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首页> 外文会议>Cluster and double star symposium >STATISTICAL STUDY OF RELATIONSHIPS BETWEEN DAYSIDEHIGH-ALTITUDE/-LATITUDE O+ OUTFLOWS, SOLAR WINDS, AND GEOMAGNETICACTIVITY
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STATISTICAL STUDY OF RELATIONSHIPS BETWEEN DAYSIDEHIGH-ALTITUDE/-LATITUDE O+ OUTFLOWS, SOLAR WINDS, AND GEOMAGNETICACTIVITY

机译：日高海拔/纬度O +气流，太阳风和地磁活动关系的统计研究

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摘要

The terrestrial origin O+ outflow, which is persistentlyrnobserved by the Cluster CIS/CODIF instrument, wasrnstudied statistically in succession in the dayside highaltitudern(from 5 up to 11 RE) and high-latitude (from 75rnto 90 degrees invariant latitude, deg ILAT) region. We extendedrnthe previous study (Arvelius et al., 2005a), investigatingrncorrelations between the properties (namely, maximumrnor 'dominant' differential particle flux,MDPF, andrnits energy, PE) of dayside high-altitude polar outflowingrnO+, solar winds (solar wind moments and the interplanetaryrnmagnetic field, IMF, conditions), and local mid-/lowlatituderngeomagnetic activity (measured by ASY /SYMrnindices). In this study, we found firstly that energizationrnand/or acceleration of dayside high-altitude polar outflowingrnO+ is(are) controlled by both strong southwardrnIMF (defined by intensity, Bt, and clock angle, θ. In thisrncase, |θ|>135°) and solar wind moments (except solarrnwind electric field), but it(they) occur(s) at two differentrnplaces: one is the poleward cusp and/or the mantle regionrncontrolled by the IMF, the other is the entire polarrncap controlled by the solar wind moments. Secondarilyrnoutflowing O+ flux enhancement and O+ keV energization/rnacceleration process(es) are different in terms ofrnoccurrence time scale and location, even tough both arerncontrolled by solar winds and the IMF. Thirdly both energization/rnacceleration and flux enhancement of daysidernhigh-altitude and high-latitude outflowing O+ correlaternto local mid-/low-latitude geomagnetic activity (as measuredrnby ASY /SYM indices), I.e. higher energy of outflowingrnO+ appears at higher altitudes and more equatorwardrn(a similar trend to that of the Kp index (Arveliusrnet al., 2005a)), and flux enhancement of outflowing O+rnappears at lower altitudes and more poleward. However the correlation is not as clear as the case of the IMF conditionsrn/ the solar wind parameters.
机译：由簇CIS / CODIF仪器持续观测的陆地起源O +流出，在白天的高海拔（从5到11 RE）和高纬度（从75rn到90度不变纬度，度ILAT）区域进行了连续的统计研究。我们扩展了先前的研究（Arvelius et al。，2005a），研究了日间高空极性流出rnO +，太阳风（太阳风矩和太阳辐射）的性质（即最大或主要的微分粒子通量，MDPF和能量，PE）之间的相关性。行星际磁场，IMF，条件）和局部中低纬度地磁活动（由ASY / SYMrnindices测量）。在这项研究中，我们首先发现，白天高空极性流出rnO +的通电和/或加速受强南向IMF（强度，Bt和时钟角θ的控制）。在这种情况下，|θ|> 135° ）和太阳风矩（太阳风电场除外），但它们发生在两个不同的地方：一个是极点风口和/或受IMF控制的地幔区域，另一个是整个太阳极控制的极帽风的瞬间。其次，流出的O +通量增强和O + keV通电/加速过程在发生时间的尺度和位置方面是不同的，甚至很难通过太阳风和IMF来控制。第三，与高中低纬度地磁活动有关的高纬度和高纬度流出O +的增磁/加速和通量增强（通过ASY / SYM指数测量），即较高的海拔高度和赤道方向出现较高的流出rn +能量（与Kp指数的趋势相似（Arveliusrnet al。，2005a）），而较低的海拔高度和极向则出现流出的O + rn的通量增强。但是，相关性不如IMF条件/太阳风参数的情况明确。

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