Triboelectric Backgrounds to radio-based UHE Neutrino Exeperiments. (arXiv:2103.06079v2 [astro-ph.IM] UPDATED)

Triboelectric Backgrounds to radio-based UHE Neutrino Exeperiments. (arXiv:2103.06079v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_J/0/1/0/all/0/1">J. A. Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anker_A/0/1/0/all/0/1">A. Anker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allison_P/0/1/0/all/0/1">P. Allison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Archambault_S/0/1/0/all/0/1">S. Archambault</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldi_P/0/1/0/all/0/1">P. Baldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barwick_S/0/1/0/all/0/1">S. W. Barwick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beatty_J/0/1/0/all/0/1">J. J. Beatty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beise_J/0/1/0/all/0/1">J. Beise</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Besson_D/0/1/0/all/0/1">D. Besson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bishop_A/0/1/0/all/0/1">A. Bishop</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bondarev_E/0/1/0/all/0/1">E. Bondarev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botner_O/0/1/0/all/0/1">O. Botner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouma_S/0/1/0/all/0/1">S. Bouma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buitink_S/0/1/0/all/0/1">S. Buitink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cataldo_M/0/1/0/all/0/1">M. Cataldo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C.C. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C.H. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_P/0/1/0/all/0/1">P. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Y.C. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_B/0/1/0/all/0/1">B. A. Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clay_W/0/1/0/all/0/1">W. Clay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Curtis_Ginsberg_Z/0/1/0/all/0/1">Z. Curtis-Ginsberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connolly_A/0/1/0/all/0/1">A. Connolly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dasgupta_P/0/1/0/all/0/1">P. Dasgupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kockere_S/0/1/0/all/0/1">S. de Kockere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vries_K/0/1/0/all/0/1">K. D. de Vries</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deaconu_C/0/1/0/all/0/1">C. Deaconu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DuVernois_M/0/1/0/all/0/1">M. A. DuVernois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaherty_J/0/1/0/all/0/1">J. Flaherty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Friedman_E/0/1/0/all/0/1">E. Friedman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaior_R/0/1/0/all/0/1">R. Gaior</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaswint_G/0/1/0/all/0/1">G. Gaswint</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glaser_C/0/1/0/all/0/1">C. Glaser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallgren_A/0/1/0/all/0/1">A. Hallgren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallmann_S/0/1/0/all/0/1">S. Hallmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanson_J/0/1/0/all/0/1">J. C. Hanson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harty_N/0/1/0/all/0/1">N. Harty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hendricks_B/0/1/0/all/0/1">B. Hendricks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoffman_K/0/1/0/all/0/1">K. D. Hoffman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hornhuber_C/0/1/0/all/0/1">C. Hornhuber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsu_S/0/1/0/all/0/1">S.Y. Hsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_L/0/1/0/all/0/1">L. Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">J.J. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_M/0/1/0/all/0/1">M.-H. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_K/0/1/0/all/0/1">K. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishihara_A/0/1/0/all/0/1">A. Ishihara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karle_A/0/1/0/all/0/1">A. Karle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelley_J/0/1/0/all/0/1">J. L. Kelley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_S/0/1/0/all/0/1">S. R. Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleinfelder_S/0/1/0/all/0/1">S. A. Kleinfelder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_K/0/1/0/all/0/1">K.-C. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_M/0/1/0/all/0/1">M.-C. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kravchenko_I/0/1/0/all/0/1">I. Kravchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krebs_R/0/1/0/all/0/1">R. Krebs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ku_Y/0/1/0/all/0/1">Y. Ku</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuo_C/0/1/0/all/0/1">C. Y. Kuo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurusu_K/0/1/0/all/0/1">K. Kurusu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lahmann_R/0/1/0/all/0/1">R. Lahmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landsman_H/0/1/0/all/0/1">H. Landsman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latif_U/0/1/0/all/0/1">U. Latif</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">C.-J. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_J/0/1/0/all/0/1">J. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_T/0/1/0/all/0/1">T.-C. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_M/0/1/0/all/0/1">M.-Y. Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madison_K/0/1/0/all/0/1">K. Madison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mammo_J/0/1/0/all/0/1">J. Mammo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mase_K/0/1/0/all/0/1">K. Mase</a>, et al. (50 additional authors not shown)

The proposed IceCube-Gen2 (ICG2) seeks to instrument ~500 sq. km of Antarctic
ice near the geographic South Pole with radio antennas, in order to observe the
highest energy (E>1 EeV) neutrinos in the Universe. To this end, ICG2 will use
the impulsive radio-frequency (RF) signal produced by neutrino interactions in
polar ice caps. In such experiments, rare single event candidates must be
unambiguously separated from background; to date, signal identification
strategies primarily reject thermal noise and anthropogenic backgrounds. Here,
we consider the possibility that fake neutrino signals may also be naturally
generated via the ‘triboelectric effect’. This broadly includes any process in
which force applied at a boundary layer results in displacement of surface
charge, generating a potential difference {Delta}V. Wind blowing over granular
surfaces such as snow can induce such a {Delta}V, with subsequent discharge.
Discharges over nanosecond-timescales can then lead to RF emissions at
characteristic MHz-GHz frequencies. We find that such backgrounds are evident
in the several neutrino experiments considered, and are generally characterized
by: a) a threshold wind velocity which likely depends on the experimental
signal trigger threshold and layout; for the experiments considered herein,
this value is typically O(10 m/s), b) frequency spectra generally shifted to
the low-end of the frequency regime to which current radio experiments are
typically sensitive (100-200 MHz), c) for the strongest background signals, an
apparent preference for discharges from above-surface structures, although the
presence of more isotropic, lower amplitude triboelectric discharges cannot be
excluded.

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