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VLTIMIDI Observations of the Massive Protostellar Candidate NGC 3603 IRS 9A

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arXiv:0711.4760v1 [astro-ph] 29 Nov 2007**FULLTITLE**ASPConferenceSeries,Vol.**VOLUME**,**YEAROFPUBLICATION****NAMESOFEDITORS**

VLTI/MIDIObservationsoftheMassiveProtostellarCandidateNGC3603IRS9A

StefanVehoff,1,2DieterE.A.N¨urnberger,1ChristianA.Hummel,3andWolfgangJ.Duschl4,5

Abstract.WeusedMIDI,themid-infraredinterferometricinstrumentoftheVLTI,toobservethemassiveprotostellarcandidateIRS9A,locatedatadistanceofabout7kpcattheperipheryoftheNGC3603starcluster.OurongoinganalysisshowsthatMIDIalmostfullyresolvestheobjectonallob-servedbaselines,yetbelow9µmwedetectasteepriseofthevisibility.Thisfeatureismodelledasacombinationofacompacthotcomponentandare-solvedwarmenvelopewhichlowersthecorrelatedfluxatlongerwavelengths.TheextendedenvelopecanalreadybeseeninbothMIDI’sacquisitionimagesandincomplementarydatafromaperturemaskingobservationsattheGeminiSouthtelescope.Itsshapeisasymmetric,whichcouldindicateacircumstellardiskinclinedagainstthelineofsight.Thecompactcomponentispossiblyre-latedtotheinneredgeofthis(accretion)disk.Theuncorrelatedmid-infraredspectrumappearsfeaturelessandcouldbecausedbyopticallythickemissionwithoutasignificantcontributionfromthediskatmosphere.

1.IntroductionThegiantHIIregionNGC3603ispoweredbyoneofthedensestclustersofhighmassstarsknowninourgalaxy.Duetoitsvicinitytothiscluster,IRS9AhasbeenliberatedfrommostofthegasanddustofitsnatalmolecularcloudbythestrongstellarwindsandionisingradiationarisingfromthenearbyO-typemain-sequencestars.Thisofferstheuniquepossibilitytoobserveahighmassstaratinfraredwavelengthsduringitsrelativelyearlyevolutionaryphase.

2.ObservationsanddatareductionIRS9AwasobservedwithMIDI(Leinertetal.2003)duringthreenightsin2005.Thefirsttwoobservationswerecarriedoutonthe26thandthe27th2Vehoffetal.UT2–UT32005-02-2708:35:1031.879.8”2005-02-2806:48:3538.060.8””07:43:5034.970.8””08:33:2531.780.2””09:21:1228.190.1UT3–UT42005-03-0307:10:4962.5131.9””08:54:3362.0155.5VLTI/MIDIObservationsofIRS9A3

Figure2.Left:AcquisitionimagefromVLTI+MIDI.Right:MEMimagefromGeminiSouth+T-ReCSaperturemaskingdata(J.Monnier,priv.comm.;scaleonbothaxesisinunitsofmas).

0 0.02 0.04 0.06 0.08 0.1

8 9 10 11 12 13V2

Wavelength [µm]

2005-02-28 - 06:48:3507:43:5008:33:2509:21:12

Figure3.Left:Spectraobtainedduringthesecondnight.Thedashedlinesaretheindividualmeasurements,thesolidlineshowstheaveragetogetherwiththestandarddeviationaserrorbars.Right:Correspondingvisibilitymeasurementsfromthesamenight.

2.3.VisbilitiesGiventhedetectionoftheextendedenvelopearoundIRS9Awealreadyexpectedthevisibilitiestobequitelow.Figure3showsthecalibratedandsquaredvis-ibilitiesofthesecondnight.Theirvalueisbasicallyzeroaboveawavelengthof9µm,butthereisaverysteeprisewithdecreasingwavelengthbelow9µm.However,eventhelargestvaluesareonlyoftheorderof0.1andlieattheveryedgeoftheatmosphericwindow.Exceptforoneobservationonthe3rdofMarch,allthemeasurementsareingoodagreementanddonotshowastrongdependencyonthepositionangle,ifany.

