WAVE DAMPING OBSERVED IN UPWARDLY PROPAGATING SAUSAGE-MODE OSCILLATIONS CONTAINED WITHIN A MAGNETIC PORE
WAVE DAMPING OBSERVED IN UPWARDLY PROPAGATING SAUSAGE-MODE OSCILLATIONS CONTAINED WITHIN A MAGNETIC PORE
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DOI：
10.1088/0004-637x/806/1/132
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发表时间：
2015-06-10
影响因子：
4.9
通讯作者：
Erdelyi, R.
中科院分区：
文献类型：
--
作者：
Grant, S. D. T.;Jess, D. B.;Erdelyi, R.
我们目前的观测证据的可压缩MHD波模式从太阳光球通过太阳磁孔的过渡区的基础上传播。使用邓恩太阳望远镜同时获得了四个波段的高节奏图像。采用傅立叶和小波技术，香肠模式振荡显示显着的功率检测强度和面积波动。强度和面积的波动表现出从181到412秒的周期范围，平均周期类似于290秒，与全球p-模式光谱一致。发现存在于相邻带通中的强度和面积振荡彼此异相，在410埃连续G带、G带-Na I D 1和Na I D-1-Ca II K高度之间分别显示6 °.12、5 °.82和15 °.97的相位角，重申存在向上传播的香肠模式波。一个相位关系类似0度之间的同带通发射和面积扰动的孔隙最好归类的波属于“慢”制度的色散图。理论计算表明，这些波是表面模式，初始光球能量超过35，000 W m（-2）。波能量学表明能量随大气高度的大幅降低，证实磁孔能够传输表现出可观的能量阻尼的波，这可能会释放相当大的能量到本地色球等离子体中。
We present observational evidence of compressible MHD wave modes propagating from the solar photosphere through to the base of the transition region in a solar magnetic pore. High cadence images were obtained simultaneously across four wavelength bands using the Dunn Solar Telescope. Employing Fourier and wavelet techniques, sausage-mode oscillations displaying significant power were detected in both intensity and area fluctuations. The intensity and area fluctuations exhibit a range of periods from 181 to 412 s, with an average period similar to 290 s, consistent with the global p-mode spectrum. Intensity and area oscillations present in adjacent bandpasses were found to be out of phase with one another, displaying phase angles of 6 degrees.12, 5 degrees.82, and 15 degrees.97 between the 410 angstrom continuum-G-band, G-band-Na I D1, and Na I D-1-Ca II K heights, respectively, reiterating the presence of upwardly propagating sausage-mode waves. A phase relationship of similar to 0 degrees between same-bandpass emission and area perturbations of the pore best categorizes the waves as belonging to the "slow" regime of a dispersion diagram. Theoretical calculations reveal that the waves are surface modes, with initial photospheric energies in excess of 35,000 W m(-2). The wave energetics indicate a substantial decrease in energy with atmospheric height, confirming that magnetic pores are able to transport waves that exhibit appreciable energy damping, which may release considerable energy into the local chromospheric plasma.