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星簇2號

編輯連結
維基百科，自由的百科全書
星簇 II號衛星
星簇2號衛星群
星簇2號衛星群藝術想象圖
任務類型磁層研究
運營方歐洲空間局與美國宇航局合作
國際衛星標識符FM6 (薩爾薩): 2000-041A
FM7 (桑巴): 2000-041B
FM5 (倫巴): 2000-045A
FM8 (探戈): 2000-045B
衛星目錄序號FM6 (薩爾薩): 26410
FM7 (桑巴): 26411
FM5 (倫巴): 26463
FM8 (探戈): 26464
網站http://sci.esa.int/cluster
任務時長計劃: 5 年
已過去：24年3個月又10天
航天器屬性
製造方空客公司 (以前的多尼爾衛星系統公司)[1]
發射質量1200(2600磅)[1]
乾質量550千克(1210磅)[1]
酬載質量71(151磅)[1]
尺寸2.9x1.3米(9.5x4.3英尺)[1]
功率224 瓦[1]
任務開始
發射日期FM6: 2000年7月16日世界時12點39分
FM7: 2000年7月16日世界時12點39分
FM5:2000年8月9日世界時11點13分
FM8: 2000年8月9日世界時11點13分
運載火箭聯盟U/弗蓋特運載火箭
發射場拜科努爾航天發射場31號發射台
承包方斯塔瑞森公司
軌道參數
參照系地心軌道
軌域橢圓軌道
近地心點FM6:16118千米(10015英里)
FM7:16157千米(100395英里)
FM5: 16022千米(9956英里)
FM8: 12902千米(8017英里)
遠地心點FM6:116740千米(72540英里)
FM7:116654千米(72485英里)
FM5: 116786千米(72567英里)
FM8:119952千米(74535英里)
傾角FM6: 135度
FM7: 135度
FM5: 138度
FM8: 134度
週期FM6: 3259分鐘
FM7: 3257分鐘
FM5: 3257分鐘
FM8: 3258分鐘
曆元2014年3月13日世界時11點15分07秒

星簇II號（Cluster II）[2]是一項美國宇航局參與的歐洲空間局太空探測任務，目的是在近兩個太陽周期內研究地球磁層。該任務由四顆相同衛星組成四面體隊形飛行，以替代1996年因發射失敗而被毀的原星簇衛星，四顆星簇II號衛星於2000年7月和8月在哈薩克斯坦拜科努爾分別搭乘兩枚「聯盟-弗雷加」火箭上成對發射升空。2011年2月，星簇II號衛星慶祝了10年成功的空間探測行動。截至2020年10月，其任務已延長至2022年底[3]。2004年至2007年，中國國家航天局/歐空局雙星任務與星簇II號衛星群一起運行。

任務概述

從北黃極視角顯示星簇2號衛星自2004年3月21日來一周內的飛行軌跡。網格線表示地球弓形激波（綠色外層）和磁層（藍色內層）的平均位置。由於地球環太陽運行，在該照片中，衛星軌道似乎在旋轉，太陽位於上方。

這四顆完全相同的星簇II號衛星組隊環繞地球飛行，以研究太陽活動對地球空間環境的影響。該任務是太空探測史上首次能夠收集有關太陽風如何與磁層相互作用並影響包括極光在內的近地空間及其大氣層的三維信息。

這些衛星外形為1.3米高、直徑2.9米的扁平圓柱體（查看在線三維模型 Archive.is的存檔，存檔日期2012-07-07），質量1200千克，其中包括650千克的推進劑和71千克的儀器，以每分鐘15圈的自旋速度保持穩定。發射後，圓柱體側面覆蓋的太陽能板可為儀器（47瓦）和各種設備（特別是通信）提供224瓦的電力，剩餘電能將儲存在5塊總容量為80安時的鎘銀電池中。由於高能帶電粒子的損害，太陽能電池板的功率會隨着任務的進行而逐漸下降，但事前已計劃好其功率水平足以保障探測操作。四顆衛星都安裝有一台400牛頓的主推進器和8台10牛頓的小型火箭發動機，燃料為聯氨和過氧化氮混合物。主引擎用於將衛星送入工作軌道上，然後調整與其他三顆衛星的距離，相距4公里到10000公里不等，機動組成各種四面體隊形以研究磁層結構和邊界。一旦進入軌道，衛星將展開多根天線和電纜：2根通信天線、2根5米長的儀器傳感器杆、4根50米長用於電場和波實驗的徑向延伸電纜，衛星平台設計至少運行5年[4][5]。

