J/ApJ/797/50ivo://CDS.VizieR/J/ApJ/797/50doi:10.26093/cds/vizier.17970050CDSAschwanden M.J.Xu Y.Jing J.2015-09-04T12:10:35Z2015-08-24T14:00:33ZCDS support team

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

cds-question@unistra.frthe-sunmagnetic-fieldsultraviolet-astronomyWe present the first part of a project on the global energetics of solar flares and coronal mass ejections that includes about 400 M- and X-class flares observed with Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). We calculate the potential (E_p_), the nonpotential (E_np_) or free energies (E_free_=E_np_-E_p_), and the flare-dissipated magnetic energies (E_diss_). We calculate these magnetic parameters using two different NLFFF codes: the COR-NLFFF code uses the line-of-sight magnetic field component B_z_ from HMI to define the potential field, and the two-dimensional (2D) coordinates of automatically detected coronal loops in six coronal wavelengths from AIA to measure the helical twist of coronal loops caused by vertical currents, while the PHOT-NLFFF code extrapolates the photospheric three-dimensional (3D) vector fields. We find agreement between the two codes in the measurement of free energies and dissipated energies within a factor of <~3. The size distributions of magnetic parameters exhibit powerlaw slopes that are approximately consistent with the fractal-diffusive self-organized criticality model. The magnetic parameters exhibit scaling laws for the nonpotential energy, E_np_{propto}E_p_^1.02^, for the free energy, E_free_{propto}E_p_^1.7^ and E_free_{propto}B_{phi}_^1.0^L^1.5^, for the dissipated energy, E_diss_{propto}E_p_^1.6^ and E_diss_{propto}E_free_^0.9^ , and the energy dissipation volume, V{propto}E_diss_^1.2^. The potential energies vary in the range of E_p_=1x10^31^-4x10^33^erg, while the free energy has a ratio of E_free_/E_p_{approx}1%-25%. The Poynting flux amounts to F_flare_{approx}5x10^8^-10^10^erg/cm2/s during flares, which averages to F_AR_{approx}6x10^6^erg/cm2/s during the entire observation period and is comparable with the coronal heating rate requirement in active regions.2014ApJ...797...50Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/797/50CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/802/53 : Global energetics of solar flares. II. (Aschwanden+, 2015)J/A+A/574/A37 : Movies of 2012-10-16 solar flare (Dalmasse+, 2015)J/ApJ/774/L27 : Solar flares predictors (Yang+, 2013)J/ApJ/759/69 : Solar electron events (1995-2005) with WIND/3DP (Wang+, 2012)J/ApJ/757/94 : Solar flares observed with GOES and AIA (Aschwanden, 2012)J/ApJ/747/L41 : Solar flares probabilities (Bloomfield+, 2012)J/A+A/304/563 : Cool X-ray flares of Sun with GOES (Phillips+, 1995)http://aia.lmsal.com/ : Atmospheric Imaging Assembly home pagehttp://www.lmsal.com/~aschwand/RHESSI/flare_energetics.html : Global Flarehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/797/50https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/797/50http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/797/50https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/797/50https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/797/50http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/797/50GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVdefaultJ/ApJ/797/50/table3Magnetic energy parameters calculated with the COR-NLFFF code for 172 M and X-class flares wuth a longitude difference of <45 degrees to the central meridianSeq[3/399] Solar flare numbermeta.id;meta.mainintprimaryFlDate of flare startstime.epochnullableClGOES class (M1-X5.4)src.classcharPosHeliographic positionmeta.notecharAngle[1/8] Magnetic field misalignment angle {mu}degstat.fit.paramfloatEp[85/3949] Potential energy; 10^+30^erg1e+23Jstat.fit.paraminte_Ep[3/788] Uncertainty in Ep1e+23Jstat.errorintEfree[1/951] Free energy; 10^+30^erg1e+23Jphys.energyinte_Efree[0/324] Uncertainty in Efree1e+23Jstat.errorintRatio[0/0.9] Energy ratio; Efree/Epphys.energyfloatEdiss[0/1546] Dissipated energy; 10^+30^erg1e+23Jphys.energyinte_Ediss[0/224] Uncertainty in Ediss1e+23Jstat.errorintPdiss[0/1021] Peak dissipation rate; in 10^+30^erg/0.2hr unit1.39e+20Wphys.energyinte_Pdiss[0/222] Uncertainty in Pdisstat.errorintL[0/236] Length scale (in 1000km)Mmsrc.morph.scLengthinte_L[0/16] Uncertainty in LMmstat.errorintT[0.08/4.1] Durationhtime.intervalfloatpPDisplay data from previous papers (Aschwanden et al. 2012, J/ApJ/757/94 and 2015, J/ApJ/802/53) for this positionmeta.ref.urlintnullable