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H alpha stokes V/I features observed in a solar active region

机译:在太阳活动区域中观察到的H alpha行程V / I特征

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We carried out an imaging polarimetry observation of active region NOAA 10596 at 9-11 wavelengths around the Ha line with a ferroelectric liquid-crystal polarimeter during 2004 April 20-26. The latitude of the region was S8 degrees, and it passed the central meridian on April 23. On the basis of this observation, the Stokes V/I features of the active region in H alpha, which are expected to indicate the chromospheric longitudinal magnetic field, were revealed as follows: (1) There is persistent weakening (sometimes reversal) of the Stokes V/I signal at the center of the umbra. This is not due to the actual weakening of the magnetic field strength, but probably due to the peculiarity of the atmospheric structure of the umbral chromosphere. (2) The peak wavelengths of the Stokes V/I profile of the plages and that of the sunspot are systematically different from each other and, therefore, it is difficult to apply the weak-field approximation to estimate the chromospheric magnetic field strength. Both of these results mean that an estimation of the chromospheric magnetic field on the basis of the H alpha polarimetry is not straightforward, and that an inversion considering the atmospheric structure in the chromosphere is essentially important.
机译:我们用铁电液晶偏振计在2004年4月20-26日对Ha线周围9-11波长处的活动区域NOAA 10596进行了成像偏振光观察。该区域的纬度为S8度,并于4月23日通过了中央子午线。基于此观察结果,活动区域的斯托克斯V / I特征位于H alpha中,有望指示色球纵向磁场,显示如下:(1)在本影中心,斯托克斯V / I信号持续减弱(有时会反转)。这不是由于磁场强度的实际减弱,而可能是由于本影色球层大气结构的特殊性所致。 (2)斑块的Stokes V / I轮廓的峰值波长和黑子的峰值波长在系统上是彼此不同的,因此,很难应用弱场近似来估计色球磁场强度。这两个结果都意味着基于Hα极化法估算色球层磁场并不简单,考虑到色球层中大气结构的反演至关重要。

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