PoS(FRAPWS2016)072 http://pos.sissa.it/ † ∗ [email protected] Speaker. This paper was partly supported by the grant GA CR 13-33324S. SMILE is a space mission whichand aims geomagnetic to variations measure with Earth’s global innovative system instrumentation,Lobster–Eye type, responses e.g. on to board. solar wide-field It wind X-ray is telescopenese a Academy of collaborative project of of Sciences. the European TheUniversity Space SMILE in Agency Prague international and and Chi- consortium the involves Czech theX–ray teams Czech telescope. are Technical expected to contribute to the project, mainly to the ∗ † Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Frontier Research in Astrophysics – II 23-28 May 2016 Mondello (Palermo), Italy Branduardi-Raymont, Graziella Mullard Space Science Laboratory, University College London, UK Sembay, Steven University of Leicester, UK René Hudec Czech Technical University in Prague, Faculty ofTechnicka 2, Electrical CZ Engineering, 160 00 Prague,Federation, Czech on Republic, behalf and of Kazan the Federal international University,E-mail: Russian SMILE consortium SMILE ESA CAS Satellite Mission PoS(FRAPWS2016)072 René Hudec 1 SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) is a space mission which aims The key science questions for SMILE [1][2][3][11] are: What are the fundamental modes of to measure Earth’s global systemSMILE will responses investigate to the solar dynamicsolar wind response wind and of in geomagnetic a the variations unique Earth’sEarth’s manner, [1][2][3]. magnetosphere magnetopause never to attempted and the before: magnetospheric impact it cuspsaurora. of will with combine the simultaneous For soft UV the X-ray imaging imaging first ofin of time the the the we Northern magnetosphere will with be thoseeventually able acting the to on aurora. trace the and charged SMILEand link particles will magnetosheath the precipitating conditions, also processes into so carry of the thatand solar in-situ cusps the contrasted wind instrumentation and simultaneous directly, injection to X-ray and monitor and self-sufficiently,parallelled the UV with payload solar images SMILE the will wind can upstream provide be driving answersrelationships compared to conditions. in a many thoroughly of With novel the its way. openEuropean SMILE un- questions Space was in Agency put solar-terrestrial and forward Chinese in Academy Marchmission. of 2015 Sciences in Out (CAS) response of joint to call the 13 for missionsphase a during originally small-size the proposed, space summer SMILE of wasand 2015. the CAS one An at chosen their initial Concurrent for study Design anmission of Facilities is initial the during feasible, study whole October with mission 2015, no was and showby stoppers. carried the the out conclusion In ESA early is by November Science that ESA 2015 the Programme SMILEreaching Committee. was mission formally adoption We selected are in early now 2018. in Launch Phase is A expected study, to with take the place objective at2. of the end Science of with 2021. SMILE the dayside solar wind/magnetosphereCoronal interaction? Mass Ejections What (CME) definesSMILE driven the storms will substorm arise determine cycle? and when whatnates. and How is Dayside where do reconnection their transient causes relationship plasma and to toaries, steady flow substorms? the antisunward magnetopause cusps, through reconnection the and magnetopause domi- overand bound- the patchy. polar It is caps. unclear whether Reconnectiongas steady can to reconnection magnetic persist occurs pressure) for when is long the low plasma (whendominates), periods, the beta–factor or and incoming (ratio be Interplanetary of whether Magnetic bursty unsteady Field (IMF)plasma reconnection pressure beta happens conditions. when SMILE will the testover converse this time is hypothesis of by true, the determining during magnetopause the boundary.extent location high and SMILE in evolution will longitude also and measure theused the proton to proton determine cusp cusp whether spot spot the latitude, intensity. magnetopauseX-line has Measurements (the experienced of compression, region spatially the over constrain protonbursty the which cusp reconnection has magnetic will