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# System prepended metadata

title: '#立方衛星設計計畫  CubeSat Mission Plan'

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# #立方衛星設計計畫  CubeSat Mission Plan
**<font color="#f00">目錄MENU:</font>**
1.About US
2.Why we have this idea?
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<font color="#f9955FF">1. About us:</font>
We come from Nanshan senior highschool 
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2. Why we have this idea:(Because everyone wants to see the beauty of the aurora, we want to do this)

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福衛五號是台灣發射的衛星，福衛五號運行於720公里太陽同步圓形軌道，傾角98.28°。福衛五號之主要光學遙測酬載，可提供2米解析度的全色(Panchromatic)和4米解析度的多波譜(Multi-spectral) 彩色影像。福衛五號也有酬載「先進電離層探測儀」，其為多功能的電漿量測儀器，可實地量測電離層的電漿成份與密度、運動速度、溫度等物理量。此儀器可收集電漿擾動變化，以研究電離層在地震前的可能異常現象。


5.怎麼會發生極光?(陳重安)
太陽風暴壓迫磁層，假如磁線像過度延展的橡皮筋一般斷裂，那些回縮的磁場磁力線將太陽粒子拉回極光同現區，而將被迫繞道的太陽粒子甩往地球，太陽粒子與地表 20 至 200 哩之上的中性氧、氮原子碰撞，把自身攜帶的能量傳遞給他們並且轉為激發態釋出光子，有光子的地方就會產生北極光與南極光。
https://tw.voicetube.com/videos/8576


但它們可以通過計算原子粒子的傳感器檢測到——帶電的質子和電子在地球周圍的空間中移動

同樣地，為了要捕捉外地核內的微小變化，的部份也需要從衛星所測得的總磁場訊號濾除，」Vincent Lesur 解釋。GFZ 衛星任務 CHAMP 與 GRACE 所記錄的資料首度使這件事能夠辦到。
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短摘:
我們知道極光(Aurora)發生的原因是因為太陽風暴壓迫磁層，假如磁線像過度延展的橡皮筋一般斷裂，那些回縮的磁場、磁力線將太陽粒子拉回極光同現區( auroral oval)，而將被迫繞道的太陽粒子甩往地球，太陽粒子進入電離層(Ionosphere)並與電離層中的中性氧、氮原子碰撞，把自身攜帶的能量傳遞給他們並且轉為激發態，等一段時間後他會轉回基礎態並釋出光子，有光子的地方就會產生北極光或南極光(視情況而定)。
為了更準確的預測極光的發生，我們決定把多顆立方衛星發射到地球的南北緯80~90°的低軌道軌道，藉由觀測地磁的變化和太陽風和地球的距離
，而觀測地磁的變化，我們透過測量地球重力場的變化，並用衛星測得的總磁場訊號濾除磁性地殼的部份以及電離層與磁層，利用多顆立方衛星分別觀測地球衛星軌道的擾動和太陽風和地球的距離，讓資料回傳並加以運算。一個更準確的極光預測就會出現了，也對未來對磁力線或離子的實驗數據有幫助。

We know that the reason Aurora occurs is because solar storms compress the magnetosphere. If the magnetic lines break like overextended rubber bands, those retracted magnetic field and magnetic field lines pull the sun particles back to the aurora iso-present zone. The sun particles that were forced to take a detour were thrown towards Earth. Sun particles enter the Ionosphere and collide with neutral oxygen and nitrogen atoms in the ionosphere, transmitting the energy they carry to them and turning into an excited state, after a period of time they will turn back to the fundamental state and release the photons, where there are photons, the Northern Aurora or the Southern Aurora will be produced (depending on the situation).In order to more accurately predict the occurrence of the aurora, we decided to launch multiple cubesats into the low orbit of the Earth's north and south latitudes of 80 to 90 degrees to observe the changes in geomagnetism and the distance between the solar wind and the Earth. To observe changes in geomagnetism, we measure changes in the Earth's gravitational field and filter out parts of the magnetic crust as well as the ionosphere and magnetosphere using the total magnetic field signal measured by satellites. Multiple cubesats are used to observe the disturbances in the orbits of the Earth satellite and the distance between the solar wind and the Earth, so that the data can be transmitted back and calculated. A more accurate aurora prediction will emerge that will also help with future experimental data on magnetic field lines or ions.

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參考文獻:
https://www.easyatm.com.tw/wiki/%E5%9C%B0%E7%90%83%E9%87%8D%E5%8A%9B%E5%A0%B4
https://www.gfz-potsdam.de/champ
https://pansci.asia/archives/30191
https://tw.voicetube.com/videos/8576




































