MAGNETIC ENERGY PARTITION BETWEEN THE CORONAL MASS EJECTION AND FLARE FROM AR 11283
MAGNETIC ENERGY PARTITION BETWEEN THE CORONAL MASS EJECTION AND FLARE FROM AR 11283
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日冕物质抛射和 AR 11283 耀斑之间的磁能分配
DOI：
10.1088/0004-637x/765/1/37
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发表时间：
2013-02
影响因子：
4.9
通讯作者：
Gan W. Q.
中科院分区：
文献类型：
--
作者：
Feng L.;Wiegelmann T.;Su Y.;Inhester B.;Li Y. P.;Sun X. D.;Gan W. Q.
2011年9月6日，在地球上观测到一个X级耀斑和一个日冕物质抛射（CME），从同一个活动区AR 11283爆发。研究了它们之间的磁能分配。SDO/HMI矢量磁图被用来获得日冕磁场使用非线性无力场（NLFFF）外推法。计算了耀斑前后的自由磁能，以估计耀斑和CME释放的能量。对于耀斑能量学，热能量和非热能量的推导使用RHESSI和GOES数据。为了获得辐射输出，使用0.1 - 37 nm波段的SDO/EVE数据。我们从STEREO-A、B和SOHO观测到的日冕物质抛射图像重建了日冕物质抛射的三维（3D）外围。质量的计算是基于一个更精确的汤姆逊散射几何。随后对CME的动能和势能的估计利用了更准确的质量，以及3D框架中的高度和速度。由NLFFF模型得到的释放自由磁能约为6.4 × 1031 erg，其上限可能为1.8 × 1032 erg。该事件的热能和非热能都低于SDO/EVE的2.2 × 10~（31）erg辐射输出。覆盖整个太阳光谱的总辐射可能要大几倍。CME的动能和势能之和可达6.5 × 1031erg。因此，自由能能够为AR 11283中的耀斑和CME提供动力。在不确定性范围内，耀斑和日冕物质抛射可能消耗类似的自由能。
On 2011 September 6, an X-class flare and a halo coronal mass ejection (CME) were observed from Earth erupting from the same active region AR 11283. The magnetic energy partition between them has been investigated. SDO/HMI vector magnetograms were used to obtain the coronal magnetic field using the nonlinear force-free field (NLFFF) extrapolation method. The free magnetic energies before and after the flare were calculated to estimate the released energy available to power the flare and the CME. For the flare energetics, thermal and nonthermal energies were derived using the RHESSI and GOES data. To obtain the radiative output, SDO/EVE data in the 0.1–37 nm waveband were utilized. We have reconstructed the three-dimensional (3D) periphery of the CME from the coronagraph images observed by STEREO-A, B, and SOHO. The mass calculations were then based on a more precise Thomson-scattering geometry. The subsequent estimate of the kinetic and potential energies of the CME took advantage of the more accurate mass, and the height and speed in a 3D frame. The released free magnetic energy resulting from the NLFFF model is about 6.4 × 1031 erg, which has a possible upper limit of 1.8 × 1032 erg. The thermal and nonthermal energies are lower than the radiative output of 2.2 × 1031 erg from SDO/EVE for this event. The total radiation covering the whole solar spectrum is probably a few times larger. The sum of the kinetic and potential energy of the CME could go up to 6.5 × 1031 erg. Therefore, the free energy is able to power the flare and the CME in AR 11283. Within the uncertainty, the flare and the CME may consume a similar amount of free energy.
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影响因子：
6.5
作者：
E. P. Kontar;A. MacKinnon;R. Schwartz;JOHN C. Brown
通讯作者：
E. P. Kontar;A. MacKinnon;R. Schwartz;JOHN C. Brown
根据 SECCHI COR 数据对极地射流进行粒子动力学分析
DOI：
10.1051/0004-6361/201117071
发表时间：
2011-12
期刊：
Astronomy & Astrophysics
影响因子：
--
作者：
Feng, L.;Inhester, B.;de Patoul, J.;Wiegelmann, T.;Gan, W. Q.
通讯作者：
Gan, W. Q.
影响因子：
--
作者：
A. Emslie;H. Kucharek;B. Dennis;N. Gopalswamy;G. Holman;G. Share;A. Vourlidas;T. Forbes;P. Gallagh
通讯作者：
A. Emslie;H. Kucharek;B. Dennis;N. Gopalswamy;G. Holman;G. Share;A. Vourlidas;T. Forbes;P. Gallagh
影响因子：
5.2
作者：
T. Woods;F. Eparvier;J. Fontenla;J. Harder;G. Kopp;W. McClintock;G. Rottman;B. Smiley;M. Snow-M.-S
通讯作者：
T. Woods;F. Eparvier;J. Fontenla;J. Harder;G. Kopp;W. McClintock;G. Rottman;B. Smiley;M. Snow-M.-S
DOI：
10.1086/427274
发表时间：
2005-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Veronig;John C. Brown;B. R. Dennis;Richard A. Schwartz;L. Sui;A. Tolbert
通讯作者：
A. Veronig;John C. Brown;B. R. Dennis;Richard A. Schwartz;L. Sui;A. Tolbert