happened. be reconnection The occurs)Southward trigger turnings and that leads of determine to the whether substorm Interplanetarymagnetotail onset steady Magnetic remains lobes. Field or controversial. However, (IMF) the are precisethis nature required of to precedes how add a the energy period energy to of isstorm the loaded enhanced may into geomagnetic start the activity after tails is the and an magnetotail how is area squeezed of by much an controversy. increase A in sub- solar wind dynamic pressure. SMILE 1. Introduction PoS(FRAPWS2016)072 René Hudec 2 : a wide field of view optic sensitive to the Lyman-Birge-Hopffman band of ultraviolet : a wide field of view proton and alpha particle analyser. This will determine the basic : a telescope with a wide field of view Lobster–eye X–ray optic based on microchannel UVI LIA The following instrumentation makes up the payloadSXI of the SMILE satellite[1][2][3][11] . moments of the solarflux wind vector. ion distributions, These such measurements,the as taken concerns velocity, simultaneously of density, with arrival temperature the times andLangrangian UV and the Point and spatial heat L1 extents X-ray are when images, used. externalcentral obviate solar plane The wind of LIA monitors the will at fieldaverage of the include plasma view distant a sheet will top-hat-type flow be electrostatic directions parallelbe analyser. remain to obtained within the using The the a ecliptic, field variable to geometric ofChinese ensure factor Academy view. that system. of the Larger Sciences, PI: solar dynamic China. Lei wind range Dai, and National will Space Science Center, plate and CCD detector atof the the focal dayside magnetospheric plane. boundaries. Theexchange X-rays interaction SXI in between will ions the in Earth’s observe the exopshere solar the resultPI: wind location, and from Steve neutrals Sembay, shape the such University and charge as of hydrogen motion Leicester, in UK. the exosphere. radiation. Filters and coatings willcap, be and used measure to the suppress location daycalised and glow. brightenings width that The of occur UVI the on will the auroral observeCanada. auroral oval. the oval It polar edges. will PI: Eric also Donovan, observe University transient of and Calgary, lo- 3. Payload SMILE Alternatively, a northward turning of theobserved IMF with may no trigger obvious a external substorm. drivers.will Some SMILE monitor substorms will the have track loading been the of evolution energyand of at the a the subsequent substorm. dayside changes magnetopause SMILE in throughalso the the test size response whether of other of the modes the of open cusps vection magnetospheric field behaviours, (when line such the region as Steady of size Magnetospheric the ofevents Con- polar (a the cap. fast open-flux expansion SMILE region and will ofas contraction the substorms, of but polar the under cap open different cap), does externaland driving are not evolution conditions. manifestations change) of SMILE of and will the the Saw-tooth follow same CME-drivenciated the process storms. with development CME-driven The storms, largest andinfrastructure. they geomagnetic present SMILE disturbances the will are largest determine oftenstorms. space-weather whether asso- threat these SMILE to CME-driven will world-wide storms alsowhy are does consider a a the sequence substorm questions: of stop?mangetotail sub- Does how have this been long happen exhausted? does when a Orsolar the wind? does substorm reserves A a of last, combination substorm stored of and conditions magnetic stop mayand how energy when be therefore and in required changes the for the occur relative the importance complete in of cessationquestions the of each using upstream a factor its substorm, must novel be approach considered. ofditions. simultaneously: SMILE will Measuring Determining answer the the input these solar location windglobal and driving nature shape con- and of properties the of the magnetospheric auroral boundaries. oval. Determining the PoS(FRAPWS2016)072 René Hudec 3 SMILE palyload module. SMILE Soft X-ray Imager (SXI). Figure 1: Figure 2: : a dual-redundant digital fluxgate magnetometer, with two tri-axial fluxgate sensors Charge exchange emission can occur when