3.ModellingtheSEDandthevisibilitiesApartfromthespectrumtakenwithMIDIwehaveathandadditionalmid-infraredfluxesofIRS9A(N¨urnberger2003).WeusetwopubliclyavailableradiativetransfercodestomodelthespectralenergydistributionofIRS9A:ThefirstoneisDUSTY(Ivezi´c,Nenkova,&Elitzur1999),whichsolvesthe4Vehoffetal. 1 10 100 1000

1 10Flux [Jy]

Wavelength [µm]

data points from Nürnberger 2003data points from recent VISIR commissioning datasum of 3 black bodies with T = 250, 1350 and 22000 Kresult of a calculation with MC3D

0 0.02 0.04 0.06 0.08

0.1

8 9 10 11 12 13V2

Wavelength [µm]

2005-02-28 - 08:33:25model visibility from MC3D

Figure4.Left:SEDmodelobtainedwithMC3Dincomparisontothesumofthreeblackbodiesandouradditionalnear-infrareddata.Right:Thevisibilityofthismodelcomparedtooneofthemeasurements.

radiationtransportforasphericaldustdistribution.ThesecondoneisMC3D(Wolf,Henning,&Stecklum1999),whichcanhandlemorecomplexgeometriesbutusesMonteCarlomethodstosolvetheradiationtransport.BothmodelsareabletoreproducetheSEDquitewell.Theradiativetransfercodesallowtocreatemapsofthesurfacebrightnessforagivenwavelength,whichcanthenbeusedtocalculatethewavelengthdependentvisibilities.TheDUSTYmodelyieldsvisibilitieswhicharenottoofarfromourmeasurements,butthevisibilitybelow9µmrisesrathergently,anditalsoshowsabumpbetween9and10µm.ThevisibilitiesfromourMC3Dmodelproduceabetterfittotheobserveddata,buttheslopebelow9µmisstillnotsteepenough.Figure4showstheresultsobtainedwithMC3D.

4.DiscussionOurongoinganalysisoftheMIDIdatashowsIRS9Atobealmostcompletelyresolvedonbaselinesoftheorderof30m.Themid-infraredspectrumisfea-tureless,andmostlikelycausedbyemissionfromawarmenvelope.Themodelsaresofarunabletoaccountforthesteepriseofthevisibilitytowardstheshortwavelengthend,sothatthenatureofthiscompactcomponentremainsunclearandfurtherrefinementsofthemodelsareneeded.

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风云卫星数据和产品应用手册讲解

风云卫星数据和产品应用手册讲解

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风云三号气象卫星将实现全球、全天候、多光谱、三维、定量对地观测。

风云三号星发射总质量为2450kg，发射尺寸：4.38m×2m×2m，卫星长期功耗1130W。

卫星本体由服务舱、推进舱与有效载荷舱组成。

服务舱采用中心承力筒和隔板结构，主要安装电源、测控、数管及姿轨控分系统的部件和设备、推进舱采用中心承筒和隔板结构，主要安装推进系统设备以及蓄电池组和放电调节器。

有效载荷舱隔板和构架结构，主要安装探测仪器的探测头部，舱内主要安装探测仪器的电子设备等。

风云三号A卫星有十一台遥感探测仪器。

遥感数据通过两个实时传输信道（HRPT和MPT）和一个延时传输信道（DPT）进行传输。

风云三号A卫星设计寿命为3年。

1.2 主要技术指标1.2.1 卫星轨道⑴轨道类型：近极地太阳同步轨道⑵轨道标称高度：831公里⑶轨道倾角：98.81°⑷入轨精度：半长轴偏差： |Δa|≤5公里轨道倾角偏差：|Δi|≤0.1°轨道偏心率≤0.003⑸标称轨道回归周期为5.79天⑹轨道保持偏心率：≤0.00013⑺交点地方时漂移：2年小于15分钟⑻卫星发射窗口：降交点地方时10:051.2.2 卫星姿态⑴姿态稳定方式：三轴稳定⑵三轴指向精度：≤0.3°⑶三轴测量精度：≤0.05°⑷三轴姿态稳定度：≤4×10-3 °/s1.2.3 太阳帆板对日定向跟踪1.2.4 星上记时⑴记时方式：J2000日计数和日毫秒计数⑵记时单位：1毫秒⑶时间精度(星地总精度):小于20毫秒1.2.5 遥感探测仪器性能指标1.2.5.1 可见光红外扫描辐射计(VIRR)(1)通道数、各通道波段范围、灵敏度见表1-1。

