The UCSD kinematic IPS solar wind boundary and its use in the ENLIL 3‐D MHD prediction model

Jackson, B. V.; Odstrčil, D.; Yu, Hsiu-Shan; Hick, P. P.; Buffington, A.; Mejia‐Ambriz, J. C.; Kim, J.; Hong, Sang Bum; Kim, Y.; Han, Jizhong; Tokumaru, M.

doi:10.1002/2014sw001130

Cited by 47 publications

(48 citation statements)

References 59 publications

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“…Although we have not used NSO Global Oscillation Network Group (GONG) observations (http://gong.nso.edu/data/magmap/) previously, we want to determine whether they provide as good or better near‐Earth magnetic‐field extrapolations. Additionally, in a recent study, Jackson et al [] used SOLIS magnetograms and the CSSS model to extrapolate fields from below the cusp surface (hereafter termed as “closed‐field” analyses) radially upward over a period of 3 years and found that these have shown positive correlations with the north‐south flux component measured in situ. These analyses (or see Yeates et al .…”

Section: Introductionmentioning

confidence: 99%

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Jackson

Buffington

et al. 2016

Space Weather

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This article investigates the use of two different types of National Solar Observatory magnetograms and two different coronal field modeling techniques over 10 years. Both the “open‐field” Current Sheet Source Surface (CSSS) and a “closed‐field” technique using CSSS modeling are compared. The University of California, San Diego, tomographic modeling, using interplanetary scintillation data from Japan, provides the global velocities to extrapolate these fields outward, which are then compared with fields measured in situ near Earth. Although the open‐field technique generally gives a better result for radial and tangential fields, we find that a portion of the closed extrapolated fields measured in situ near Earth comes from the direct outward mapping of these fields in the low solar corona. All three closed‐field components are nonzero at 1 AU and are compared with the appropriate magnetometer values. A significant positive correlation exists between these closed‐field components and the in situ measurements over the last 10 years. We determine that a small fraction of the static low‐coronal component flux, which includes the Bn (north‐south) component, regularly escapes from closed‐field regions. The closed‐field flux fraction varies by about a factor of 3 from a mean value during this period, relative to the magnitude of the field components measured in situ near Earth, and maximizes in 2014. This implies that a relatively more efficient process for closed‐flux escape occurs near solar maximum. We also compare and find that the popular Potential Field Source Surface and CSSS model closed fields are nearly identical in sign and strength.

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Section: Introductionmentioning

confidence: 99%

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Jackson

Buffington

et al. 2016

Space Weather

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“…Alternatively, a 3‐D iterative tomography, which modifies a time‐dependent three‐dimensional kinematic heliospheric model to fit interplanetary scintillation (IPS) observations, can supply solar wind velocity and density from 15 R s to 3 AU [ Jackson et al , ; Jian et al , ]. This 3‐D tomography technique can also be combined with some magnetic field models based on photospheric magnetograms to specify the bottom boundary conditions for the MHD solar wind simulations [ Yu et al , ; Jackson et al , ].…”

Section: Introductionmentioning

confidence: 99%

Data‐driven modeling of the solar wind from 1 R_s to 1 AU

Feng

Xiang

2015

JGR Space Physics

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We present here a time‐dependent three‐dimensional magnetohydrodynamic (MHD) solar wind simulation from the solar surface to the Earth's orbit driven by time‐varying line‐of‐sight solar magnetic field data. The simulation is based on the three‐dimensional (3‐D) solar‐interplanetary (SIP) adaptive mesh refinement (AMR) space‐time conservation element and solution element (CESE) MHD (SIP‐AMR‐CESE MHD) model. In this simulation, we first achieve the initial solar wind background with the time‐relaxation method by inputting a potential field obtained from the synoptic photospheric magnetic field and then generate the time‐evolving solar wind by advancing the initial 3‐D solar wind background with continuously varying photospheric magnetic field. The model updates the inner boundary conditions by using the projected normal characteristic method, inputting the high‐cadence photospheric magnetic field data corrected by solar differential rotation, and limiting the mass flux escaping from the solar photosphere. We investigate the solar wind evolution from 1 July to 11 August 2008 with the model driven by the consecutive synoptic maps from the Global Oscillation Network Group. We compare the numerical results with the previous studies on the solar wind, the solar coronal observations from the Extreme ultraviolet Imaging Telescope board on Solar and Heliospheric Observatory, and the measurements from OMNI at 1 astronomical unit (AU). Comparisons show that the present data‐driven MHD model's results have overall good agreement with the large‐scale dynamical coronal and interplanetary structures, including the sizes and distributions of the coronal holes, the positions and shapes of the streamer belts, the heliocentric distances of the Alfvénic surface, and the transitions of the solar wind speeds. However, the model fails to capture the small‐sized equatorial holes, and the modeled solar wind near 1 AU has a somewhat higher density and weaker magnetic field strength than observed. Perhaps better preprocessing of high‐cadence observed photospheric magnetic field (particularly 3‐D global measurements), combined with plasma measurements and higher resolution grids, will enable the data‐driven model to more accurately capture the time‐dependent changes of the ambient solar wind for further improvements. In addition, other measures may also be needed when the model is employed in the period of high solar activity.

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“…Instead of presenting information from imaging separately, in whatever form, to allow forecasters to make subjective decisions, the heliospheric imagery could potentially be assimilated into the heliospheric model itself; such assimilation is, however, challenging. One way in which this could be done is a manner analogous to what his now being done using the ground‐based IPS data, which are being exploited as inner boundary values to drive 3‐D MHD models including Enlil [ Jackson et al ., ; Yu et al ., ].…”

Section: The Futurementioning

confidence: 98%

The application of heliospheric imaging to space weather operations: Lessons learned from published studies

et al. 2017

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The field of heliospheric imaging has matured significantly over the last 10 years—corresponding, in particular, to the launch of NASA's STEREO mission and the successful operation of the heliospheric imager (HI) instruments thereon. In parallel, this decade has borne witness to a marked increase in concern over the potentially damaging effects of space weather on space and ground‐based technological assets, and the corresponding potential threat to human health, such that it is now under serious consideration at governmental level in many countries worldwide. Hence, in a political climate that recognizes the pressing need for enhanced operational space weather monitoring capabilities most appropriately stationed, it is widely accepted, at the Lagrangian L1 and L5 points, it is timely to assess the value of heliospheric imaging observations in the context of space weather operations. To this end, we review a cross section of the scientific analyses that have exploited heliospheric imagery—particularly from STEREO/HI—and discuss their relevance to operational predictions of, in particular, coronal mass ejection (CME) arrival at Earth and elsewhere. We believe that the potential benefit of heliospheric images to the provision of accurate CME arrival predictions on an operational basis, although as yet not fully realized, is significant and we assert that heliospheric imagery is central to any credible space weather mission, particularly one located at a vantage point off the Sun‐Earth line.

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The UCSD kinematic IPS solar wind boundary and its use in the ENLIL 3‐D MHD prediction model

Cited by 47 publications

References 59 publications

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Data‐driven modeling of the solar wind from 1 R_s to 1 AU

The application of heliospheric imaging to space weather operations: Lessons learned from published studies

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The UCSD kinematic IPS solar wind boundary and its use in the ENLIL 3‐D MHD prediction model

Cited by 47 publications

References 59 publications

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Exploration of solar photospheric magnetic field data sets using the UCSD tomography

Data‐driven modeling of the solar wind from 1 Rs to 1 AU

The application of heliospheric imaging to space weather operations: Lessons learned from published studies

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Data‐driven modeling of the solar wind from 1 R_s to 1 AU