Variations of hot O in the thermosphere
Variations of hot O in the thermosphere
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DOI：
10.1029/1999gl900612
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发表时间：
1999-09
影响因子：
5.2
通讯作者：
William L. Oliver;J. Schoendorf
中科院分区：
文献类型：
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作者：
William L. Oliver;J. Schoendorf
利用电子温度和密度的测量，中性密度的模型，以及O+−O碰撞截面的理论表达式，我们计算了离子温度，发现它低于测量值。我们计算了在4000°K时提供这种热亏损所需的热O的量。在400公里的高度上，太阳活动极大期只需要很少的热氧，而在太阳活动极大期，总氧的1-2%必须是热的。在400公里高度的热氧密度在白天最低，在晚上最高;在春分点最低，在至点最高;在太阳最大值最低，在太阳最小值最高;最低的磁干扰时期，最高的平静时期;最低的温暖，密集的热层，最高的凉爽，罕见的热层。所有这些变化是一致的热淬火环境O，较大的环境O密度产生较低的热O密度。这表明热O应该在大气中形成一层形状。
Using measurements of electron temperature and density, a model of neutral density, and a theoretical expression for the O+−O collision cross section, we compute the ion temperature and find it to be lower than the measured value. We compute the amount of hot O at 4000°K necessary to provide this heat deficit. At 400 km altitude very little hot O is needed at solar maximum while 1–2% of total O must be hot at solar maximum. Hot O densities at 400 km altitude are lowest during the day, highest at night; lowest at the equinoxes, highest at the solstices; lowest at solar maximum, highest at solar minimum; lowest for magnetically disturbed periods, highest for quiet periods; lowest for a warm, dense thermosphere, highest for a cool, rare thermosphere. All of these variations are consistent with thermal quenching by ambient O, with larger ambient O densities yielding lower hot O densities. This indicates that hot O should form a layer shape in the atmosphere.