\u30e1\u30bf\u968e\u5c64\u30c0\u30a4\u30ca\u30df\u30af\u30b9\u30e6\u30cb\u30c3\u30c8\u30bb\u30df\u30ca\u30fc\u3092\u958b\u50ac\u3057\u307e\u3059\u3002\u7686\u69d8\u306e\u3054\u53c2\u52a0\u3092\u304a\u5f85\u3061\u3057\u3066\u304a\u308a\u307e\u3059\u3002<\/p>\n\n\n\n
\u65e5\u6642\uff1a2026\u5e742\u670824\u65e5\uff08\u706b\uff0914:00-16:00<\/p>\n\n\n\n
\u5834\u6240\uff1a\u6838\u878d\u5408\u79d1\u5b66\u7814\u7a76\u6240 \u7814\u7a76\u2160\u671f\u68df\uff18\u968e\uff18\uff10\uff11\u4f1a\u8b70\u5ba4\uff08\u30cf\u30a4\u30d6\u30ea\u30c3\u30c9\u958b\u50ac\uff09<\/p>\n\n\n\n
\u8b1b\u6f14\u8005\uff1aDr. Patrick Antolin (Northumbria Univ.)<\/p>\n\n\n\n
\u984c\u76ee\uff1aThe Delicate Mass and Energy Balance of the Solar Atmosphere<\/p>\n\n\n\n
\u6982\u8981\uff1a<\/p>\n\n\n\n
Cool plasmas (mostly at 10^4 K or less) at the interface or embedded in a larger, much hotter (10^6 K or
higher) medium are ubiquitous in different astrophysical systems such as solar and stellar atmospheres, the circumgalactic (CGM), interstellar (ISM) and intra-cluster (ICM) media. Known as cool multiphase plasma, its role has been highlighted in mass and energy cycles at all such scales, from the chromosphere-corona interface and feedback cycles in quiescent and flaring regimes in the solar atmosphere to precipitation-regulated feedback cycles that drive star and galaxy formation. The properties of multiphase plasma across these multiple scales are strikingly similar, intimately linked to the yet unclear but fundamental mechanisms of the heating and flaring, and thermal and dynamic instabilities linked to mixing and cooling. Being so close and governed by small timescales, the solar corona constitutes a formidable physics and astrophysics laboratory where we can spatially and temporally resolve the physics of the production and removal of such multiphase plasma, thus providing a testbed for theories in multiple disciplines that apply in extreme conditions. Increasing theoretical, observational, and numerical work suggests that a significant fraction of the solar atmosphere is in a state of thermal non-equilibrium (TNE) and thermal instability (TI). This TNE-TI state manifests, in particular, with the formation of prominences and pervasive coronal rain. The presence of this cool and dense, partially ionised phenomena is intimately linked to the spatial and temporal properties of how the enigmatic coronal heating and flaring mechanisms operate. In this talk I will review recent observational and numerical advances in our understanding of multiphase plasma on the Sun, and particularly coronal rain. I will discuss the major open questions in the field linked to the formation of coronal rain, its mysterious morphology, kinematics and thermodynamics, while making interesting analogies to multiphase plasmas at the much larger scales of the ISM, CGM and ICM.<\/p>\n\n\n\n
\u9023\u7d61\u5148\uff1a\u77f3\u5ddd\u907c\u592a\u90ce\uff08\u30e1\u30bf\u968e\u5c64\u30c0\u30a4\u30ca\u30df\u30af\u30b9\u30e6\u30cb\u30c3\u30c8\uff09\u3000ishikawa.ryohtaro(at)nifs.ac.jp<\/p>\n\n\n\n
\u203b(at) \u3092\uff20\u306b\u76f4\u3057\u3066\u304f\u3060\u3055\u3044\u3002<\/p>\n\n\n\n