Theoretical modeling for the stereo mission

Aschwanden, Markus J.; Burlaga, L. F.; Kaiser, M. L.; Ng, C. K.; Reames, D. V.; Reiner, M. J.; Gombosi, T. I.; Lugaz, Noé; Manchester, W.; Roussev, I. I.; Zurbuchen, T. H.; Farrugia, C. J.; Galvin, A. B.; Lee, M. A.; Linker, J. A.; Mikić, Z.; Riley, Pete; Alexander, D. M.; Sandman, A.; Cook, J. W.; Howard, R. A.; Odstrčil, D.; Pizzo, V. J.; Kóta, J.; Liewer, Paulett C.; Luhmann, J. G.; Inhester, B.; Schwenn, R.; Solanki, S. K.; Vasyliūnas, V. M.; Wiegelmann, T.; Blush, L. M.; Bochsler, P.; Cairns, Iver H.; Robinson, P. A.; Bothmer, V.; Kecskeméty, K.; Llebaria, A.; Maksimović, M.; Scholer, M.; Wimmer‐Schweingruber, R. F.

doi:10.1007/s11214-006-9027-8

Cited by 40 publications

(26 citation statements)

References 173 publications

(141 reference statements)

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“…Solar wind heating/acceleration has long been debated by scientists for long (Aschwanden 2004;Aschwanden et al 2008). Since the creative work by Pneuman & Kopp (1971) empirically describing the source terms for the deposition of energy and/or momentum into the solar wind, many works have been devoted to the numerical study of producing solar steady-state conditions (e.g., Usmanov 1993;McKenzie et al 1997;Mikić et al 1999;Suess et al 1996Suess et al , 1999Wu et al 1999;Groth et al 2000;Feng et al 2005Feng et al , 2007Kleimann et al 2009;Nakamizo et al 2009).…”

Section: Determination Of the Momentum Source Term S M And The Energymentioning

confidence: 99%

THREE-DIMENSIONAL SOLARWINDMODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

Feng

Yang

Cui

et al. 2010

ApJ

171

144

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The objective of this paper is to explore the application of a six-component overset grid to solar wind simulation with a three-dimensional (3D) Solar-InterPlanetary Conservation Element/Solution Element MHD model. The essential focus of our numerical model is devoted to dealing with: (1) the singularity and mesh convergence near the poles via the use of the six-component grid system, (2) the ∇ · B constraint error via an easy-to-use cleaning procedure by a fast multigrid Poisson solver, (3) the Courant-Friedrichs-Levy number disparity via the Courant-number insensitive method, (4) the time integration by multiple time stepping, and (5) the time-dependent boundary condition at the subsonic region by limiting the mass flux escaping through the solar surface. In order to produce fast and slow plasma streams of the solar wind, we include the volumetric heating source terms and momentum addition by involving the topological effect of the magnetic field expansion factor f S and the minimum angular distance θ b (at the photosphere) between an open field foot point and its nearest coronal hole boundary. These considerations can help us easily code the existing program, conveniently carry out the parallel implementation, efficiently shorten the computation time, greatly enhance the accuracy of the numerical solution, and reasonably produce the structured solar wind. The numerical study for the 3D steady-state background solar wind during Carrington rotation 1911 from the Sun to Earth is chosen to show the above-mentioned merits. Our numerical results have demonstrated overall good agreements in the solar corona with the Large Angle and Spectrometric Coronagraph on board the Solar and Heliospheric Observatory satellite and at 1 AU with WIND observations.

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Section: Determination Of the Momentum Source Term S M And The Energymentioning

confidence: 99%

THREE-DIMENSIONAL SOLARWINDMODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

Feng

Yang

Cui

et al. 2010

ApJ

171

144

View full text Add to dashboard Cite

show abstract

“…There is a large amount of literature on the topic that is impossible to report here (see Aschwanden et al 2008, for a comprehensive review on progress in modelling solar structures, CME/shocks and solar energetic particles). Generally, to explain the different characteristics observed in solar particles events a continuous acceleration in one-phase (related to the DC mechanism-mainly impulsive events) was proposed for some cases and for others (gradual or two-component events) an intermittent acceleration with two or more acceleration phases (mainly associated with stochastic or shock wave accelerations) with possible particle trapping between them.…”

Section: Suprathermal Solar Particlesmentioning

confidence: 99%

Solar Weather Event Modelling and Prediction

et al. 2009

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Key drivers of solar weather and mid-term solar weather are reviewed by considering a selection of relevant physics-and statistics-based scientific models as well as a selection of related prediction models, in order to provide an updated operational scenario for space weather applications. The characteristics and outcomes of the considered scientific and prediction models indicate that they only partially cope with the complex nature of solar activity for the lack of a detailed knowledge of the underlying physics. This is indicated by the fact that, on one hand, scientific models based on chaos theory and non-linear dynamics reproduce better the observed features, and, on the other hand, that prediction models based on statistics and artificial neural networks perform better. To date, the solar weather prediction success at most time and spatial scales is far from being satisfactory, but the forthcoming ground-and space-based high-resolution observations can add fundamental tiles to the modelling and predicting frameworks as well as the application of advanced mathematical approaches in the analysis of diachronic solar observations, that are a must to provide comprehensive and homogeneous data sets.

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“…In order to predict the arrival of a CME and avoid potential damages, many methods have been developed to monitor the position and three-dimensional (3D) structure of CMEs using data from multiple coronagraphs. These methods include stereoscopy (Inhester 2006;Aschwanden et al 2008), GCS Forward Modeling (GCSFM) (Thernisien et al 2006), Polarization Ratio method (PR) (Moran & Davila 2004), mask fitting (Feng et al 2012), and the local correlation tracking plus triangulation (Mierla et al 2009). Comparisons between different methods have been made by Mierla et al (2010), Thernisien (2011) and Feng et al (2013).…”

Section: Introductionmentioning

confidence: 99%

Measure the Propagation of a Halo CME and Its Driven Shock with the Observations from a Single Perspective at Earth

Inhester

et al. 2017

ApJ

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We present a detailed study of an earth-directed coronal mass ejection (Full halo CME) event happened on 2011 February 15 making use of white light observations by three coronagraphs and radio observations by Wind/WAVES. We applied three different methods to reconstruct the propagation direction and traveling distance of the CME and its driven shock. We measured the kinematics of the CME leading edge from white light images observed by STEREO A and B, tracked the CME-driven shock using the frequency drift observed by Wind/WAVES together with an interplanetary density model, and obtained the equivalent scattering centers of the CME by Polarization Ratio(PR) method. For the first time, we applied PR method to different features distinguished from LASCO/C2 polarimetric observations and calculated their projections onto white light images observed by STEREO A and B. By combining the graduated cylindrical shell (GCS) forward modeling with the PR method, we proposed a new GCS-PR method to derive 3D parameters of a CME observed from a single perspective at Earth. Comparisons between different methods show a good degree of consistence in the derived 3D results.

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Theoretical modeling for the stereo mission

Cited by 40 publications

References 173 publications

THREE-DIMENSIONAL SOLARWINDMODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

THREE-DIMENSIONAL SOLARWINDMODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

Solar Weather Event Modelling and Prediction

Measure the Propagation of a Halo CME and Its Driven Shock with the Observations from a Single Perspective at Earth

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