太陽射電爆發(fā)參數(shù)與日冕動力學(xué)過程2025/2/202提綱太陽物理前沿問題及太陽射電天文學(xué)的優(yōu)勢太陽射電爆發(fā)類型劃分日冕動力學(xué)及太陽射電爆發(fā)參數(shù)提取總結(jié)2025/2/2031.太陽物理前沿問題及太陽射電天文學(xué)的優(yōu)勢太陽物理前沿問題CoronalheatingprocessesNatureofsolareruptionsOriginofsolarcyclesInteriorstructureoftheSun2025/2/204太陽射電天文學(xué)的優(yōu)勢射電觀測對太陽大氣中的各種非熱過程、粒子加速和傳播、等離子體不穩(wěn)定性活動等都有非常靈敏的響應(yīng)射電觀測可以用毫秒級的時間分辨率對太陽爆發(fā)過程進(jìn)行快速頻譜和成像觀測射電探測：空間范圍廣、動態(tài)范圍大、對爆發(fā)活動靈敏度高RadioemissionintensityofSunandMilkyWay30GHz3.0GHz300MHz30MHz3MHz300kHz射電探測：能對幾乎所有太陽物理前沿問題給出新的觀測證據(jù)2025/2/205太陽射電天文學(xué)的復(fù)雜性多種輻射機(jī)制共存非相干輻射

韌致輻射回旋共振輻射回旋加速輻射同步加速輻射相干輻射電子回旋脈澤輻射等離子體輻射2025/2/206太陽射電流量計單天線、在單一頻段或少數(shù)幾個頻點上測量太陽輻射流量?？色@得極高的靈敏度和時間分辨率。如懷柔2840流量計、日本NoRP偏振計（7個頻段）等太陽射電觀測手段每日數(shù)據(jù)量較小，大約幾MB到幾十MB2025/2/207太陽射電頻譜儀單天線、在寬帶多頻點觀測，可得到寬帶動態(tài)頻譜圖，有較高的時間分辨率和頻率分辨率。如懷柔的SBRS/Huairou,捷克ORSC/Ondrejov等SBRS/Huairou每日數(shù)據(jù)量可達(dá)幾百MB到幾個GB量級2025/2/208單頻射電日像儀在單一頻點或少數(shù)幾個頻點上進(jìn)行全日面成像觀測，如日本NoRH(17、34GHz)、法國Nancay(150-500MHz，10個頻點)等。每日數(shù)據(jù)量可達(dá)幾十到幾百GBNoRHiscomposedof84antennawithdiameter80cminT-shapearray.Itsspatialresolutionis10?withcadenceof1sand50ms.NoRH2025/2/209射電頻譜日像儀用許多望遠(yuǎn)鏡組成干涉陣列，利用合成孔徑成像技術(shù)，可以同時獲得較高的時間-空間-頻率分辨率。MUSER2014-11-11eventobservedbyMUSER每日觀測數(shù)據(jù)量非常巨大，可達(dá)幾百GB到若干TB左右，MUSER,etc.2025/2/2010太陽射電流量計太陽射電頻譜儀單頻射電日像儀射電頻譜日像儀每日數(shù)據(jù)量：1-100MB每日數(shù)據(jù)量：300MB-10GB每日數(shù)據(jù)量：1-100GB每日數(shù)據(jù)量：2-6TB隨著探測能力的不斷提高，積累的觀測數(shù)據(jù)也呈指數(shù)地迅速增加如何從海量觀測數(shù)據(jù)中提取有價值的信息，是太陽物理研究的重要任務(wù)2025/2/20112.太陽射電爆發(fā)的類型劃分太陽射電輻射包含非常豐富的太陽爆發(fā)過程的信息:

熱過程

非熱過程

粒子加速及相關(guān)傳播和能量釋放

等離子體不穩(wěn)定性(相干過程及非相干過程)

