Subject: ~{<+9bJGUbQy2zIz5D#!~}

From: Atmospheric_Physics_Radiopropagation <[email-masked]>
Date: Thu, 9 Dec 1993 12:07:30 GMT

极光的形成简单来说是这样的：
    太阳不断地产生高速太阳风（由等离子体组成）。以超音速向地球方向传播的
太阳风同地球磁场相互作用的结果，在地球周围形成一种叫磁层（Magnetosphere)
的“庞然大物”。其尺度在向阳面大约有十几个地球半径，而在背日而却拖得很长，
达 200 个地球半径以上。这一磁层中的磁场的主要特征是在高纬地区（尤其在极
区地带）磁力线是开的，而不象中低纬度范围内的磁场磁力线是从南到北闭合的。
这样太阳风中的高速带电粒子就很容易从极区磁层中沉降到地球的大气层高度。这
些沉降到大气层高度上的高能粒子与地球大气（主要是氧和氮）相互碰撞和摩擦使
地球大气被电离和激发。被激发的大气份子和原子发出的光就形成所谓的极光。

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From: [email-masked] (GARMARHARD)
Date: 9 Dec 1993 20:49:03 GMT

Atmospheric_Physics_Radiopropagation ([email-masked]) wrote:
: ~{<+9b5DPN3I<r5%@4K5JGUbQy5D#:~}
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: ~{L+Qt7gM,5XGr4E3!O`;%WwSC5D=a9{#,TZ5XGrV\N'PN3IR;VV=P4E2c#(~}Magnetosphere)
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: ~{4o~} 200 ~{8v5XGr0k>6RTIO!#UbR;4E2cVP5D4E3!5DVwR*LXUwJGTZ8_N35XGx#(SHFdTZ<+~}
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: ~{P)3A=55=4sFx2c8_6HIO5D8_D\A#WSSk5XGr4sFx#(VwR*JGQu:M5*#)O`;%EvW2:MD&2AJ9~}
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~{5XGr5D4sFx2c!#H;:s2ESP<+9b#(<{G0Cf8=Ly#)!#

--
~{8gBm9~5B#@0~K@l@4sQ'~}

--
~{8gBm9~5B#@0~K@l@4sQ'~}

---

From: [email-masked] (GARMARHARD)
Date: 11 Dec 1993 18:43:54 GMT

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~{!>2N?<Ji!?
~{JVM7C;SP?FFU@`5DJi?I9)2N?<!#Ht6TW(R5JiSPPKH$#,Dc?I7-7-~}
  "Solar-Terrestrial Physics", by S.-I. Akasofu and S. Chapman, 1972, 
  Oxford (at the Clarendon) Press.
~{4KJiKdH;SPP)DjM7AK#,5+;y4!DZH]H+Cf#,6xGRVxU_V.R;~}Sydney Chapman
~{JGUbCE?FQ'#-!0?U<dNo@m!1#-5D?*MXU_V.R;#,G0U_N*:sU_5DQ'Iz#(Wf<.HU1>#)#,
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--
~{8gBm9~5B#@0~K@l@4sQ'~}