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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Validation of a scaling law for the coronal magnetic field strength and loop length of solar and stellar flares
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Validation of a scaling law for the coronal magnetic field strength and loop length of solar and stellar flares

机译：验证冠状磁场强度和太阳能和恒星耀斑的循环长度的缩放法

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摘要

Shibata and Yokoyama (1999, ApJ, 526, L49; 2002, ApJ, 577, 422) proposed a method of estimating the coronal magnetic field strength (B) and magnetic loop length (L) of solar and stellar flares, on the basis of magnetohydrodynamic simulations of the magnetic reconnection model. Using the scaling law provided by Shibata and Yokoyama (1999, ApJ, 526, L49; 2002, ApJ, 577, 422), we obtain B and L as functions of the emission measure (EM = n(2)L(3)) and temperature (T) at the flare peak. Here, n is the coronal electron density of the flares. This scaling law enables the estimation of B and L for unresolved stellar flares from the observable physical quantities EM and T, which is helpful for studying stellar surface activities. To apply this scaling law to stellar flares, we discuss its validity for spatially resolved solar flares. Quantities EM and T are calculated from GOES (Geostationary Operational Environmental Satellite) soft X-ray flux data, and B and L are theoretically estimated using the scaling law. For the same flare events, B and L were also observationally estimated with images taken by the Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager (HMI) Magnetogram and Atmospheric Imaging Assembly (AIA) 94 angstrom pass band. As expected, a positive correlation was found between the theoretically and observationally estimated values. We interpret this result as indirect evidence that flares are caused by magnetic reconnection. Moreover, this analysis makes us confident about the validity of applying this scaling law to stellar flares as well as solar flares.
机译：Shibata和Yokoyama（1999年，ApJ，526，L49；2002年，ApJ，577，422）提出了一种基于磁重联模型的磁流体动力学模拟估算太阳耀斑和恒星耀斑日冕磁场强度（B）和磁环长度（L）的方法。利用Shibata和Yokoyama（1999年，ApJ，526，L49；2002年，ApJ，577，422）提供的标度定律，我们得到了B和L作为排放测量值（EM=n（2）L（3））和耀斑峰值温度（T）的函数。这里，n是耀斑的日冕电子密度。这种标度律可以根据可观测的物理量EM和T来估计未分辨恒星耀斑的B和L，这有助于研究恒星表面的活动。为了将这个比例定律应用于恒星耀斑，我们讨论了它对空间分辨太阳耀斑的有效性。根据GOES（地球静止运行环境卫星）软X射线通量数据计算EM和T，并使用标度定律从理论上估算B和L。对于相同的耀斑事件，B和L也通过太阳动力学观测台（SDO）/太阳地震和磁成像仪（HMI）磁图和大气成像组件（AIA）94埃通带拍摄的图像进行了观测估计。正如预期的那样，理论估计值和观测估计值之间存在正相关性。我们将这一结果解释为耀斑是由磁重联引起的间接证据。此外，这一分析使我们确信，将这种标度定律应用于恒星耀斑以及太阳耀斑的有效性。

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