(2)空间分辨率：星下点分辨率1.1Km(3)扫描范围：±55.4°(4)扫描器转速：6线/秒(5)每条扫描线采样点数：2048(6)MTF≥0.3(7)通道配准：飞行方向/扫描方向星下点配准精度<0.5个像元(8)扫描抖动：<0.8个IFOV(9)通道信号衰减：<15%/2年(10)量化等级：10比特(11)定标精度：可见光和近红外通道：CH1、2、7、8、9 7%(反射率)CH6、10 10%(反射率)红外通道：1k(270k)。

风云三号_E_星空间环境载荷综合探测技术

风云三号_E_星空间环境载荷综合探测技术

北京大学学报(自然科学版) 第60卷 第1期 2024年1月Acta Scientiarum Naturalium Universitatis Pekinensis, Vol. 60, No. 1 (Jan. 2024)doi: 10.13209/j.0479-8023.2023.096风云三号E星空间环境载荷综合探测技术沈国红1,2,†黄聪3,4张鹏飞5张效信3,4王金华5李佳薇3,4宗位国3,4张珅毅1,2张贤国1,2孙越强1,2杨勇5张焕新1,2邹鸿6王劲东1,2孙莹1,2白超平1,2田峥1,21.中国科学院国家空间科学中心, 北京 100190;2.北京市空间环境探测重点实验室, 北京 100190;3.中国气象局国家卫星气象中心北京市空间天气重点实验室, 北京 100081; 4.许健民气象卫星创新中心, 北京 100081; 5.上海卫星工程研究所, 上海 201109; 6.北京大学地球与空间科学学院, 北京摘要针对中国风云三号卫星运行的低地球太阳同步轨道, 开展空间环境及粒子辐射效应监测, 提出基于空间环境监测器Ⅱ型载荷的综合探测技术。

在各载荷技术指标的地面研制过程中, 通过标准放射源、等效信号源、粒子加速器和标准磁场等不同方式进行标定和实验验证。

结果表明, 多方向全能谱粒子探测的能量范围为30keV~300MeV, 精度优于10%; 磁场强度测量范围为−65023~+65023nT, 精度优于0.73nT; 电位探测范围为−32.4~+23.7kV, 灵敏度优于10V; 辐射剂量探测范围为0~3×104rad(Si), 灵敏度优于8.3rad(Si)。

通过空间环境监测器Ⅱ型载荷对卫星运行轨道上的粒子辐射环境、原位磁场矢量变化、辐射剂量累积以及卫星表面电位变化等进行观测, 可以为航天活动、卫星设计、空间科学研究及空间天气预警预报业务提供必要的数据支撑。

