{"id":6683,"date":"2020-01-16T21:01:55","date_gmt":"2020-01-16T21:01:55","guid":{"rendered":"https:\/\/www.istp.cnr.it\/?post_type=product&#038;p=6683"},"modified":"2022-06-21T09:57:12","modified_gmt":"2022-06-21T09:57:12","slug":"evolution-of-turbulence-in-the-kelvin-helmholtz-instability-in-the-terrestrial-magnetopause","status":"publish","type":"product","link":"https:\/\/www.istp.cnr.it\/it\/research-product\/evolution-of-turbulence-in-the-kelvin-helmholtz-instability-in-the-terrestrial-magnetopause\/","title":{"rendered":"Evolution of Turbulence in the Kelvin-Helmholtz Instability in the Terrestrial Magnetopause"},"content":{"rendered":"<p>The dynamics occurring at the terrestrial magnetopause are investigated by using Geotail and THEMIS spacecraft data of magnetopause crossings during ongoing Kelvin-Helmholtz instability. Properties of plasma turbulence and intermittency are presented, with the aim of understanding the evolution of the turbulence as a result of the development of Kelvin-Helmholtz instability. The data have been tested against standard diagnostics for intermittent turbulence, such as the autocorrelation function, the spectral analysis and the scale-dependent statistics of the magnetic field increments. A quasi-periodic modulation of different scaling exponents may exist along the direction of propagation of the Kelvin-Helmholtz waves along the Geocentric Solar Magnetosphere coordinate system (GSM), and it is visible as a quasi-periodic modulation of the scaling exponents we have studied. The wave period associated with such oscillation was estimated to be approximately 6.4 Earth Radii (R-E). Furthermore, the amplitude of such modulation seems to decrease as the measurements are taken further away from the Earth along the magnetopause, in particular after X (GSM) less than or similar to -15 R-E. The observed modulation seems to persist for most of the parameters considered in this analysis. This suggests that a kind of signature related to the development of the Kelvin-Helmholtz instabilities could be present in the statistical properties of the magnetic turbulence.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Di Mare, Francesca; Sorriso-Valvo, Luca; Retino, Alessandro; Malara, Francesco; Hasegawa, Hiroshi<\/p>\n","protected":false},"featured_media":1294,"comment_status":"closed","ping_status":"open","template":"","meta":[],"product_cat":[574],"product_tag":[801,802,1110,1111],"class_list":["post-6683","product","type-product","status-publish","has-post-thumbnail","hentry","product_cat-journal-articles","product_tag-turbulence","product_tag-intermittency","product_tag-magnetosheath","product_tag-kelvin-helmholtz-instability","prodpage-style2"],"acf":[],"_links":{"self":[{"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/product\/6683","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/product"}],"about":[{"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/types\/product"}],"replies":[{"embeddable":true,"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/comments?post=6683"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/media\/1294"}],"wp:attachment":[{"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/media?parent=6683"}],"wp:term":[{"taxonomy":"product_cat","embeddable":true,"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/product_cat?post=6683"},{"taxonomy":"product_tag","embeddable":true,"href":"https:\/\/www.istp.cnr.it\/it\/wp-json\/wp\/v2\/product_tag?post=6683"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}