PRIDE (Passive Radio [frequency] Ice Depth Experiment): An instrument to passively measure ice depth from a Europan orbiter using neutrinos

Abstract

a b s t r a c tWe describe a concept for an instrument to measure the thickness of the ice shell on a planetary body such as Jupiter's moon Europa. Unlike a high powered and massive device such as an ice-penetrating radar, the instrument would be a passive receiver of a naturally occurring signal generated by interactions of deep penetrating cosmic ray neutrinos. We discuss the basic concept and consider the instrument design requirements from the perspective of a NASA Outer Planet Orbiter Mission. We show results of simulations, compare signal-to-noise estimates, and examine possible components and configurations for the antenna, receiver, and electronics. We note some options that can be used to reduce mass and power. Finally, we present a list of issues that would need further study to produce a more concrete design.

Heavy decaying dark matter at future neutrino radio telescopes

“…These include several planned experiments, e.g. ARIANNA [34], ARA [35], TAMBO [36,37], POEMMA [38], JEM-EUSO [39], RNO-G [40], GRAND [41] and IceCube-Gen2 radio array [42,43]. Their primary aim is the determination of the neutrino sources in this ultra-high energy range, and in particular the detection of the so-called cosmogenic neutrinos [44].…”

Heavy decaying dark matter at future neutrino radio telescopes

“…These include several planned experiments, e.g. ARIANNA [33], ARA [34], POEMMA [35], JEM-EUSO [36], RNO-G [37], GRAND [38] and IceCube-Gen2 radio array [39,40]. Their primary aim is the determination of the neutrino sources in this ultra-high energy range, and in particular the detection of the so-called cosmogenic neutrinos [41].…”

Radio Detection of High Energy Neutrinos

“…The PRIDE experiment is even exploring other worlds as possible detection media, such as Enceladus or Europa, icy moons of Saturn and Jupiter, respectively. 50 Detectors on the ground or embedded in their detection medium, such as the Askaryan Radio Array (ARA) and The Antarctic Ross Ice Shelf Antenna Neutrino Array (ARIANNA), which sit in and on glacial ice, have a lower energy threshold than ones that are situated farther from the interactions. In addition, the livetime can be much longer for an embedded experiment compared to a balloon experiment (years compared to several weeks).…”