2.7.1 https://spdx.org/licenses/ SPDX CC0-1.0 https://spdx.org/licenses/CC0-1.0.html Creative Commons Zero v1.0 Universal CC0 1.0 Universal is the Creative Commons license applicable to all publicly available SPASE metadata descriptions spase://NASA/DisplayData/UCLA/Global-MHD-code/mS4-BIF/PT10S NASA DisplayData Characteristics of Reconnection Sites and Fast Flow Channels in an MHD Simulation. Supplementary MHD simulation movie mS4-BIF.mp4 for 14 March 2008. https://doi.org/10.21978/p8rw5g 2025-12-04T13:28:08Z 2022-03-16T00:00:00Z Only known prior ReleaseDate of the metadata 2025-03-03T13:30:47Z Modified Funding AwardNumber. ZCB 2025-09-30T14:25:28Z Updated PublishedBy name to match ROR Registry. Added ResourceType and NamingAuthority. ZCB 2025-12-04T13:28:08Z Added MetadataRightsList. Updated to 2.7.1. ZCB Section 4.1 of the text describes our procedure for identifying the locations of x-lines in a map of the neutral surface. At each value of Y in an interpolated grid, we scan the entire length of the trace of Vx from -10 to -70 Re. A function finds all intervals of Vx>=250 km/s and Vx less then or equal to -250 km/s. We call these earthward and tailward fast flow intervals. We define a bifurcation of fast flow as the point at which Vx changes sign from fast earthward to fast tailward flow. In simple cases, this transition occurs in about 2 Re (20 grid points). The zero crossing is the location of the x-line at this value of Y. As described in the text, we process the arrays of zero crossings to define a line in the neutral surface. We display this information as lines parallel to X at fixed Y. Intervals of fast earthward flow are represented by a thick red line. Fast flow is a thick blue line. The zero crossing is a gray circle. After completion of the plot, we add x-lines as colored ropes (yellow with black stripes). Each map is in a file and subsequently made into a movie. The movie illustrates the formation and evolution of x-lines. The movie begins at 04:00 UT with at least five significant x-lines and six earthward flow channels. This is the start of the growth phase of a substorm. As time advances the locations of the x-lines change as flow channels move away from them. New lines form and channels merge. When the movie approaches substorm onset at 04:44 UT the x-lines merge into a single long x-line stretching diagonally across the tail. About 04:35, the nose of the fast earthward flow channel penetrates close to the Earth, and then begins to sweep westward to earlier local times. At this, time the movie mS02 and the text Figure 13 shows magnetic flux accumulating close to the Earth. At 04:50 UT, the single channels spawns new channels that flow directly toward Earth rather than along the diagonal channel. Mostafa El-Alaoui, Raymond J. Walker; Robert L. McPherron R.L. McPherron; M. El-Alaoui; R.J. Walker; and R.L. Richard 2020-08-31T00:00:00Z University of California, Los Angeles NASA Substorm current wedge development and evolution using THEMIS observation and simulations NNX17AB83G NASA Structure and evolution of plasma sheet fast flows using THEMIS observation and global MHD simulations NNX15AI63G NSF GEM: A Statistical Study of the Substorm Sequence and Phenomena Associated with Expansion Onset 1602588 spase://SMWG/Person/Robert.L.McPherron GeneralContact spase://SMWG/Person/James.M.Weygand MetadataContact Virtual Magnetospheric Observatory directory containing movies for Journal of Gephysical Research publication. http://vmo.igpp.ucla.edu/data1/McPherron/Simulation_Movies_and_Data/Simulation_Movies/mS2-Bz.avi Supplimentary movies for JGR publication spase://SMWG/Repository/UCLA/VMO Online Open Virtual Magnetospheric Observatory http://vmo.igpp.ucla.edu/data1/ Virtual Magnetospheric Observatory EN AVI If data downloaded from the VMO Data Repository are used in publication kindly acknowledge the Virtual Magnetospheric Observatory, Earth, Planetary and Space Science Department, University of California, Los Angeles for providing access to the data. Raw UCLA M. El-Alaoui MHD Simulation MHD Simulation Movies Raw spase://SMWG/Instrument/UCLA/Global-MHD-code ThermalPlasma 2008-03-14T04:00:00 2008-03-14T05:00:00 PT10S Earth.Magnetosphere MHD Simulation Substorm High Speed Earthward Flows MHD simulation movie of GSM X component of position for 14 March 2008 X component of position Two dimensional display of this movie of the GSM X component of position is on the original. PT10S Re Cartesian GSM 3840 1890 Each image is 3840 pixels by 1890 pixels and there are 360 frames in the movie. -70 0 Direction Positional MHD simulation movie of GSM Y component of position for 14 March 2008 Y component of position Two dimensional display of this movie of the GSM Y component of position is on the original. PT10S Re Cartesian GSM 3840 1890 Each image is 3840 pixels by 1890 pixels and there are 360 frames in the movie. -20 20 Direction Positional MHD simulation movie of GSM X component of plasma flow velocity for 14 March 2008 Vx component of plasma flow Two dimensional display of this movie of the GSM X component of plasma flow velocity is on the original, not interpolated grid. Red means Vx flows earthward and is greater then or equal to 250 km/s, Blue means Vx flows tailward and is less then or equal to 250 km/s, and white means flows are between -250 and 250 km/s. PT10S km/s Cartesian GSM 3840 1890 Each image is 3840 pixels by 1890 pixels and there are 360 frames in the movie. -250 250 Vector Velocity MHD simulation movie of GSM plasma flow velocity for 14 March 2008 Vx and Vy components of plasma flow Two dimensional display of this movie of the GSM plasma flow velocity interpolated grid. PT10S km/s Cartesian GSM 3840 1890 Each image is 3840 pixels by 1890 pixels and there are 360 frames in the movie. -300 300 Vector Velocity