Unifying the validation of ambient solar wind models

Reiss, Martin A.; Muglach, K.; Mullinix, R.; Кузнецова, М.; Wiegand, C.; Temmer, Manuela; Arge, C. N.; Dasso, S.; Fung, S. F.; González-Avilés, J. J.; Gonzi, Siegfried; Jian, L. K.; MacNeice, P. J.; Möstl, Christian; Owens, M. J.; Perri, Barbara; Pinto, Rui; Rastätter, L.; Riley, Pete; Samara, Evangelia

doi:10.1016/j.asr.2022.05.026

Cited by 15 publications

(10 citation statements)

References 97 publications

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“…In particular, we compared measurements and model solutions by estimating the Normalized Root Mean Square Error (NRMSE) and the Pearson Correlation Coefficient (PCC). The NRMSE represents the normal- ized mean squared difference between measurements and models and facilitates comparing models with different scales [36], while the PCC measures linear correlation between two data sets. These two statistical measures are defined as follows:…”

Section: Discussionmentioning

confidence: 99%

Investigating the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind in the inner heliosphere

De León Alanís,

González Avilés,

Riley

et al. 2024

Rev. Mex. Fís.

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This paper explores the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind (SW) in the inner heliosphere. To do so, we use sunRunner3D, a 3-D magnetohydrodynamics model that employs the boundary conditions generated by CORHEL and the PLUTO code to compute the plasma properties of the SW with the ideal magnetohydrodynamics approximation up to 1.1 AU in the inner heliosphere. Mainly, we define three different combinations of numerical algorithms based on their diffusion level. This diffusion level is related to the way of solving the magnetohydrodynamics equations using the finite volume formulation, and, therefore, we set in terms of the divergence-free condition methods, Riemann solvers, variable reconstruction schemes, limiters, and time-steeping algorithms. According to the simulation results, we demonstrate that sunRunner3D reproduces global features of Corotating Interaction Regions observed by Earth-based spacecraft for a set of Carrington rotations that cover a period that lays in the late declining phase of solar cycle 24, independently of the numerical algorithms. Moreover, statistical analyses between models and in-situ measurements show reasonable agreement with the observations, and remarkably, the high diffusive method matches better with in-situ data than low diffusive methods.

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Section: Discussionmentioning

confidence: 99%

Investigating the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind in the inner heliosphere

De León Alanís,

González Avilés,

Riley

et al. 2024

Rev. Mex. Fís.

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“…Jian et al (2011) reported that SIR timing predictions can have temporal offsets of up to 2 days at 1 AU and up to 4 days at 5 AU. Large-scale efforts dedicated to benchmarking solar wind models (e.g., Reiss et al, 2022) will likely lead to improved predictions of solar wind structures (including SIRs and CMEs) and their effects at different planets. In fact, a well-constrained and well-reproduced solar wind background is of great importance for simulating solar minimum CMEs, which tend to alter their structure and orientation during propagation largely due to interactions with the steady wind (see, e.g., the May 1997 event; Cohen et al, 2010;Odstrcil et al, 2004;Titov et al, 2008).…”

Section: Discussionmentioning

confidence: 99%

CME Evolution in the Structured Heliosphere and Effects at Earth and Mars During Solar Minimum

et al. 2022

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The activity of the Sun alternates between a solar minimum and a solar maximum, the former corresponding to a period of “quieter” status of the heliosphere. During solar minimum, it is in principle more straightforward to follow eruptive events and solar wind structures from their birth at the Sun throughout their interplanetary journey. In this paper, we report analysis of the origin, evolution, and heliospheric impact of a series of solar transient events that took place during the second half of August 2018, that is, in the midst of the late declining phase of Solar Cycle 24. In particular, we focus on two successive coronal mass ejections (CMEs) and a following high‐speed stream (HSS) on their way toward Earth and Mars. We find that the first CME impacted both planets, whilst the second caused a strong magnetic storm at Earth and went on to miss Mars, which nevertheless experienced space weather effects from the stream interacting region preceding the HSS. Analysis of remote‐sensing and in‐situ data supported by heliospheric modeling suggests that CME–HSS interaction resulted in the second CME rotating and deflecting in interplanetary space, highlighting that accurately reproducing the ambient solar wind is crucial even during “simpler” solar minimum periods. Lastly, we discuss the upstream solar wind conditions and transient structures responsible for driving space weather effects at Earth and Mars.

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“…While somewhat computationally expensive, these models are currently run for real time forecasts, such as at NOAA's Space Weather Prediction Center (SWPC; https://www.swpc.noaa.gov) and at the UK Met Office (https://www.metoffice.gov.uk/weather/specialist-forecasts/space-weather). International efforts aimed at unifying the validation of ambient solar wind models are currently underway (e.g., Jian et al., 2015; Reiss et al., 2022).…”

Section: Introductionmentioning

confidence: 99%

An Efficient, Time‐Dependent High Speed Stream Model and Application to Solar Wind Forecasts

et al. 2023

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A continuous stream of plasma blows out from the solar atmosphere, spreading out into interplanetary space. This so-called solar wind is not uniform, but rather contains distinct regions of fast (≳600 km/s) and slow (300-400 km/s) plasma flows. The fast solar wind is known to originate along the open magnetic field lines emanating from coronal holes (CHs; e.g., Cranmer, 2009) but there is less consensus on the source of the slow wind (see Cranmer et al., 2017, for a review on the origins of the ambient solar wind). Possible sources of the slow wind that have been proposed in the literature include helmet streamers (e.g.,

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Unifying the validation of ambient solar wind models

Cited by 15 publications

References 97 publications

Investigating the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind in the inner heliosphere

Investigating the effects of numerical algorithms on global magnetohydrodynamics simulations of solar wind in the inner heliosphere

CME Evolution in the Structured Heliosphere and Effects at Earth and Mars During Solar Minimum

An Efficient, Time‐Dependent High Speed Stream Model and Application to Solar Wind Forecasts

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