Relevant bibliographies by topics / Solar-interplanetary magnetosphere coupling

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Academic literature on the topic 'Solar-interplanetary magnetosphere coupling'

Author: Grafiati
Published: 6 September 2023

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Journal articles on the topic "Solar-interplanetary magnetosphere coupling"

1

Marques de Souza, Adriane, Ezequiel Echer, Mauricio José Alves Bolzan, and Rajkumar Hajra. "Cross-correlation and cross-wavelet analyses of the solar wind IMF <i>B</i><sub><i>z</i></sub> and auroral electrojet index AE coupling during HILDCAAs." Annales Geophysicae 36, no. 1 (2018): 205–11. http://dx.doi.org/10.5194/angeo-36-205-2018.

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Abstract. Solar-wind–geomagnetic activity coupling during high-intensity long-duration continuous AE (auroral electrojet) activities (HILDCAAs) is investigated in this work. The 1 min AE index and the interplanetary magnetic field (IMF) Bz component in the geocentric solar magnetospheric (GSM) coordinate system were used in this study. We have considered HILDCAA events occurring between 1995 and 2011. Cross-wavelet and cross-correlation analyses results show that the coupling between the solar wind and the magnetosphere during HILDCAAs occurs mainly in the period ≤ 8 h. These periods are similar to the periods observed in the interplanetary Alfvén waves embedded in the high-speed solar wind streams (HSSs). This result is consistent with the fact that most of the HILDCAA events under present study are related to HSSs. Furthermore, the classical correlation analysis indicates that the correlation between IMF Bz and AE may be classified as moderate (0.4–0.7) and that more than 80 % of the HILDCAAs exhibit a lag of 20–30 min between IMF Bz and AE. This result corroborates with Tsurutani et al. (1990) where the lag was found to be close to 20–25 min. These results enable us to conclude that the main mechanism for solar-wind–magnetosphere coupling during HILDCAAs is the magnetic reconnection between the fluctuating, negative component of IMF Bz and Earth's magnetopause fields at periods lower than 8 h and with a lag of about 20–30 min. Keywords. Magnetospheric physics (solar-wind–magnetosphere interactions)
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Stumpo, Mirko, Giuseppe Consolini, Tommaso Alberti, and Virgilio Quattrociocchi. "Measuring Information Coupling between the Solar Wind and the Magnetosphere–Ionosphere System." Entropy 22, no. 3 (2020): 276. http://dx.doi.org/10.3390/e22030276.

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The interaction between the solar wind and the Earth’s magnetosphere–ionosphere system is very complex, being essentially the result of the interplay between an external driver, the solar wind, and internal processes to the magnetosphere–ionosphere system. In this framework, modelling the Earth’s magnetosphere–ionosphere response to the changes of the solar wind conditions requires a correct identification of the causality relations between the different parameters/quantities used to monitor this coupling. Nowadays, in the framework of complex dynamical systems, both linear statistical tools and Granger causality models drastically fail to detect causal relationships between time series. Conversely, information theory-based concepts can provide powerful model-free statistical quantities capable of disentangling the complex nature of the causal relationships. In this work, we discuss how to deal with the problem of measuring causal information in the solar wind–magnetosphere–ionosphere system. We show that a time delay of about 30–60 min is found between solar wind and magnetospheric and ionospheric overall dynamics as monitored by geomagnetic indices, with a great information transfer observed between the z component of the interplanetary magnetic field and geomagnetic indices, while a lower transfer is found when other solar wind parameters are considered. This suggests that the best candidate for modelling the geomagnetic response to solar wind changes is the interplanetary magnetic field component B z . A discussion of the relevance of our results in the framework of Space Weather is also provided.
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Finch, I., and M. Lockwood. "Solar wind-magnetosphere coupling functions on timescales of 1 day to 1 year." Annales Geophysicae 25, no. 2 (2007): 495–506. http://dx.doi.org/10.5194/angeo-25-495-2007.

