{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360005744498154752.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4365/ab64f2"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4365/ab64f2/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4365/ab64f2"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1912.10626"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"A Magnetohydrodynamic Relaxation Method for Non-force-free Magnetic Field in Magnetohydrostatic Equilibrium"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>A nonlinear force-free field (NLFFF) extrapolation is widely used to reconstruct the three-dimensional magnetic field in the solar corona from the observed photospheric magnetic field. However, the pressure gradient and gravitational forces are ignored in the NLFFF model, even though the photospheric and chromospheric magnetic fields are not in general force-free. Here we develop a magnetohydrodynamic (MHD) relaxation method that reconstructs the solar atmospheric (chromospheric and coronal) magnetic field as a non-force-free magnetic field (NFFF) in magnetohydrostatic equilibrium where the Lorentz, pressure gradient, and gravitational forces are balanced. The system of basic equations for the MHD relaxation method is derived, and mathematical properties of the system are investigated. A robust numerical solver for the system is constructed based on the modern high-order shock capturing scheme. Two-dimensional numerical experiments that include the pressure gradient and gravitational forces are also demonstrated.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380005744498154755","@type":"Researcher","foaf:name":[{"@value":"Takahiro Miyoshi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005744498154627","@type":"Researcher","foaf:name":[{"@value":"Kanya Kusano"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005744498154628","@type":"Researcher","foaf:name":[{"@value":"Satoshi Inoue"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00670049"},{"@type":"EISSN","@value":"15384365"}],"prism:publicationName":[{"@value":"The Astrophysical Journal Supplement Series"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2020-02-20","prism:volume":"247","prism:number":"1","prism:startingPage":"6"},"reviewed":"false","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/1538-4365/ab64f2/pdf"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4365/ab64f2"}],"createdAt":"2020-02-20","modifiedAt":"2024-01-17","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Solar%20and%20Stellar%20Astrophysics","dc:title":"Astrophysics - Solar and Stellar Astrophysics"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20and%20Stellar%20Astrophysics%20(astro-ph.SR)","dc:title":"Solar and Stellar Astrophysics (astro-ph.SR)"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781833807488","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"15H05814"},{"@type":"JGN","@value":"JP15H05814"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PLANNED-15H05814/"}],"notation":[{"@language":"ja","@value":"太陽嵐の発生機構の解明と予測"},{"@language":"en","@value":"Understanding and prediction of the solar storm"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360011142937142400","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Extrapolation of a nonlinear force-free field containing a highly twisted magnetic loop"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011142938818560","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FORCED FIELD EXTRAPOLATION: TESTING A MAGNETOHYDRODYNAMIC (MHD) RELAXATION METHOD WITH A FLUX-ROPE EMERGENCE MODEL"}]},{"@id":"https://cir.nii.ac.jp/crid/1360290617473116800","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references","isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Solar force-free magnetic fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292617906630144","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Preprocessing of Vector Magnetograph Data for a Nonlinear Force-Free Magnetic Field Reconstruction"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292617915503744","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"An optimization principle for the computation  of MHD equilibria in the solar corona"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292617916807808","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Nonlinear Force-Free Modeling of Coronal Magnetic Fields. II. Modeling a Filament Arcade and Simulated Chromospheric and Photospheric Vector Fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292619105541632","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A CRITICAL ASSESSMENT OF NONLINEAR FORCE-FREE FIELD MODELING OF THE SOLAR CORONA FOR ACTIVE REGION 10953"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565167378412160","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"NONLINEAR FORCE-FREE EXTRAPOLATION OF THE CORONAL MAGNETIC FIELD BASED ON THE MAGNETOHYDRODYNAMIC RELAXATION METHOD"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574092885149312","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Nonlinear Force-Free Modeling of Coronal Magnetic Fields Part I: A Quantitative Comparison of Methods"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574092886386432","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"An Optimization Approach to Reconstructing Force‐free Fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574092893656192","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Optimization code with weighting function for the reconstruction of coronal magnetic fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567860051456","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A Magnetostatic Grad–Rubin Code for Coronal Magnetic Field Extrapolations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567864468480","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Hyperbolic Divergence Cleaning for the MHD Equations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567868100992","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Well posed reconstruction of \n the solar coronal magnetic field"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567868594560","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The ∇·B=0 Constraint in Shock-Capturing Magnetohydrodynamics Codes"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855568612181632","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Magneto-static Modeling from Sunrise/IMaX: Application to an Active Region Observed with Sunrise II"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855570977156224","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MAGNETO-STATIC MODELING OF THE MIXED PLASMA BETA SOLAR ATMOSPHERE BASED ON SUNRISE/IMaX DATA"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520284947328","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A Fixed-point Scheme for the Numerical Construction of Magnetohydrostatic Atmospheres in Three Dimensions"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981470211754752","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Preprocessing of solar vector magnetograms for force-free magnetic field extrapolation"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981470622195456","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A High-order Weighted Finite Difference Scheme with a Multistate Approximate Riemann Solver for Divergence-free Magnetohydrodynamic Simulations"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981471120403584","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Nonlinear Force‐free Field Modeling of a Solar Active Region around the Time of a Major Flare and Coronal Mass Ejection"}]},{"@id":"https://cir.nii.ac.jp/crid/1362262944740115072","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"On the Extrapolation of Magnetohydrostatic Equilibria on the Sun"}]},{"@id":"https://cir.nii.ac.jp/crid/1362262945641908992","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FORCED FIELD EXTRAPOLATION OF THE MAGNETIC STRUCTURE OF THE Hα FIBRILS IN THE SOLAR CHROMOSPHERE"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107368271606144","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Three-dimensional structures of magnetostatic atmospheres. III - A general formulation"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107369330106496","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Is the solar chromospheric magnetic field force-free?"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107370539975168","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Strong Stability-Preserving High-Order Time Discretization Methods"}]},{"@id":"https://cir.nii.ac.jp/crid/1363107371028268416","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Plasma Beta above a Solar Active Region: Rethinking the Paradigm"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388843909117696","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Calculation of force-free magnetic field with non-constant ?"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670320681544320","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A 3D code for MHD equilibrium and stability"}]},{"@id":"https://cir.nii.ac.jp/crid/2050588892104455680","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"PSTEP : project for solar–terrestrial environment prediction"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.3847/1538-4365/ab64f2"},{"@type":"KAKEN","@value":"PRODUCT-22828483"},{"@type":"OPENAIRE","@value":"doi_dedup___::56a975978c00d8d14341db90b191c9e1"},{"@type":"CROSSREF","@value":"10.1007/s41116-020-00027-4_references_DOI_Xdh59anGlczmCXzFUlQrxGXL1p6"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01486-1_references_DOI_Xdh59anGlczmCXzFUlQrxGXL1p6"}]}