The magnetosheath at high spectral resolution  

作　　者：K.D.Küntz D.Koutroumpa W.R.Dunn A.Foster F.S.Porter D.G.Sibeck B.Walsh 

机构地区：[1]The Henry A.Rowland Department of Physics and Astronomy,Johns Hopkins University,3701 San Martin Drive,Baltimore,MD,21218,USA [2]NASA Goddard Space Flight Center,8800 Greenbelt Road,Greenbelt,MD 20771,USA [3]LATMOS-OVSQ,CNRS,UVSQ Paris-Saclay,Sorbonne Université,11 Boulevard d’Alembert,78280,Guyancourt,France [4]Department of Physics and Astronomy,University College London,London,UK [5]The Centre for Planetary Science at UCL/Birkbeck,Gower Street,London WC1E 6BT,UK [6]Center for Astrophysics,Harvard University&Smithsonian Institution,60 Garden Street,Cambridge,MA 02138,USA [7]Center for Space Physics,Boston University,110 Cummington Mall,Boston,MA,USA

出　　处：《Earth and Planetary Physics》2024年第1期234-246,共13页地球与行星物理（英文版）

基　　金：financial support from CNES via its Sun-Heliosphere-Magnetosphere(SHM)program;support from NASA grant#80NSSC20K1709。

摘　　要：While we eagerly anticipate SMILE’s(Solar wind Magnetosphere Ionosphere Link Explorer)unprecedented X-ray observations of the Earth’s magnetosheath and the initiation of a new era of magnetospheric research,it seems appropriate to look ahead to the abilities of the next generation of astrophysics missions.Of these,the Line Emission Mapper(LEM),a large aperture micro-calorimeter based mission,is currently planned to be able to observe the magnetosheath at high spectral resolution(~2 eV).With a field of view of~30′,LEM will allow higher spatial resolution and higher cadence measurement of the motion of a very small portion of the magnetopause over relatively short periods of time(multiple hours),complementing SMILE’s global mapping.LEM’s strength is its spectral resolution.It will be able to measure the abundance of a broad range of elements and ionization states,many of which are inaccessible to current in situ instruments,and will be able to separate the emission from the magnetosheath from the emission from the cosmic X-ray background using the difference in their relative velocities.

关 键 词：MAGNETOSHEATH charge exchange solar wind abundances 

分 类 号：P353[天文地球—空间物理学]