title: TheHelioseismic and Magnetic Imager(HMI) Vector Magnetic Field Pipeline: Magnetohydrodynamics Simulation Module for the Global Solar Corona.
abstract: Time-dependent three-dimensional magnetohydrodynamics (MHD) simulation modules are implemented at the Joint Science Operation Center (JSOC) of theSolar Dynamics Observatory(SDO). The modules regularly produce three-dimensional data of the time-relaxed minimum-energy state of the solar corona using global solar-surface magnetic-field maps created fromHelioseismic and Magnetic Imager(HMI) full-disk magnetogram data. With the assumption of a polytropic gas with specific-heat ratio of 1.05, three types of simulation products are currently generated: i) simulation data with medium spatial resolution using the definitive calibrated synoptic map of the magnetic field with a cadence of one Carrington rotation, ii) data with low spatial resolution using the definitive version of the synchronic frame format of the magnetic field, with a cadence of one day, and iii) low-resolution data using near-real-time (NRT) synchronic format of the magnetic field on a daily basis. The MHD data available in the JSOC database are three-dimensional, covering heliocentric distances from 1.025 to 4.975 solar radii, and contain all eight MHD variables: the plasma density, temperature, and three components of motion velocity, and three components of the magnetic field. This article describes details of the MHD simulations as well as the production of the input magnetic-field maps, and details of the products available at the JSOC database interface. To assess the merits and limits of the model, we show the simulated data in early 2011 and compare with the actual coronal features observed by theAtmospheric Imaging Assembly(AIA) and the near-Earthin-situdata.
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA ; National Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, China.
authors.forename: K
authors.initials: K
authors.lastname: Hayashi
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA.
authors.forename: J T
authors.initials: JT
authors.lastname: Hoeksema
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA.
authors.forename: Y
authors.initials: Y
authors.lastname: Liu
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA.
authors.forename: M G
authors.initials: MG
authors.lastname: Bobra
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA.
authors.forename: X D
authors.initials: XD
authors.lastname: Sun
authors.affiliation: W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA USA.
authors.forename: A A
authors.initials: AA
authors.lastname: Norton
keywords: Corona; Instrumentation and data management; Interplanetary; Magnetic field; Magnetohydrodynamics; Photosphere