衛星高度橢圓的軌道最初抵達約4倍地球半徑（RE=6371公里）的近地點和19.6倍的遠地點，每圈軌道運行時間約需57小時。衛星軌道將隨着時間的推移發生改變，拱頂線逐步向南旋轉，使得軌道穿過磁尾電流片的距離逐漸減小，並可對所穿越緯度的大範圍白晝側磁層頂進行採樣。引力效應使近地點（和遠地點）距離發生了長期變化，2011年，近地點縮減至數百公里，然後又開始上升，軌道平面已偏離了90度傾角，歐洲太空營運中心的軌道修正也將衛星繞軌周期改為了54小時，所有這些變化使得該衛星群能夠探訪比最初兩年任務更廣的一系列重要磁層區，從而擴大了任務的探測範圍。

歐洲太空營運中心（ESOC）進行遙測並將來自衛星的科學數據分發到在線數據中心。位於英國盧瑟福阿普爾頓實驗室的聯合科學運營中心（JSOC）負責協調科學規劃，並與儀器團隊合作，向歐洲空間業務中心提供合併的儀器指令請求。

星簇衛星科學檔案是歐空局星簇和雙星科學任務的長期檔案。自2014年11月1日起，它是星簇任務科學數據和支持數據庫的唯一公共訪問點。雙星數據可通過該檔案公開獲得。星簇衛星科學檔案館位於西班牙馬德里附近的歐洲空間天文中心內歐空局所有其他科學檔案館旁。從2006年2月到2014年10月，可以通過星簇衛星科學檔案 （頁面存檔備份，存於網際網路檔案館）訪問星簇衛星數據。

歷史

星簇衛星任務於1982年被提交給歐空局，並於1986年與太陽和日光層觀測台（SOHO）一起獲得批准，這兩項任務共同構成了歐洲航天局地平線2000計劃的日地物理學「奠基石」任務。 儘管最初的星簇衛星於1995年完成，但由於1996年攜帶衛星的阿麗亞娜5型火箭爆炸，使任務被推遲四年，以重新研製新的儀器和衛星。

2000年7月16日，一枚從拜科努爾航天發射場發射的聯盟-弗雷加火箭將兩顆替代的星簇2號衛星（薩爾薩號和桑巴號）送入停駐軌道，在那裡它們以自身動力機動到環繞期為57小時的19000×119000公里軌道。三周後的2000年8月9日，另一枚「聯盟-弗雷加」火箭將其餘兩顆衛星（倫巴號和探戈號）送入相同的軌道。1號衛星「倫巴」也被稱為鳳凰衛星，因為它主要是用原任務失敗後剩下的備件所製造。四顆在軌衛星經設備調試後，於2001年2月1日展開了首次科學探測。

歐洲空間局在所有歐空局成員國中舉辦了一場衛星征名大賽[6]，來自英國的雷·科頓以倫巴、探戈、薩爾薩和桑巴等名稱贏得了比賽[7]。雷居住的市鎮布里斯托爾被授予微縮版衛星模型，以表彰獲獎作品以及該市與衛星的聯繫[8][9]。在擺放多年後，它們最終在盧瑟福·阿普爾頓實驗室找到了自己歸宿。

該任務原計劃只持續到2003年底，現已多次延期。第一次從2004年延至2005年，第二次從2005年延至2009年6月，目前該任務已延長至2020年底[10]。

科學目標

地球磁層示意圖，太陽風從左向右吹。弓形激波(Bow shock)、偏轉的太陽風粒子(Deflected solar wind particles)、射入的太陽風粒子(Incoming solar wind particles)、磁鞘(Magentsheath)、磁尾(Magentotail)、中性層(Neutral sheet)、等離子片(Plasma sheet)、極尖區(Polar cusp)、范艾倫輻射帶(Van Allen radiation belt)。