輻射源區(qū)的磁場信息太陽射電爆發(fā)的時標(biāo)跨越從毫秒級到幾個小時的很寬的范圍，其源區(qū)空間尺度也大到整個活動區(qū)、小到亞角秒量級對不同類型太陽射電爆發(fā)的準(zhǔn)確描述是我們理解相應(yīng)日冕動力學(xué)過程的基礎(chǔ)2025/2/2012(1)TypeIstorm/bursts(Iwai,etal.ApJ,2014)<300MHz,enhancedbroadbandcontinuum(TypeIstorm),overlappedwithshort-life,narrowbandstrongbursts(TypeIbursts)2025/2/2013(2)TypeIIbursts(Du,etal.,ApJ,2015)Thefrequencydriftrate:Frequencydriftsslowly,alwayshaveharmonicstructures,associatedtoCMEorshocks,importantindicatoroffastplasmaflows2025/2/2014(Tan,etal,2016,ApJ)(3)TypeIIIburstsThefrequencydriftrate:TypeIIIburstisasignatureofenergeticelectronbeams,andthetypeIIIpaircanpinpointtheaccelerationsite,andbeaindicatorofmagneticreconnection.Fastfrequencydrifts,rangefromdecametertodecimeterwavelengths.2025/2/2015(4)TypeⅣbursts(Aurass,etal,2003,AA,410,1001)Overlappingmanyfinestructures:QPP,ZP,fiber,narrowtypeIII,spike,dot,etc.Thesefinestructuresrevealcomplexphysicalprocessesinthesourceregions.Broadbandcontinuumbursts,2025/2/2016(5)TypeVburstsObservedbyCulgooraSpectropolarimeter,afteratrainoftypeIIIbursts(Dulk,etal,A&A,1980)2025/2/2017TypefrequencyMainfeaturesMagneticconfigurationPhysicalconditionsEmissionmechanismⅠ<300MHzBroadbandcontinuum,lastforseveralhourstomorethan1day,overlappingmanynarrow,shortburst,strongpolarizationOpenorclosedloopsTrappedelectronsinARPlasmaemissionⅡ1-300MHzSlowfrequencydrift,Harmonicstructure,lastsforseveralor10minOpenfieldShock,CME,JetsPlasmaemissionⅢ(U,J)1MHz–10GHzFastfrequencydrift,Highbrightnesstemperature,shortlifetimeOpenorclosedloopsElectronbeamsPlasmaemissionOrECMEⅣ10MHz–30GHzBroadbandcontinuum,lastsforn–30min.OverlappingspectralfinestructuresClosedloopsTrappednon-thermalparticlesGyro-magneticradiation(?)Ⅴ10–120MHzContinuum,lastsfor1-2min,afterTypeIIIs.WeakpolarizationOpenloops?Plasmaemission(?)各類型射電爆發(fā)的主要特征2025/2/2018Finger-likestructureWeaklypolarization.ZebrapatternstructureWeaklypolarization,stripswithparalleledequidistance.(Huang&Yan,2007,AdSpR)(Chernovetal.,2011,RAA)其他頻譜結(jié)構(gòu)類型2025/2/2019纖維狀爆發(fā)FiberburstThereareseveralsegmentsfiberburstsintheflaredecayphase.df/dt:-58~-73MHz/sCentralfreq:1220MHzPolarization:~100%2025/2/2020窄帶III型爆Narrow-bandTypeIIIburstsduration:~0.6sFreqbandwidth:50~110MHzPolarization:~85%Partofdots:df/dt~3.20~9.60GHz/sPeriodicity:P~20-30ms2025/2/2021尖峰爆發(fā)Spikeburstsduration:~18-25msFreqbandwidth:28–72MHzPolarization:~80%Partofspikes:df/dt:~-2.31~-9.66GHz/sSeveralclustersofspikeburstsdistributeirregularlyinthedecayphase.2025/2/2022點狀爆發(fā)Dotbursts7clustersofdotburstsdistributeirregularlyinthedecayphase.duration:~16-23msFreqbandwidth:24–30MHzPolarization:~90%Partofdots:df/dt~-4.10~-8.60GHz/s2025/2/2023classDuration(s)DR(MHz/s)Δf(MHz)Pol(%)lace4-8-500~75024070-80fiber0.5-2.2-58~-7380-20075-85zebra0.8-1.2-145~-155>24080-90SpikyQPP2-3-3700~-730020080-90TypeIII0.63200~9600110~85spike0.018~0.025-2310~-966028-72~80dot0.016~0.023-4100~-860024-3085~95精細(xì)結(jié)構(gòu)爆發(fā)的統(tǒng)計特征（以2004年12月1日耀斑事件為例）2025/2/2024短周期脈動結(jié)構(gòu)(SPP):0.5<P<10sBandwidth:600-900MHzPeriod:7.5secondsStrongpolarizationDriftingrate:–4.0GHz/sto3.5GHz/s.mostfasterthanthatofVLPandLPP.Thismayimplythattheyarerelatedtosomeenergeticelectrons.2025/2/2025甚短周期脈動結(jié)構(gòu)(VSP):P<0.5sOrdinaryVSP:Wg<2WpExtraordinaryVSP:Wg>>2WpWp:pulsewidth(energyrelease)Wg:gapwidth(energystorage)Narrowband,strongpolarization,fastdrift(Tanetal,2007,ApJ)2025/2/202626微波斑馬紋結(jié)構(gòu)(ZP)

MicrowaveZPisthemostintriguingandcomplexphenomenoninsolarradioastronomy.SBRSobservedmanymicrowaveZPssince1999,includingtheZebraatthehighestfrequency(7GHz)Chen&Yan,SoPh,2007Chernovetal.2011Altyntsevetal.,A&A,2005etc.2025/2/2027魚群結(jié)構(gòu)Moderatefrequencydriftingrate,weaklypolarization,alwaysinpairs.Itsformationmechanismisanopenproblem.Wuetal.(2007,ApJ,665)proposedthatitproducedbyagroupof“solitarykineticAlfvenwaves”(SKAWs)withsmallcross-fieldscales.2025/2/2028(Tan,ApJ,2013)微波小爆發(fā)微波小爆發(fā)（Solarsmall-scalemicrowavebursts，SMBs）包括點狀爆發(fā)、尖峰爆發(fā)、窄帶III型爆發(fā)等，具有壽命短、帶寬窄、強(qiáng)偏振、超高的輻射亮溫等特征，為一類強(qiáng)相干輻射過程需要提取參數(shù)包括：輻射頻率帶寬輻射強(qiáng)度偏振度頻率漂移率時間分布特征