[1] |
Irons F E. The escape factor in plasma spectroscopy-I. The escape factor defined and evaluated[J]. J. Quant. Spectrosc. Radiat. Trans., 1979, 22(1):1-20
|
[2] |
Guo Ce, Xue Bingsen, Lin Zhaoxiang. Study for prediction method of X-ray flare characteristic parameters[J]. Chin. J. Space Sci., 2012, 32(6):771-777. In Chinese (郭策, 薛炳森, 林兆祥. 太阳X射线耀斑特征参数预报 方法研究[J]. 空间科学学报, 2012, 32(6):771-777)
|
[3] |
Sun Weiying, Wu Ji. The study on bremsstrahlung of plasma in 1AU during quiet Sun and solar flare period[J]. Chin. J. Space Sci., 2004, 24(6):412-420. In Chinese (孙伟英, 吴季. 太阳宁静及耀斑期间1AU附近等离子体轫 致辐射研究[J]. 空间科学学报, 2004, 24(6):412-420)
|
[4] |
Lin Huaan. The evolution of hard x-Ray energy spectrum in solar flares[J]. Chin. J. Space Sci., 1999, 19(4):295-300. In Chinese (林华安. 太阳耀斑硬X射线能谱演 变特征[J]. 空间科学学报, 1999, 19(4):295-300)
|
[5] |
Rugge H R, McKenzie D L. X-ray line ratios for FeV!I!I observed in the solar coronal[J]. Astrophys. J., 1985, 297:338-346
|
[6] |
Waljeski K, Moses D, Dere K P, et al. The composition of a coronal active region[J]. Astrophys. J., 1994, 429(2):909-923
|
[7] |
Wattaker D S, Tallents G J. Iron opacity predictions under solar interior conditions[J]. Mon. Notic. Roy. Astron. Soc., 2009, 400(4):1808-1813
|
[8] |
Brichhouse N S, Schmelz J T. The transparency of solar coronal active regions[J]. Astrophys. J. Lett., 2006, 636(1):L53-L56
|
[9] |
Schmelz J T, Saba J L R, Strong K T. Resonance scattering of Fe XVⅡ-A density diagnostic[J]. Astrophys. J., 1992, 398:L115-L118
|
[10] |
Meyer J P. The baseline composition of solar energetic particles[J]. Astrophys. J., 1985, 57(Supp.S):151-171
|
[11] |
Schmeiz J T, Saba J L R, Chuavin J C, et al. Investigation the effect of opacity in soft x-Ray spectral lines emitted by solar coronal active regions[J]. Astrophys. J., 1997, 477:509-515
|
[12] |
Keenan F P, Kingston A E. An approximate calculation of the effect of opacity on SiⅢ emission line ratios near the solar limb[J]. Mon. Notic. Roy. Astron. Soc., 1986, 220:493-500
|
[13] |
Kastner S O, Bhatia A K. Half-widths, escape probabilities and intensity factors of opacity-broadened Doppler- and Voigt-profile lines[J]. J. Quant. Spectrosc. Radiat. Trans., 1997, 58(2):217-231
|
[14] |
He J, Zhang Q G. Calculation of the effect of opacity in the solar spectral lines of carbon ions[J]. Adv. Space Res., 2013, 51:2002-2009
|
[15] |
Saba J L R, Schmelz J T, Bhatia A K, et al. Fe XVⅡ soft s-Ray lines: theory and data comparisons[J]. Astrophys. J., 1999, 510:1064-1077
|
[16] |
He J, Liao L L. The opacity of the solar spectral lines of CⅡ 133.5nm[J]. Spectr. Lett., 2012, 45(6):452-457
|
[17] |
Doyle J G, Mcwhirter R W P. An approximate calculation of the effect of opacity in the solar spectral lines of CⅢ[J]. Mon. Notic. Roy. Astron. Soc., 1980, 193:947-955
|