. F.; Kim, I.; Kouzes, R. T.; Lannen, T. E.; Li, A.; Lopez, A. M.; López-Castaño, J. M.; Martin, E. L.; Martin, R. D.; Massarczyk, R.; Meijer, S. J.; Oli, T. K.; Othman, G.; Paudel, L. S.; Pettus, W.; Poon, A. W. P.; Radford, D. C.; Reine, A. L.; Rielage, K.; Ruof, N. W.; Schaper, D. C.; Tedeschi, D.; Varner, R. L.; Vasilyev, S.; Wilkerson, J. F.; Wiseman, C.; Xu, W.; Yu, C. -H.; Zhu, B. X.

doi:10.48550/arxiv.2206.05789

Cited by 2 publications

(7 citation statements)

References 52 publications

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“…During this time, the specific activities of cosmogenic radionuclides will decrease through decay. The manufacturing/processing steps and specific activities of the considered radionuclides are presented in tables 2 and 3, respectively, compared with a competitive Ge-based experiment, the MAJORANA DEMONSTRATOR (denoted as MJD) [45][46][47][48][49], in cosmogenic radionuclide-induced background sensitivity. The 3 H radioactivity of CDEX-50, which contributes most in the low-energy region, is lower than that of MJD by a factor of ∼6.…”

Section: Cosmogenic Radioactivitymentioning

confidence: 99%

“…Manufacturing/processing step CDEX-50 MJD Shielding 3. Specific activities of the cosmogenic radionuclides of the germanium crystal after 3 years of cooling down, along with MJD with approximately 4 years of cooling down derived from best fit based on the observed spectrum [46,48]. The specific activity of 68 Ga is considered the same as 68 Ge because the progeny of 68 Ge, 68 Ga has a much shorter half life compared to 68 Ge.…”

Section: Jcap07(2024)009mentioning

confidence: 99%

“…The manufacturing/processing steps of the germanium crystal and detector[43] of CDEX-50, along with those of MJD[45][46][47][48][49]. The unit duration of each manufacturing/processing step is day.…”

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confidence: 99%

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Projected WIMP sensitivity of the CDEX-50 dark matter experiment

Geng,

Yang,

Yue

et al. 2024

J. Cosmol. Astropart. Phys.

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CDEX-50 is a next-generation project of the China Dark Matter Experiment (CDEX) that aims to search for dark matter using a 50-kg germanium detector array. This paper comprises a thorough summary of the CDEX-50 dark matter experiment, including an investigation of potential background sources and the development of a background model. Based on the baseline model, the projected sensitivity of weakly interacting massive particle (WIMP) is also presented. The expected background level within the energy region of interest, set to 2–2.5 keVee, is ∼0.01 counts keVee-1 kg-1 day-1. At 90% confidence level, the expected sensitivity to spin-independent WIMP-nucleon couplings is estimated to reach a cross-section of 5.1 × 10-45 cm2 for a WIMP mass of 5 GeV/c2 with an exposure objective of 150 kg·year and an analysis threshold of 160 eVee. This science goal will correspond to the most sensitive results for WIMPs with a mass of 2.2–8 GeV/c2.

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Section: Cosmogenic Radioactivitymentioning

confidence: 99%

Section: Jcap07(2024)009mentioning

confidence: 99%

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Projected WIMP sensitivity of the CDEX-50 dark matter experiment

Geng,

Yang,

Yue

et al. 2024

J. Cosmol. Astropart. Phys.

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“…In stellar environments, axions could be abundantly produced via the Primakoff process, leading to various interesting astrophysical consequences [6,7]. In particular, solar axions might be detectable in laboratories via the inverse Primakoff process, motivating a number of experimental searches [8][9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

“…[13], is not applicable to massive axions if the mass is significant. 1 Although the axion mass effect JCAP07(2024)013 is negligible in helioscope experiments like CAST which quickly loses sensitivity above a few eV [15], it could be of importance to experiments utilizing crystal [8,[10][11][12] or liquid xenon [16][17][18][19] detectors if the search range extends to keV or higher.…”

Section: Introductionmentioning

confidence: 99%

A comprehensive calculation of the Primakoff process and the solar axion flux

Wu,

2024

J. Cosmol. Astropart. Phys.

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The Primakoff process plays a crucial role in axion production in astrophysical environments and laboratories. Given the rising interest in axion physics and many on-going experimental activities, we conduct a comprehensive calculation of this process and carefully examine several aspects that have been neglected in the literature. In particular, our calculation is valid for axions with significantly large masses, which would be of importance to axion searches utilizing crystal and liquid xenon detectors. We present the most updated calculation of the Primakoff solar axion flux, with a simple parametrization that is applicable to a broad range of axion masses up to a few tens of keV. Our code is publicly available at GitHub.

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Search for solar axions via axion-photon coupling with the Majorana Demonstrator

Cited by 2 publications

References 52 publications

Projected WIMP sensitivity of the CDEX-50 dark matter experiment

Projected WIMP sensitivity of the CDEX-50 dark matter experiment

A comprehensive calculation of the Primakoff process and the solar axion flux

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