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Selected events (\u224830,000 on each component) typically have much greater amplitude on the\n                    <jats:italic>H<\/jats:italic>\n                    component with respect to\n                    <jats:italic>D<\/jats:italic>\n                    . They often reveal two prominent spectral peaks, one in band\n                    <jats:italic>A<\/jats:italic>\n                    (\n                    <jats:italic>f\u2009&lt;<\/jats:italic>\n                    \u2009\u2248\u200945\u2009mHz), mostly related to the transmission of upstream waves, and the other one in band\n                    <jats:italic>B<\/jats:italic>\n                    (\n                    <jats:italic>f\u2009&gt;<\/jats:italic>\n                    \u2009\u2248\u200955\u2009mHz), including resonances of local field lines and higher\u2010frequency upstream waves. The occurrence of resonant phenomena on the\n                    <jats:italic>D<\/jats:italic>\n                    component is also clearly evidenced. The solar wind speed is confirmed as the key element for the manifestation of events; by contrast, their appearance is inhibited during extremely low solar wind densities. The events mostly manifest between dawn and early afternoon, with highest occurrence at \u224808:00\u201310:00 LT, as might be expected for the usual distribution of the interplanetary magnetic field orientation determining more or less favorable conditions for a foreshock region on the morning flank of the bow shock. No evidence is found for a favorite occurrence for low cone angles (\n                    <jats:italic>\u03b8<\/jats:italic>\n                    <jats:sub>XB<\/jats:sub>\n                    \u2009&lt;\u2009\u2248\u200910\u00b0); rather, they preferentially manifest for\n                    <jats:italic>\u03b8<\/jats:italic>\n                    <jats:sub>XB<\/jats:sub>\n                    \u2009\u2248\u200925\u00b0\u201340\u00b0. The polarization pattern, much more definite in the afternoon, is consistent with the expected antisunward propagation; in the morning sector, it also suggests the possible occurrence of sunward propagating modes, mostly at\n                    <jats:italic>f<\/jats:italic>\n                    \u2009&lt;\u2009\u2248\u200922\u2009mHz. The tilt angle of the major axis of the polarization ellipses during daytime hours is oriented in the NW\/SE quadrant and experiences remarkable changes at sunrise and sunset; it also shows a seasonal modulation with larger angles in the winter.\n                  <\/jats:p>","DOI":"10.1002\/2014ja020558","type":"journal-article","created":{"date-parts":[[2015,2,16]],"date-time":"2015-02-16T16:34:59Z","timestamp":1424104499000},"page":"1784-1802","source":"Crossref","is-referenced-by-count":2,"title":["A comprehensive analysis of the occurrence and characteristics of midperiod ULF waves at low latitude"],"prefix":"10.1029","volume":"120","author":[{"given":"Umberto","family":"Villante","sequence":"first","affiliation":[{"name":"Dipartimento di Ingegneria e Scienze dell'Informazione e Matematica Universit\u00e1  L'Aquila Italy"},{"name":"Area di Ricerca in Astrogeofisica  L'Aquila Italy"}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"Pietro","family":"Tiberi","sequence":"additional","affiliation":[{"name":"Area di Ricerca in Astrogeofisica  L'Aquila Italy"}],"role":[{"role":"author","vocabulary":"crossref"}]}],"member":"13","published-online":{"date-parts":[[2015,3,14]]},"reference":[{"key":"e_1_2_10_2_1","doi-asserted-by":"publisher","DOI":"10.1002\/2013JA019637"},{"key":"e_1_2_10_3_1","doi-asserted-by":"publisher","DOI":"10.1029\/93JA02905"},{"key":"e_1_2_10_4_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA079i007p01024"},{"key":"e_1_2_10_5_1","doi-asserted-by":"publisher","DOI":"10.1029\/96JA00139"},{"key":"e_1_2_10_6_1","doi-asserted-by":"publisher","DOI":"10.1134\/S0016793206010075"},{"key":"e_1_2_10_7_1","doi-asserted-by":"publisher","DOI":"10.1029\/2010JA015967"},{"key":"e_1_2_10_8_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA091iA08p08909"},{"key":"e_1_2_10_9_1","doi-asserted-by":"publisher","DOI":"10.1029\/90JA02101"},{"key":"e_1_2_10_10_1","doi-asserted-by":"publisher","DOI":"10.1029\/95JA00768"},{"key":"e_1_2_10_11_1","doi-asserted-by":"publisher","DOI":"10.1029\/JZ072i011p02871"},{"key":"e_1_2_10_12_1","doi-asserted-by":"publisher","DOI":"10.1016\/j.pss.2013.03.008"},{"key":"e_1_2_10_13_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA079i031p04632"},{"key":"e_1_2_10_14_1","doi-asserted-by":"publisher","DOI":"10.1016\/0032-0633(76)90064-7"},{"key":"e_1_2_10_15_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA084iA02p00527"},{"key":"e_1_2_10_16_1","doi-asserted-by":"publisher","DOI":"10.1029\/GL010i008p00659"},{"key":"e_1_2_10_17_1","doi-asserted-by":"publisher","DOI":"10.1029\/GL010i008p00765"},{"key":"e_1_2_10_18_1","doi-asserted-by":"publisher","DOI":"10.5194\/angeo-28-1703-2010"},{"key":"e_1_2_10_19_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA088iA03p02021"},{"key":"e_1_2_10_20_1","doi-asserted-by":"publisher","DOI":"10.1029\/2004JA010417"},{"key":"e_1_2_10_21_1","doi-asserted-by":"publisher","DOI":"10.1029\/JA081i019p03241"},{"key":"e_1_2_10_22_1","first-page":"1018","article-title":"Numerical simulations on ionospheric control of polarization of low\u2010latitude geomagnetic pulsations","volume":"11","author":"Itonaga M.","year":"1993","journal-title":"Ann. 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