Presentazione

Full-3D relativistic MHD simulations of bow shock pulsar wind nebulae: dynamics

“…They have been mainly revealed as non-thermal radio and X-ray emission (Arzoumanian et al 2004;Gaensler et al 2004;Yusef-Zadeh & Gaensler 2005;Li et al 2005;Gaensler 2005;Chatterjee et al 2005;Kargaltsev et al 2008;Misanovic et al 2008;Ng et al 2009;Hales et al 2009;Ng et al 2010;De Luca et al 2011;Ng et al 2012;Marelli et al 2013;Jakobsen et al 2014;Auchettl et al 2015;Posselt et al 2017), with polarimetric informations only available for a few cases, suggesting a large variety of magnetic configurations (Ng et al 2012;Yusef-Zadeh & Gaensler 2005;Ng et al 2010;Kargaltsev et al 2017). Extended TeV halos have also been recently detected surrounding some BSPWNe (Abeysekara 2017), attracting much attention because these nebulae are thought to be one of the major contributors of leptonic anti-matter in the Galaxy, in competition with possible dark matter sources (Blasi & Amato 2011;Amato & Blasi 2017). If the pulsar is moving through a partially ionized medium the collisional and/or charge exchange excitations of neutral hydrogen atoms in the tail can also allow one to reveal the BSPWN as H α emission (Chevalier et al 1980;Kulkarni & Hester 1988;Cordes et al 1993;Bell et al 1995;van Kerkwijk & Kulkarni 2001;Jones et al 2002;Browns-berger & Romani 2014;Romani et al 2017), or alternatively in the UV , and IR (Wang et al 2013).…”