Prospects for detecting ultra-high-energy particles with FAST

被引：7
作者：
James, Clancy W. [1 ,2 ]
Bray, Justin D. [3 ]
Ekers, Ronald D. [4 ]
机构：
[1] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia
[2] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia
[3] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England
[4] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia
来源：
RESEARCH IN ASTRONOMY AND ASTROPHYSICS | 2019年 / 19卷 / 02期
关键词：
cosmic rays; neutrinos; techniques: miscellaneous; Moon; COSMIC-RAYS; UHE NEUTRINOS; SEARCH; EMISSION; SHOWERS; CHARGE; LIMITS;
D O I：
10.1088/1674-4527/19/2/19
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The origin of the highest-energy particles in nature, ultra-high-energy (UIIE) cosmic rays, is still unknown. In order to resolve this mystery, very large detectors are required to probe the low flux of these particles - or to detect the as-yet unobserved flux of UHE neutrinos predicted from their interactions. The `lunar Askaryan technique' is a method to do both. When energetic particles interact in a dense medium, the Askaryan effect produces intense coherent pulses of radiation in the MHz-GHz range. By using radio telescopes to observe the Moon and look for nanosecond pulses, the entire visible lunar surface (20 million km(2)) can be used as a UHE particle detector. A large effective area over a broad bandwidth is the primary telescope requirement for lunar observations, which makes large single-aperture instruments such as the Five-hundred-meter Aperture Spherical radio Telescope (FAST) well-suited to the technique. In this contribution, we describe the lunar Askaryan technique and its unique observational requirements. Estimates of the sensitivity of FAST to both the UHE cosmic ray and neutrino flux are given, and we describe the methods by which lunar observations with FAST, particularly if equipped with a broadband phased-array feed, could detect the flux of UHE cosmic rays.
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页数：14
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