以前僅靠一、兩顆衛星飛行任務無法提供準確研究磁層邊界所需的數據，由於組成磁層的等離子體無法用遙感技術進行觀測，因此必須使用衛星進行原位測量。四顆衛星使科學家能夠進行所需的三維辨時測量，以創建磁層區域之間以及磁層和太陽風間所發生的複雜等離子體相互作用的真實圖像。

每顆衛星都攜帶了11台探測儀器，旨在研究關鍵等離子體區時空內的小尺度等離子體結構：太陽風、弓形激波、磁層頂、極地尖點、磁尾、等離子層邊界層以及極冠上空和極光帶。

  • 弓形激波是地球和太陽之間的空間區域，在那裡太陽風在繞地球偏轉之前從超音速減速到亞音速。在穿越該區域時，衛星進行測量以幫助描述發生在弓激波中的作用過程，例如異常熱流的起源和穿過來自太陽風的弓形激波和磁鞘傳播的電磁波。
  • 弓形激波的背後是分隔地球和太陽風磁場的薄等離子體層，稱為磁層頂。因太陽風壓的不斷變化，該邊界也在不斷移動。但由於太陽風和磁層內的等離子體和磁壓分別應處於平衡狀態，因此磁層應該是一層不可穿透的邊界。然而，現已觀察到等離子體從太陽風中穿過磁層頂進入磁層的現象。 星簇2號衛星的四點測量使得追蹤磁層頂的運動以及闡明太陽風中等離子體的穿透機製成為可能。
  • 在北半球和南半球兩個地區，地球磁場與磁層頂垂直而非相切。這些「極地尖點」允許由離子和電子組成的太陽風粒子流入磁層。星簇2號衛星將記錄粒子的分布，從而可以描述外部尖點的湍流區域。
  • 被太陽風吹離太陽的地球磁場區域統稱為「磁尾」，長度跨越月球的兩個裂瓣構成了外磁尾，而中央等離子片則形成高度活躍的內磁尾。星簇2號衛星將監測來自電離層的粒子和太陽風，因為它們穿過了磁尾瓣。在中央等離子體片中，衛星將測定離子束的起源以及由亞磁暴引起的磁場向電流的紊亂。
  • 大氣層中沉澱的帶電粒子在磁極周圍形成了一圈輻射光環，稱為「極光帶」，星簇衛星將測量該區域不同時間的瞬態粒子流及電場和磁場的變化

每顆星簇衛星上的儀器

星簇2號衛星上的儀器

四顆星簇2號衛星中的每顆都攜帶了11台相同的儀器（總質量71 公斤），其功能如下表所示。 這些儀器一方面測量電場 (E) 和磁場 (B) 的強度和方向；另一方面測量構成等離子體的電子和離子的密度與分布。


編號 縮寫 儀器 測量 用途
1 ASPOC 衛星電位主動控制器 衛星靜電位的調節 啟用冷電子的等離子體電子和電流探測器進行測量（數電子伏特溫度），否則會被衛星光電子遮蔽。
2 CIS 星簇離子譜儀 測量離子飛行時間（TOFs）和從0到40千電子伏特的能量 等離子體中離子的組成和三維分布
3 DWP 數字波處理器 協調電場和波實驗儀、場波動時空分析器、寬帶數據設備和高頻波及電子密度探測器的操作。 最低級別，提供電信號以同步儀器採樣；最高級別，通過宏命令啟用更複雜的操作模式。
4 EDI 電子漂移器 探測E電場的大小和方向 E矢量，局部磁場B中的梯度。
5 EFW 電場和波實驗儀 探測E電場的大小和方向 E矢量、航天器電位、電子密度和溫度。
6 FGM 磁通門磁力計 測量B磁場的大小和方向 除衛星電位主動控制器外，B矢量和事件觸發的所有儀器。
7 PEACE 等離子體電子和電流探測器 測量從0.0007到30千電子伏特的電子能量 等離子體中電子的三維分布
8 RAPID 自適應粒子成像探測器研究設備 測量39到406千電子伏特的電子能量；20到450電子伏特的離子能量。 等離子體中高能電子和離子的三維分布。
9 STAFF 場波動時空分析器 檢測B磁場電磁波動的幅度和方向，E和B」的互相關性。 小尺度電流結構特性、等離子波和湍流來源。
10 WBD 寬帶數據設備 從25赫茲至577赫茲選定頻段內，對電場和磁場進行高時間分辨率測量。它提供了一種獨特的新功能來執行甚長基線干涉測量（VLBI）。 地球磁層及其附近的自然等離子體波（如極光千米波輻射）的特性，包括：源位置、大小和擴展。
11 WHISPER 高頻波和電子密度探測器 2–8千赫範圍內發射的無線電和地球等離子體波的E電場頻譜圖；通過有源發聲器觸發等離子體共振 通過三角測量定位波源位置及0.2-80厘米−3範圍內的電子密度。