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Abstract. There are no direct observational methods for determining the total rate at which energy is extracted from the solar wind by the magnetosphere. In the absence of such a direct measurement, alternative means of estimating the energy available to drive the magnetospheric system have been developed using different ionospheric and magnetospheric indices as proxies for energy consumption and dissipation and thus the input. The so-called coupling functions are constructed from the parameters of the interplanetary medium, as either theoretical or empirical estimates of energy transfer, and the effectiveness of these coupling functions has been evaluated in terms of their correlation with the chosen index. A number of coupling functions have been studied in the past with various criteria governing event selection and timescale. The present paper contains an exhaustive survey of the correlation between geomagnetic activity and the near-Earth solar wind and two of the planetary indices at a wide variety of timescales. Various combinations of interplanetary parameters are evaluated with careful allowance for the effects of data gaps in the interplanetary data. We show that the theoretical coupling, Pα, function first proposed by Vasyliunas et al. is superior at all timescales from 1-day to 1-year.
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Zhang, Qing-He, Yong-Liang Zhang, Chi Wang, et al. "Multiple transpolar auroral arcs reveal insight about coupling processes in the Earth’s magnetotail." Proceedings of the National Academy of Sciences 117, no. 28 (2020): 16193–98. http://dx.doi.org/10.1073/pnas.2000614117.

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A distinct class of aurora, called transpolar auroral arc (TPA) (in some cases called “theta” aurora), appears in the extremely high-latitude ionosphere of the Earth when interplanetary magnetic field (IMF) is northward. The formation and evolution of TPA offers clues about processes transferring energy and momentum from the solar wind to the magnetosphere and ionosphere during a northward IMF. However, their formation mechanisms remain poorly understood and controversial. We report a mechanism identified from multiple-instrument observations of unusually bright, multiple TPAs and simulations from a high-resolution three-dimensional (3D) global MagnetoHydroDynamics (MHD) model. The observations and simulations show an excellent agreement and reveal that these multiple TPAs are generated by precipitating energetic magnetospheric electrons within field-aligned current (FAC) sheets. These FAC sheets are generated by multiple-flow shear sheets in both the magnetospheric boundary produced by Kelvin–Helmholtz instability between supersonic solar wind flow and magnetosphere plasma, and the plasma sheet generated by the interactions between the enhanced earthward plasma flows from the distant tail (less than −100 RE) and the enhanced tailward flows from the near tail (about −20 RE). The study offers insight into the complex solar wind-magnetosphere-ionosphere coupling processes under a northward IMF condition, and it challenges existing paradigms of the dynamics of the Earth’s magnetosphere.
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Eriksson, S., L. G. Blomberg, N. Ivchenko, T. Karlsson, and G. T. Marklund. "Magnetospheric response to the solar wind as indicated by the cross-polar potential drop and the low-latitude asymmetric disturbance field." Annales Geophysicae 19, no. 6 (2001): 649–53. http://dx.doi.org/10.5194/angeo-19-649-2001.

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Abstract. The cross-polar potential drop Φpc and the low-latitude asymmetric geomagnetic disturbance field, as indicated by the mid-latitude ASY-H magnetic index, are used to study the average magnetospheric response to the solar wind forcing for southward interplanetary magnetic field conditions. The state of the solar wind is monitored by the ACE spacecraft and the ionospheric convection is measured by the double probe electric field instrument on the Astrid-2 satellite. The solar wind-magnetosphere coupling is examined for 77 cases in February and from mid-May to mid-June 1999 by using the interplanetary magnetic field Bz component and the reconnection electric field. Our results show that the maximum correlation between Φpc and the reconnection electric field is obtained approximately 25 min after the solar wind has reached a distance of 11 RE from the Earth, which is the assumed average position of the magnetopause. The corresponding correlation for ASY-H shows two separate responses to the reconnection electric field, delayed by about 35 and 65 min, respectively. We suggest that the combination of the occurrence of a large magnetic storm on 18 February 1999 and the enhanced level of geomagnetic activity which peaks at Kp = 7- may explain the fast direct response of ASY-H to the solar wind at 35 min, as well as the lack of any clear secondary responses of Φpc to the driving solar wind at time delays longer than 25 min.Key words. Magnetospheric physics (solar wind-magnetosphere interactions; plasma convection) – Ionosphere (electric fields and currents)
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6

González, W. D., A. L. Calu de González, and B. T. Tsurutani. "Interplanetary-magnetosphere coupling during intense geomagnetic storms at solar maximum." Geofísica Internacional 31, no. 1 (1992): 11–18. http://dx.doi.org/10.22201/igeof.00167169p.1992.31.1.1299.