关键词空间环境; 粒子探测; 电位探测; 辐射剂量; 磁场探测Comprehensive Detection Payload Technology for SpaceEnvironment of FY-3E SatelliteSHEN Guohong1,2,†, HUANG Cong3,4, ZHANG Pengfei5, ZHANG Xiaoxin3,4, WANG Jinhua5,LI Jiawei3,4, ZONG Weiguo3,4, ZHANG Shenyi1,2, ZHANG Xianguo1,2, SUN Yueqiang1,2, YANG Yong5, ZHANG Huanxin1,2, ZOU Hong6, WANG Jindong1,2, SUN Ying1,2,BAI Chaoping1,2, TIAN Zheng1,21. National Space Science Center, Chinese Academy of Science, Beijing 100190;2. Beijing Key Laboratory of Space EnvironmentExploration, Beijing 100190; 3. Key Laboratory of Space Weather, National Satellite Meteorological Center, China Meteorological Administration, Beijing 100081; 4. Innovation Center for FengYun Meteorological Satellite (FYSIC), Beijing 100081;5. Shanghai Institute of Satellites Engineering, Shanghai 201109;6. School of Earth and Space Sciences,Abstract To monitor the space environment and its effects in the low-Earth sun-synchronous orbit of China’s FY-Ⅱ3 satellite, a comprehensive detection technology based on the type loads of the space environment monitor isproposed. In the process of ground development, various technical indicators of the space environment compre-hensive detection payload have been calibrated and experimentally verified by different methods such as standard radiation source, equivalent signal source, particle accelerator and standard magnetic field. The results show that the multi-direction full-spectrum particle detection achieves an energy range of 30 keV–300 MeV, with the accuracy of ≤10%. The magnetic field detection realizes the measurement range of −65023–+65023 nT, with the accuracy of ≤0.73 nT. The potential detection realizes the measurement range of −32.4–+23.7 kV, with the sensitivity of ≤10V.The detection of radiation dose realizes the measurement range of 0–3×104 rad (Si), with the sensitivity of ≤8.3 rad国家自然科学基金(41931073)和国家重点研发计划(2021YFA0718600)资助收稿日期: 2023–01–29; 修回日期: 2023–02–28145北京大学学报(自然科学版) 第60卷 第1期 2024年1月146(Si). Through comprehensive observation of particle radiation environment, change of in-situ magnetic field vector, radiation dose accumulation and change of satellite surface potential in satellite operation orbit, the space environ-ment monitor provides necessary data support for space activities, satellite design, space science research and space weather early warning and prediction.Key words space environment; particle detection; potential detection; radiation dose; magnetic field detection风云三号(FY-3)气象卫星是实现全球、全天候、多光谱、三维、定量遥感的我国第二代极轨气象卫星系列, 包括 01 批、02 批、03 批和已规划的04 吉林农业大学批共 4 个批次。

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然而，当前对ERA5对流层延迟产品精度评价的相关研究仍甚少。

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21925065_榴辉岩中单斜辉石-石榴子石镁同位素地质温度计评述