與中國的雙星任務

2003年和2004年，中國國家航天局發射了雙星衛星"探測1號"(TC-1)和"探測2號"(TC-2)，該任務與星簇2號衛星合作，主要在磁層內進行協作測量。探測1號於2007年10月14日停止運行，探測2號則在2008年發回最後一次數據，探測2號對磁星[11][12]以及磁層物理學研究做出了貢獻研究做出了貢獻。探測1號檢測了地球弓形激波附近的密度洞，這些密度洞可能在弓形激波的形成中發揮了作用[13][14]。此外，它還觀察了中性層的振盪[15]。

獎項

星簇團隊獎

個人獎

發現和任務里程碑

2020年

2019年

2018年

2017年

2016年

2015年

2014年

2013年

2012年

2011年

2010年

2009年

2008年

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2006年

2005年

2004年

2001年–2003年

精選刊物

截至2021年10月31日，所有與星簇和雙星任務有關的3522篇出版物都可以在 歐空局星簇探測任務網刊物區 （頁面存檔備份，存於網際網路檔案館）找到。在這些出版物中，有3029篇參考刊物、342篇論文、121篇博士論文和30篇其他類型的論文。

參考文獻

  1. ^ 1.0 1.1 1.2 1.3 1.4 1.5 Cluster (Four Spacecraft Constellation in Concert with SOHO). ESA. [2014-03-13]. （原始內容存檔於2021-12-29）. 
  2. ^ Cluster II operations. European Space Agency. [29 November 2011]. （原始內容存檔於2011-12-31）. 
  3. ^ Extended Operations Confirmed for Science Missions. ESA. [6 July 2021]. （原始內容存檔於2021-11-13）. 
  4. ^ Cluster 3D Model Archive.is的存檔，存檔日期2012-07-07, ESA
  5. ^ {{URL|example.com|可选的显示文本}}
  6. ^ European Space Agency Announces Contest to Name the Cluster Quartet (PDF). XMM-Newton Press Release (European Space Agency). 2000: 4 [2021-12-29]. Bibcode:2000xmm..pres....4.. （原始內容存檔 (PDF)於2016-03-04）. 
  7. ^ Bristol and Cluster – the link. European Space Agency. [2 September 2013]. （原始內容存檔於2013-09-03）. 
  8. ^ Cluster II – Scientific Update and Presentation of Model to the City of Bristol. SpaceRef Interactive Inc. [2021-12-29]. （原始內容存檔於2013-09-03）. 
  9. ^ Cluster – Presentation of model to the city of Bristol and science results overview. European Space Agency. [2021-12-29]. （原始內容存檔於2013-09-03）. 
  10. ^ Extended life for ESA's science missions. ESA. [14 November 2018]. （原始內容存檔於2019-09-04）. 
  11. ^ Schwartz, S.; et al. A γ-ray giant flare from SGR1806-20: evidence for crustal cracking via initial timescales. The Astrophysical Journal. 2005, 627 (2): L129–L132. Bibcode:2005ApJ...627L.129S. S2CID 119371524. arXiv:astro-ph/0504056 可免費查閱. doi:10.1086/432374. 
  12. ^ ESA Science & Technology - Double Star and Cluster observe first evidence of crustal cracking. sci.esa.int. September 21, 2005 [2021-07-14]. （原始內容存檔於2021-12-29） （美國英語）. 
  13. ^ ESA Science & Technology - Cluster and Double Star discover density holes in the solar wind. sci.esa.int. June 20, 2006 [2021-07-14]. （原始內容存檔於2021-12-29）. 
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外部連結

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