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Durante el intervalo del 16 de agosto de 1978 al 28 de diciembre de 1979, 90% de las tempestades geomagnéticas intensas (Dst &lt; -100nT) fueron precedidas por la llegada a 1AU de ondas de choque interplanetarias rápidas, conforme fueron identificadas con los datos de plasma y campos magnéticos colectados por la nave espacial ISEE-3. En la relación con estos eventos, discutiremos las estructuras interplanetarias asociadas a campos magnéticos Bz negativos, de gran amplitud y larga duración, que se consideran como la causa principal de las tempestades intensas. Presentaremos también un resumen de las funciones de acoplamiento interplanetario- magnetosféricas, basadas en el proceso de reconexión en la magnetopausa terrestre. Terminaremos con una revisión sucinta de la evolución a largo plazo de las tempestades geomagnéticas intensas, tales como las mostradas en las distribuciones estacionales y del ciclo solar.
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7

Yermolaev, Yuri I., Irina G. Lodkina, Alexander A. Khokhlachev, and Michael Yu Yermolaev. "Peculiarities of the Heliospheric State and the Solar-Wind/Magnetosphere Coupling in the Era of Weakened Solar Activity." Universe 8, no. 10 (2022): 495. http://dx.doi.org/10.3390/universe8100495.

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Based on the data of the solar wind (SW) measurements of the OMNI database for the period 1976–2019, we investigate the behavior of SW types, as well as plasma and interplanetary magnetic field (IMF) parameters, for 21–24 solar cycles (SCs). Our analysis shows that with the beginning of the period of low solar activity (SC 23), the number of all types of disturbed events in the interplanetary medium decreased, but the proportion of magnetic storms initiated by CIR increased. In addition, a change in the nature of SW interaction with the magnetosphere could occur due to a decrease in the density, temperature, and IMF of solar wind.
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8

Pokhotelov, D., I. J. Rae, K. R. Murphy, and I. R. Mann. "The influence of solar wind variability on magnetospheric ULF wave power." Annales Geophysicae 33, no. 6 (2015): 697–701. http://dx.doi.org/10.5194/angeo-33-697-2015.

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Abstract. Magnetospheric ultra-low frequency (ULF) oscillations in the Pc 4–5 frequency range play an important role in the dynamics of Earth's radiation belts, both by enhancing the radial diffusion through incoherent interactions and through the coherent drift-resonant interactions with trapped radiation belt electrons. The statistical distributions of magnetospheric ULF wave power are known to be strongly dependent on solar wind parameters such as solar wind speed and interplanetary magnetic field (IMF) orientation. Statistical characterisation of ULF wave power in the magnetosphere traditionally relies on average solar wind–IMF conditions over a specific time period. In this brief report, we perform an alternative characterisation of the solar wind influence on magnetospheric ULF wave activity through the characterisation of the solar wind driver by its variability using the standard deviation of solar wind parameters rather than a simple time average. We present a statistical study of nearly one solar cycle (1996–2004) of geosynchronous observations of magnetic ULF wave power and find that there is significant variation in ULF wave powers as a function of the dynamic properties of the solar wind. In particular, we find that the variability in IMF vector, rather than variabilities in other parameters (solar wind density, bulk velocity and ion temperature), plays the strongest role in controlling geosynchronous ULF power. We conclude that, although time-averaged bulk properties of the solar wind are a key factor in driving ULF powers in the magnetosphere, the solar wind variability can be an important contributor as well. This highlights the potential importance of including solar wind variability especially in studies of ULF wave dynamics in order to assess the efficiency of solar wind–magnetosphere coupling.
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9

Lopez, Ramon E., Charles Goodrich, Michael Wiltberger, and John Lyon. "Solar wind–magnetosphere energy coupling under extreme interplanetary conditions: MHD simulations." Journal of Atmospheric and Solar-Terrestrial Physics 62, no. 10 (2000): 865–74. http://dx.doi.org/10.1016/s1364-6826(00)00058-4.

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10

Umar, R., S. N. A. Syed Zafar, N. H. Sabri, et al. "Earth’s geomagnetic response to solar wind changes associated with solar events at low latitude regions at the TRE MAGDAS Station." IOP Conference Series: Earth and Environmental Science 880, no. 1 (2021): 012009. http://dx.doi.org/10.1088/1755-1315/880/1/012009.

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Abstract The Sun’s magnetic activity influences disturbances that perturb interplanetary space by producing large fluxes of energetic protons, triggering geomagnetic storms and affecting the ground geomagnetic field. The effect of two solar events, namely Coronal Mass Ejection (CME) and Coronal Holes, on geomagnetic indices (SYM/H), solar wind parameters and ground geomagnetic fields has provided magnetic ground data, which were extracted from the Terengganu (TRE, -4.21° N, 175.91° E) Magnetometer (MAGDAS) station, and investigated in this study. Results show that the physical dynamic mechanism in the Earth’s magnetosphere is triggered by various solar wind parameters associated with CMEs and Coronal hole events during the minimum solar cycle of 24 at low latitudes. It is important to study solar wind-magnetosphere coupling because it has an impact on ground-based technological systems and human activities.
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