Full-Text Search:
Home|Journal Papers|About CNKI|User Service|FAQ|Contact Us|中文
《天文和天体物理学研究(英文版)》 2014-02
Add to Favorite Get Latest Update

On the line profile changes observed during the X2.2 class flare in the active region NOAA 11158

Ankala Raja Bayanna;Brajesh Kumar;Parameswaran Venkatakrishnan;Shibu Kunchandy Mathew;Belur Ravindra;Savita Mathur;Rafael A Garcia;Udaipur Solar Observatory,Physical Research Laboratory,Dewali,Badi Road,Udaipur 313 004,India;Indian Institute of Astrophysics,II Block,Koramangla,Bangalore 560034,India;Space Science Institute,4750 Walnut Street Suite#205,Boulder,CO 80301,USA;Laboratoire AIM,CEA/DSM-CNRS,Universit′e Paris 7 Diderot,IRFU/SAp,Centre de Saclay,91191,Gif-sur-Yvette,France;  
The solar active region NOAA 11158 produced a series of flares during its passage through the solar disk.The first major flare(of class X2.2) of the current solar cycle occurred in this active region on 2011 February 15 around 01:50 UT.We have analyzed the Dopplergrams and magnetograms obtained by the Helioseismic and Magnetic Imager(HMI) instrument onboard Solar Dynamics Observatory to examine the photospheric velocity and magnetic field changes associated with this flare.The HMI instrument provides high-quality Doppler and magnetic maps of the solar disk with 0.5 spatial scale at a cadence of 45 s along with imaging spectroscopy.We have identified five locations of velocity transients in the active region during the flare.These transient velocity signals are located in and around the flare ribbons as observed by Hinode in the Ca II H wavelength and the footpoints of hard X-ray enhancement are in the energy range 12–25 keV from RHESSI.The changes in shape and width of two circular polarization states have been observed at the time of transients in three out of five locations.Forward modeling of the line profiles shows that the change in atmospheric parameters such as magnetic field strength,Doppler velocity and source function could explain the observed changes in the line profiles with respect to the pre-flare condition.
【Fund】: support from the NASA grant NNX12AE17G.R.A.;; the support of the GOLF CNES grant at the SAp/CEA-Saclay
【CateGory Index】: P182.52
Download(CAJ format) Download(PDF format)
CAJViewer7.0 supports all the CNKI file formats; AdobeReader only supports the PDF format.
【Co-citations】
Chinese Journal Full-text Database 10 Hits
1 Guo Jianpeng 1,2) Yan Yihua 1) Yang Zhiliang 2) ( 1)National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; 2)Department of Astronomy, Beijing Normal University, 100875, Beijing, China);RADIO, HXR AND EUV MULTIWAVELENGTH ANALYSIS FOR A SOLAR FLARE EVENT ON 13 JUNE 2003[J];Journal of Beijing Normal University(Natural Science);2005-03
2 QIAN Lu-lu 1,2,XIANGLI Bin 1,2,L Qun-bo 2,ZHOU Zhi-liang 2,FU Qiang 2 1.Department of Precision Machinery and Precision Instrumentation,University of Science and Technology of China,Hefei 230026,China 2.Key Laboratory of Computational Optical Imaging Technology,Academy of Opto-Electronics,Chinese Academy of Sciences,Beijing 100094,China;Imaging Quality Evaluation of Computational Imaging Spectrometry[J];Spectroscopy and Spectral Analysis;2013-07
3 DENG YuanYong & ZHANG HongQi Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;Progress in Space Solar Telescope[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
4 NING ZongJun Purple Mountain Observatory, Nanjing 210008, China;The investigation of the Neupert effect in two solar flares[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
5 ZHANG Jun & JIN ChunLan National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;Emergence and cancellation of small-scale magnetic flux in a quiet region[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
6 LI YiXuan, JING Ju, TAN ChangYi & WANG HaiMin Center for Solar-Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07102, USA;The change of magnetic inclination angles associated with the X3.4 flare on December 13, 2006[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
7 WANG Dong1, ZHANG Mei1, LI Hui2 & ZHANG HongQi1 1 Key Laboratory of Solar Activity, National Astronomical Observatory, Chinese Academy of Sciences, Beijing 100012, China; 2 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China;A comparison of co-temporal magnetograms obtained with the Huairou magnetograph and the Spectro-Polarimeter on board Hinode[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
8 HAO Juan & ZHANG Mei Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;The influence of the stray-light component in determining coronal temperature structures[J];中国科学(G辑:物理学 力学 天文学)(英文版);2009-11
9 ZHANG Ping1,2*,FANG Cheng1,2 & ZHANG QingMin1,2 1 School of Astronomy and Space Science,Nanjing University,Nanjing 210093,China;2 Key Lab of Modern Astronomy and Astrophysics,Nanjing University,Ministry of Education,Nanjing 210093,China;Hαcounterparts of X-ray bright points in the solar atmosphere[J];中国科学:物理学 力学 天文学(英文版);2012-05
10 NING ZongJun1,2 1Key Laboratory of Dark Matter and Space Astronomy,Chinese Academy of Sciences,Nanjing 210008,China; 2 Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China;Power conversion factor in solar flares[J];科学通报(英文版);2012-12
©2006 Tsinghua Tongfang Knowledge Network Technology Co., Ltd.(Beijing)(TTKN) All rights reserved