太阳耀斑环——射电微波及相关波段的研究
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摘要
与大多以光学波段为主的耀斑研究不同的是,作者拟以射电微波(厘米波段)的频谱和成像观测为主及相应的辐射机制研究太阳活动的基本单元——耀斑环及其物理参数的空间分布和时间演化规律。特别是中国研制的具有国际最高的时间、空间和频率分辨率的射电日像仪(MUSER)已投入运行,文章将为推动该设备即将开展的科学研究提供重要的参考工具。此外,文中也加入了与射电微波辐射密切相关的X射线、紫外和光学波段的研究,符合太阳物理乃至整个天体物理多波段研究的大趋势。文章集中介绍作者最具特色的研究,由于篇幅所限只能给出基本物理思想和概念、主要结论和代表性插图,对相应的理论推导、观测数据处理等细节,读者可根据需要参阅对应的参考文献。
Different from most flare studies based on observations in the optical band,this paper focuses on the elementary units of solar activity —— flaring loops and physical parameters that vary in time and space, as observed by radio microwave(cm band) spectra and images. In particular, this paper will be an important reference for studies on the data collected by a new radio heliograph(MUSER) built in China, which has the highest time, space, and frequency resolutions to date. In addition, X-ray, EUV, and optical studies related to microwave emission are included, in accordance with the trend of multiple wavelength research in all the various fields of astrophysics, including solar physics. Only the most representative studies, the ideas, main conclusions and typical figures are mentioned; for detailed data analysis and theoretical derivations, readers can look up the original references.
Different from most flare studies based on observations in the optical band,this paper focuses on the elementary units of solar activity —— flaring loops and physical parameters that vary in time and space, as observed by radio microwave(cm band) spectra and images. In particular, this paper will be an important reference for studies on the data collected by a new radio heliograph(MUSER) built in China, which has the highest time, space, and frequency resolutions to date. In addition, X-ray, EUV, and optical studies related to microwave emission are included, in accordance with the trend of multiple wavelength research in all the various fields of astrophysics, including solar physics. Only the most representative studies, the ideas, main conclusions and typical figures are mentioned; for detailed data analysis and theoretical derivations, readers can look up the original references.
引文
[1]方成,丁明德,陈鹏飞.太阳活动区物理.南京:南京大学出版社,2008
[2]谭宝林,程俊,谭程明等.天文学报,2018,59:37-1
[3] Yan Y,Zhang J,Wang W et al. EM&P,2009,104:97
[4] Nakajima H,Nishio M,Enome S et al. Proc. IEEE,1994,82:705
[5]黄光力.等离子体动力学及其在太阳物理中的应用——现代太阳物理丛书.北京:科学出版社,2009
[6]黄光力,Melnikov V F,季海生等.耀斑环物理.北京:科学出版社,2016
[7] Huang G L,Melnikov V F,Ji H S et al. Solar Flare Loops:Observations and Interpretations. Singapore:Springer,jointly with Beijing:Science Press,2018
[8] Dulk G A. Annual Rev. Astron. Astrophys.,1985,23:169
[9] Ramaty R. Astrophys. J.,1969,158:753
[10] Melnikov V F,Gorbikov S P,Pyatakov N P. Formation of anisotropic distributions of mildly relativistic electrons in flaring loops. Proceedings of the International Astronomical Union,IAU Symposium,2009,Volume 257,p. 323-328
[11] Fleishman G D,Kuznetsov A A. Astrophys. J.,2010,721:1127
[12] Zhou A H,Li J P,Wang X D. Research in Astron. and Astrophys.,2016,16:31
[13] Melnikov V F,Gary D E,Nita G M. Solar Phys.,2008,253:43
[14] Charbonneau P,McIntosh S W,Liu H L et al. Solar Phys.,2001,203:321
[15] Song Q,Huang G,Tan B. Astrophys. J.,2012,750:160
[16] Song Q,Huang G,Huang Y. Astrophys. Space Sci.,2013,347:15
[17] Huang G L,Nakajima H. Astrophys. J.,2009,696:136
[18] Melnikov V F,Shibasaki K,Reznikova V E. Astrophys. J.,2002,580:L185
[19] Huang G L,Song Q W,Huang Y. Astrophys. J.,2010,723:1806
[20] Song Q W,Huang G L,Nakajima H. Astrophys. J.,2011,734:113
[21] Metcalf T R,Alexander D. Astrophys. J.,1999,522:1108
[22] Huang G,Song Q,Li J. Astrophys. Space Sci.,2013,345:41
[23] Cohen M H. Astrophys. J.,1960,131:664
[24] Brown J. Solar Phys.,1972,26:441
[25] Huang G L. Solar Phys.,2009,257:323
[26] Huang G L. New Astron.,2007,12:483
[27] Melnikov V F,Charikov Y E,Kudryavtsev I V. Geomagn.Aeron.,2015,55:983
[28] Shao C,Huang G. Astrophys. J.,2009,691:299
[29] Huang G L,Li J P. Astrophys. J.,2011,740:46
[30]黄光力.日冕磁场的射电诊断,10000个科学难题——天文学卷.北京:科学出版社,2010. 59
[31] Dulk G A,Marsh K A. Astrophys. J.,1982,259:350
[32] Zhou A H,Karlicky M. Solar Phys.,1994,153:441
[33] Huang G L. Solar Phys.,2006,237:173
[34] Huang G L,Li J P,Song Q W. Research in Astron. Astrophys.,2013,13:215
[35] Kontar E P,MacKinnon A L,Schwartz R A et al. Astron. Astrophys.,2006,446:1157
[36]韩钢,李友平,甘为群.天文学报,2008,49:403
[37] Gan W Q,Li Y P,Chang J. Astrophys. J.,2001,552:858
[38] Huang G L. Solar Phys.,2000,196:395
[39] Zhang J,Huang G L. Astrophys. J.,2003,592:L49
[40] Ji H,Wang H,Goode P R et al. Astrophys. J.,2004,607:L55
[41] Ji H,Huang G,Wang H et al. Astrophys. J.,2006,636:L173
[42] Ji H,Wang H,Liu C et al. Astrophys. J.,2008,680:734
[43] Li Y P,Gan W Q. Astrophys. J.,2005,629:L137
[44] Reznikova V E,Melnikov V F,Shibasaki K et al. Astrophys. J.,2009,697:735
[45] Nakariakov V M,Melnikov V F. Space Science Rev.,2009,149:119
[46] Sturrock P A,Kaufmann P,Moore R L et al. Solar Phys.,1984,94:341
[47] Huang G,Song Q. Solar Phys.,2010,264:345
[48] Huang G L,Lin J. Astrophys. J.,2006,639:L99
[49] Ning Z,Cao W. Astrophys. J.,2010,717:1232
[50] Zhang Q M,Li D,Ning Z J et al. Astrophys. J.,2016,827:27
[2]谭宝林,程俊,谭程明等.天文学报,2018,59:37-1
[3] Yan Y,Zhang J,Wang W et al. EM&P,2009,104:97
[4] Nakajima H,Nishio M,Enome S et al. Proc. IEEE,1994,82:705
[5]黄光力.等离子体动力学及其在太阳物理中的应用——现代太阳物理丛书.北京:科学出版社,2009
[6]黄光力,Melnikov V F,季海生等.耀斑环物理.北京:科学出版社,2016
[7] Huang G L,Melnikov V F,Ji H S et al. Solar Flare Loops:Observations and Interpretations. Singapore:Springer,jointly with Beijing:Science Press,2018
[8] Dulk G A. Annual Rev. Astron. Astrophys.,1985,23:169
[9] Ramaty R. Astrophys. J.,1969,158:753
[10] Melnikov V F,Gorbikov S P,Pyatakov N P. Formation of anisotropic distributions of mildly relativistic electrons in flaring loops. Proceedings of the International Astronomical Union,IAU Symposium,2009,Volume 257,p. 323-328
[11] Fleishman G D,Kuznetsov A A. Astrophys. J.,2010,721:1127
[12] Zhou A H,Li J P,Wang X D. Research in Astron. and Astrophys.,2016,16:31
[13] Melnikov V F,Gary D E,Nita G M. Solar Phys.,2008,253:43
[14] Charbonneau P,McIntosh S W,Liu H L et al. Solar Phys.,2001,203:321
[15] Song Q,Huang G,Tan B. Astrophys. J.,2012,750:160
[16] Song Q,Huang G,Huang Y. Astrophys. Space Sci.,2013,347:15
[17] Huang G L,Nakajima H. Astrophys. J.,2009,696:136
[18] Melnikov V F,Shibasaki K,Reznikova V E. Astrophys. J.,2002,580:L185
[19] Huang G L,Song Q W,Huang Y. Astrophys. J.,2010,723:1806
[20] Song Q W,Huang G L,Nakajima H. Astrophys. J.,2011,734:113
[21] Metcalf T R,Alexander D. Astrophys. J.,1999,522:1108
[22] Huang G,Song Q,Li J. Astrophys. Space Sci.,2013,345:41
[23] Cohen M H. Astrophys. J.,1960,131:664
[24] Brown J. Solar Phys.,1972,26:441
[25] Huang G L. Solar Phys.,2009,257:323
[26] Huang G L. New Astron.,2007,12:483
[27] Melnikov V F,Charikov Y E,Kudryavtsev I V. Geomagn.Aeron.,2015,55:983
[28] Shao C,Huang G. Astrophys. J.,2009,691:299
[29] Huang G L,Li J P. Astrophys. J.,2011,740:46
[30]黄光力.日冕磁场的射电诊断,10000个科学难题——天文学卷.北京:科学出版社,2010. 59
[31] Dulk G A,Marsh K A. Astrophys. J.,1982,259:350
[32] Zhou A H,Karlicky M. Solar Phys.,1994,153:441
[33] Huang G L. Solar Phys.,2006,237:173
[34] Huang G L,Li J P,Song Q W. Research in Astron. Astrophys.,2013,13:215
[35] Kontar E P,MacKinnon A L,Schwartz R A et al. Astron. Astrophys.,2006,446:1157
[36]韩钢,李友平,甘为群.天文学报,2008,49:403
[37] Gan W Q,Li Y P,Chang J. Astrophys. J.,2001,552:858
[38] Huang G L. Solar Phys.,2000,196:395
[39] Zhang J,Huang G L. Astrophys. J.,2003,592:L49
[40] Ji H,Wang H,Goode P R et al. Astrophys. J.,2004,607:L55
[41] Ji H,Huang G,Wang H et al. Astrophys. J.,2006,636:L173
[42] Ji H,Wang H,Liu C et al. Astrophys. J.,2008,680:734
[43] Li Y P,Gan W Q. Astrophys. J.,2005,629:L137
[44] Reznikova V E,Melnikov V F,Shibasaki K et al. Astrophys. J.,2009,697:735
[45] Nakariakov V M,Melnikov V F. Space Science Rev.,2009,149:119
[46] Sturrock P A,Kaufmann P,Moore R L et al. Solar Phys.,1984,94:341
[47] Huang G,Song Q. Solar Phys.,2010,264:345
[48] Huang G L,Lin J. Astrophys. J.,2006,639:L99
[49] Ning Z,Cao W. Astrophys. J.,2010,717:1232
[50] Zhang Q M,Li D,Ning Z J et al. Astrophys. J.,2016,827:27