J/ApJ/752/126ivo://CDS.VizieR/J/ApJ/752/126doi:10.26093/cds/vizier.17520126CDSYamamoto T.T.Kusano K.2014-03-17T15:56:40Z2014-03-04T09:55:44ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-sunmagnetic-fieldsNonlinear force-free field (NLFFF) extrapolation is a powerful tool for the modeling of the magnetic field in the solar corona. However, since the photospheric magnetic field does not in general satisfy the force-free condition, some kind of processing is required to assimilate data into the model. In this paper, we report the results of new preprocessing for the NLFFF extrapolation. Through this preprocessing, we expect to obtain magnetic field data similar to those in the chromosphere. In our preprocessing, we add a new term concerning chromospheric longitudinal fields into the optimization function proposed by Wiegelmann et al (2006SoPh..233..215W). We perform a parameter survey of six free parameters to find minimum force- and torque-freeness with the simulated-annealing method. Analyzed data are a photospheric vector magnetogram of AR 10953 observed with the Hinode spectropolarimeter and a chromospheric longitudinal magnetogram observed with SOLIS spectropolarimeter. It is found that some preprocessed fields show the smallest force- and torque-freeness and are very similar to the chromospheric longitudinal fields. On the other hand, other preprocessed fields show noisy maps, although the force- and torque-freeness are of the same order. By analyzing preprocessed noisy maps in the wave number space, we found that small and large wave number components balance out on the force-free index. We also discuss our iteration limit of the simulated-annealing method and magnetic structure broadening in the chromosphere.2012ApJ...752..126Yhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/752/126CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJS/169/439 : Models of solar magnetic structures (Socas-Navarro, 2007)J/A+A/432/1063 : Analysis of inner solar corona in EUV (Lanzafame+, 2005)http://solis.nso.edu/ : National Solar Observatory NISP/SOLIShttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/752/126https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/752/126http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/752/126https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/752/126https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/752/126http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/752/126GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/752/126/table1Free parameter pairsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNum[0/85] Parameter combination numbermeta.idintlogt0[-4/2] Log of coefficient of the initial pseudo temperature; T_init_=t0*L_init_stat.fit.paramintdT[995/0.9995] Temperature cooling factor: new T = old T * dTstat.fit.paramfloatlogmu3Log of coefficient of L3stat.fit.paramintlogmu4Log of coefficient of L4stat.fit.paramintlogmu5Log of coefficient of L5 (See equation (20))stat.fit.paramintSeed[3/259] Random number seedstat.fit.paramintcnv[0/1] Calculation convergence code; 1=convergedmeta.codeintr1Ratio of L1_init_/L1_finish_stat.fit.paramdoubler5Ratio of L5_init_/L5_finish_stat.fit.paramdouble