ions interact with neutral atoms or molecules; one X-ray emission from Solar Wind Charge Exchange (SWCX) recombination occurs in plane- MAG or more electrons are transferred toion the ion (with into the an charge excited now state. reducedbe In by emitted. the the subsequent number relaxation of of electrons the captured), a cascade of photonstary may atmospheres, comets, interplanetary space,extrasolar charge and exchange emission in has the been observed Earth’s in exosphere, supernova remnants, while galaxies and evidence galaxy for 4. Solar Wind Charge Exchange (SWCX) connected by a boom to aconsists spacecraft-mounted of electronics box. a The FPGA accompanying digitalScience electronics Center, processing unit Chinese unit Academy with of Sciences, a China. DC-DC converter. PI: Lei Li, National Space SMILE PoS(FRAPWS2016)072 René Hudec 4 relationships. Geophysical Research Abstracts Vol. 19, EGU2017-8153, 2017. Link Explorer): X-ray imaging of theProceedings Sun-Earth of connection, the in Conference XMM-Newton: held 9-11 Thehttp://www.cosmos.esa.int/web/xmm-newton/2016-workshop, id.81. May, Next 2016 Decade, at ESAC, Madrid. Online at SWCX emission could be used to image the Earth’s magnetosheath. The magnetosheath is the CTU in Prague and Rene Hudec are the SMILE project consortium members.Expected Czech contribution The is Czech as follows: SXI with emphasis on focal plane detector system The SMILE satellite with innovative instrumentation onboard including a Lobster Eye X-ray Acknowledgments We acknowledge partial support by the grant GA CR 13-33324S. [1] http://www.mssl.ucl.ac.uk/SMILE/ [2] Graziella Branduardi-Raymont et al., SMILE: A new approach to exploring solar-terrestrial [3] Branduardi-Raymont, G.; Wang, C.; Smile Team. SMILE (Solar wind Magnetosphere Ionosphere area near the Earth where thethe magnetic Earth’s field, magnetic embedded in field. thewhich solar This protects wind results the plasma, in Earth is from the confronted the by magnetosphere;not harsh static a conditions as cavity within the the of Earth solar Earth-confined system wind. responds plasma This quickly picture, to however, changes is in the solar wind5. density and Czech velocity. Participation participation is based on veryCzech long Republic experience with with emphasis imaging on X wide ray field telescopes X ray and monitors monitors Lobster in Eye(temperature the type control, [4–10]. active/passive coolingmechanics etc.), and thermal electronics. control There system, ismeetings optics expected were participation thermal held of in baffle, Czech Prague, space2015 namely industry. with SMILE Two session SMILE presentations at of Praguemeeting AXRO SMILE in conference Prague PIs in in July negotiating December 2016. details on Czech participation, and6. SMILE Conclusions telescope will study X-rays from theX-ray magnetosphere: astrophysical SMILE will observatories turn in "unwanted to background"trace for a and diagnostic link tool processes ofon Sun-Earth of relationships. charged solar particles wind SMILE precipitating injection will intoas in well: the the SMILE cusps Earth’s images and magnetosphere andfar the with videos invisible. aurora. will those The captivate acting There project public is to willDouble science based Star be (that on experience. outreach of cooperation aspects the with magnetic China: field) SMILE so is a showcase, building on References SMILE clusters. Consequently, the heliophysics, planetary science,an and interest astrophysics in communities SWCX. all have PoS(FRAPWS2016)072 René Hudec 5 2004); doi: 10.1117/12.551915, 2004 in Exploring the Cosmic Frontier, ESOpp.73-74, Astrophysics 2007 Symposia European Southern Observatory 2007, [4] Hudec, R., et al., Proc. SPIE 5488, UV and Gamma-Ray Space[5] Telescope Systems, (11Hudec, October R., Pína, L., Inneman, A., Švéda, L., LOBSTER - Astrophysics with Lobster Eye Telescopes, [6] Inneman, A., et al., 2000, Proc.[7] SPIE, 4138,Hudec, 94 R., et al., 2000, SPIE[8] Proc. 4012,Hudec, 432 R., et al., 2003, SPIE[9] Proc. 4851,Hudec, 578 R., et al., 2004a, SPIE Proc. 5488, 449 SMILE [10] Hudec, R., et al., 2004b, Nucl.[11] Phys. BRaab Proc. W. Suppl. et 132, al., 320 2016, Proceedings of the SPIE, Volume 9905, id. 990502 9