21925065_榴辉岩中单斜辉石-石榴子石镁同位素地质温度计评述

１０００ ０５６９／２０２０／０３６（０６） １７０５ １８ＡｃｔａＰｅｔｒｏｌｏｇｉｃａＳｉｎｉｃａ　岩石学报ｄｏｉ：１０ １８６５４／１０００ ０５６９／２０２０ ０６ ０４榴辉岩中单斜辉石 石榴子石镁同位素地质温度计评述黄宏炜１　杜瑾雪１　柯珊２ＨＵＡＮＧＨｏｎｇＷｅｉ１，ＤＵＪｉｎＸｕｅ１ ａｎｄＫＥＳｈａｎ２１ 中国地质大学地球科学与资源学院，北京　１０００８３２ 中国地质大学地质过程与矿产资源国家重点实验室，北京　１０００８３１ ＳｃｈｏｏｌｏｆＥａｒｔｈＳｃｉｅｎｃｅｓａｎｄＲｅｓｏｕｒｃｅｓ，ＣｈｉｎａＵｎｉｖｅｒｓｉｔｙｏｆＧｅｏｓｃｉｅｎｃｅｓ，Ｂｅｉｊｉｎｇ１０００８３，Ｃｈｉｎａ２ ＳｔａｔｅＫｅｙＬａｂｏｒａｔｏｒｙｏｆＧｅｏｌｏｇｉｃａｌＰｒｏｃｅｓｓｅｓａｎｄＭｉｎｅｒａｌＲｅｓｏｕｒｃｅｓ，ＣｈｉｎａＵｎｉｖｅｒｓｉｔｙｏｆＧｅｏｓｃｉｅｎｃｅｓ，Ｂｅｉｊｉｎｇ１０００８３，Ｃｈｉｎａ２０１９ １１ １４收稿，２０２０ ０４ ０８改回ＨｕａｎｇＨＷ，ＤｕＪＸａｎｄＫｅＳ ２０２０ Ｒｅｖｉｅｗｏｎｔｈｅｃｌｉｎｏｐｙｒｏｘｅｎｅ ｇａｒｎｅｔｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓｆｏｒｅｃｌｏｇｉｔｅｓ ＡｃｔａＰｅｔｒｏｌｏｇｉｃａＳｉｎｉｃａ，３６（６）：１７０５－１７１８，ｄｏｉ：１０ １８６５４／１０００ ０５６９／２０２０ ０６ ０４Ａｂｓｔｒａｃｔ Ｔｈｅｒｅｍａｒｋａｂｌｅｅｑｕｉｌｉｂｒｉｕｍｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｆｒａｃｔｉｏｎａｔｉｏｎｂｅｔｗｅｅｎｃｌｉｎｏｐｙｒｏｘｅｎｅａｎｄｇａｒｎｅｔｏｂｓｅｒｖｅｄｉｎｅｃｌｏｇｉｔｅｓｍａｋｅｓｉｔａｐｏｔｅｎｔｉａｌｈｉｇｈ ｐｒｅｃｉｓｉｏｎｇｅｏｔｈｅｒｍｏｍｅｔｅｒ Ｔｈｅｒｅｆｏｒｅ，ｔｈｉｓｐａｐｅｒｓｅｌｅｃｔｓ６４ｐａｉｒｓｏｆｃｌｉｎｏｐｙｒｏｘｅｎｅ ｇａｒｎｅｔｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｄａｔａｏｆｅｃｌｏｇｉｔｅｓｉｎｔｈｅＣｈｉｎｅｓｅｓｏｕｔｈｗｅｓｔｅｒｎＴｉａｎｓｈａｎｏｒｏｇｅｎ，ｉｎｔｈｅＤａｂｉｅ ＳｕｌｕｏｒｏｇｅｎａｎｄｉｎｔｈｅＫａａｐｖａａｌｃｒａｔｏｎｉｎｔｈｅＳｏｕｔｈＡｆｒｉｃａｆｒｏｍｌｉｔｅｒａｔｕｒｅｓ Ｔｈｅｎ，ｗｅｓｃｒｅｅｎｅｄ５０ｐａｉｒｓｏｆｄａｔａｔｈａｔｒｅａｃｈｔｈｅｅｑｕｉｌｉｂｒｉｕｍｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｆｒａｃｔｉｏｎａｔｉｏｎｂｙｔｈｅδ２６ＭｇＣｐｘ δ２６ＭｇＧｒｔｄｉａｇｒａｍ Ｕｓｉｎｇｔｈｅｓｅｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｅｑｕｉｌｉｂｒｉｕｍｆｒａｃｔｉｏｎａｔｉｏｎｄａｔａ，ｗｅｃａｌｃｕｌａｔｅｄｐｅａｋｔｅｍｐｅｒａｔｕｒｅｓｏｆｅｃｌｏｇｉｔｅｓｂｙｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓｏｆＨｕａｎｇｅｔａｌ （２０１３）ｔｈｒｏｕｇｈｆｉｒｓｔ ｐｒｉｎｃｉｐｌｅｓｃａｌｃｕｌａｔｉｏｎａｎｄＷａｎｇｅｔａｌ （２０１２）ａｎｄＬｉｅｔａｌ （２０１６）ｔｈｒｏｕｇｈｅｍｐｉｒｉｃａｌｅｓｔｉｍａｔｉｏｎ，ａｎｄｃｏｍｐａｒｅｄｔｈｅｍｗｉｔｈｔｈｅｐｅａｋｔｅｍｐｅｒａｔｕｒｅｓｇｉｖｅｎｂｙｏｔｈｅｒｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓ Ｂｙａｎａｌｙｚｉｎｇｔｈｅｃａｌｃｕｌａｔｉｏｎｒｅｓｕｌｔｓ，ｉｔｉｓｆｏｕｎｄｔｈａｔｆｏｒｏｒｏｇｅｎｉｃｅｃｌｏｇｉｔｅｓ，ｔｈｅｃａｌｃｕｌａｔｉｏｎｒｅｓｕｌｔｓｏｆｔｈｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｏｆＨｕａｎｇｅｔａｌ （２０１３）ａｒｅｃｏｎｓｉｓｔｅｎｔｗｉｔｈｔｈｏｓｅｐｒｅｖｉｏｕｓｌｙｏｂｔａｉｎｅｄｂｙｔｒａｄｉｔｉｏｎａｌｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓａｎｄｐｈａｓｅｅｑｕｉｌｉｂｒｉａｍｏｄｅｌｉｎｇ，ｗｈｉｌｅｔｈｅｃａｌｃｕｌａｔｉｏｎｒｅｓｕｌｔｓｏｆｔｈｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓｏｆＷａｎｇｅｔａｌ （２０１２）ａｎｄＬｉｅｔａｌ （２０１６）ａｒｅｓｉｇｎｉｆｉｃａｎｔｌｙｌｏｗｅｒ Ｆｏｒｔｈｅｃｒａｔｏｎｅｃｌｏｇｉｔｅｓ，ｔｈｅｃａｌｃｕｌａｔｉｏｎｒｅｓｕｌｔｓｏｆａｌｌｔｈｅｔｈｒｅｅｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓａｒｅｓｉｇｎｉｆｉｃａｎｔｌｙｄｉｆｆｅｒｅｎｔｆｒｏｍｒｅｓｕｌｔｓｏｆｔｒａｄｉｔｉｏｎａｌｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓｂｙｍｏｒｅｔｈａｎ５０℃，ｗｈｉｃｈｉｓｍｏｓｔｐｒｏｂａｂｌｙｃａｕｓｅｄｂｙｒｅ ｅｑｕｉｌｉｂｒｉｕｍｏｆｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｄｕｒｉｎｇｅａｒｌｙｒｅｔｒｏｇｒａｄｅｍｅｔａｍｏｒｐｈｉｓｍａｔｈｉｇｈｔｅｍｐｅｒａｔｕｒｅｓ Ｔｈｉｓｉｎｄｉｃａｔｅｓｔｈａｔｔｈｅｓｅｔｈｒｅｅｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓａｒｅｎｏｔａｐｐｌｉｃａｂｌｅｆｏｒｔｈｅｃｒａｔｏｎｅｃｌｏｇｉｔｅｓ Ｂａｓｅｄｏｎｔｈｅａｂｏｖｅｄａｔａ，ｔｈｅｍｅｔｈｏｄｏｆｅｍｐｉｒｉｃａｌｅｓｔｉｍａｔｉｏｎｉｓｕｓｅｄｔｏｃａｌｉｂｒａｔｅａｎｅｗｃｌｉｎｏｐｙｒｏｘｅｎｅ ｇａｒｎｅｔｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒ，ｗｈｉｃｈｉｓΔ２６ＭｇＣｐｘ Ｇｒｔ＝１ １１×１０６／［Ｔ（Ｋ）］２（Ｒ２＝０ ９２）．Ｉｎａｄｄｉｔｉｏｎ，ｔｈｉｓｐａｐｅｒａｌｓｏｂｒｉｅｆｌｙｄｉｓｃｕｓｓｅｓａｐｐｌｉｃａｔｉｏｎｐｒｏｓｐｅｃｔｏｆｔｈｅｃｌｉｎｏｐｙｒｏｘｅｎｅ ｇａｒｎｅｔｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒｓａｎｄｔｈｅｐｒｏｂｌｅｍｓｔｈａｔｓｈｏｕｌｄｂｅｐａｉｄａｔｔｅｎｔｉｏｎｔｏｄｕｒｉｎｇａｐｐｌｉｃａｔｉｏｎ Ｋｅｙｗｏｒｄｓ Ｅｃｌｏｇｉｔｅｓ；Ｉｓｏｔｏｐｅｇｅｏｔｈｅｒｍｏｍｅｔｅｒ；Ｍａｇｎｅｓｉｕｍｉｓｏｔｏｐｅ；Ｃｌｉｎｏｐｙｒｏｘｅｎｅ ｇａｒｎｅｔ摘　要 榴辉岩中单斜辉石和石榴子石之间显著的镁同位素平衡分馏，使其成为一种具有潜力的高精度地质温度计。