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

Author: Grafiati

Published: 6 September 2023

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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 simil

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2

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 a

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3

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

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4

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

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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

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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 < -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 d

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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 densit

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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 traditi

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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 mechanis

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11

Prikryl, P., G. Provan, K. A. McWilliams, and T. K. Yeoman. "Ionospheric cusp flows pulsed by solar wind Alfvén waves." Annales Geophysicae 20, no. 2 (2002): 161–74. http://dx.doi.org/10.5194/angeo-20-161-2002.

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Abstract. Pulsed ionospheric flows (PIFs) in the cusp foot-print have been observed by the SuperDARN radars with periods between a few minutes and several tens of minutes. PIFs are believed to be a consequence of the interplanetary magnetic field (IMF) reconnection with the magnetospheric magnetic field on the dayside magnetopause, ionospheric signatures of flux transfer events (FTEs). The quasiperiodic PIFs are correlated with Alfvénic fluctuations observed in the upstream solar wind. It is concluded that on these occasions, the FTEs were driven by Alfvén waves coupling to the day-side magnet

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12

Dudeney, J. R., K. B. Baker, P. H. Stoker, and A. D. M. Walker. "The Southern Hemisphere Auroral Radar Experiment (SHARE)." Antarctic Science 6, no. 1 (1994): 123–24. http://dx.doi.org/10.1017/s0954102094000155.

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The near Earth space environment (known as Geospace) is dominated by the interaction between the solar wind and the geomagnetic field, which creates the magnetosphere. Considerable energy flows from the solar wind into the magnetosphere and ends up in the Earth's upper atmosphere (the thermosphere and ionosphere). The coupling of the geomagnetic field with that of the solar wind (known as the interplanetary magnetic field, or IMF) produces a variety of electro-dynamic responses with signatures such as electric fields and currents in the polar ionospheres. These produce, inter alia, motion of t

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Oprea, Constantin, Marilena Mierla, and Georgeta Maris. "Earth–directed coronal mass ejections and their geoeffectiveness during the 2007–2010 interval." Proceedings of the International Astronomical Union 7, S286 (2011): 242–45. http://dx.doi.org/10.1017/s1743921312004917.

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AbstractIn this study we analyse the coronal mass ejections (CMEs) directed towards the Earth during the interval 2007–2010, using the data acquired by STEREO mission and those provided by SOHO, ACE and geomagnetic stations. A study of CMEs kinematics is performed. This is correlated with CMEs interplanetary manifestations and their geomagnetic effects, along with the energy transfer flux into magnetosphere (the Akasofu coupling function). The chosen interval that is practically coincident with the last solar minimum, offered us a good opportunity to link and analyse the chain of phenomena fro

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14

Nielsen, E., and F. Honary. "Observations of ionospheric flows and particle precipitation following a Sudden Commencement." Annales Geophysicae 18, no. 8 (2000): 908–17. http://dx.doi.org/10.1007/s00585-000-0908-y.

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Abstract. On May 4, 1998, at 0227 UT an interplanetary shock crossed the WIND spacecraft, and half an hour later a Sudden Commencement occurred. Coinciding with the Sudden Commencement a rapid intensification of the flux of particle precipitation into the ionosphere was observed. Evidence is presented that the ionospheric electric fields were influenced by the associated dynamic variations of the ionospheric conductivities. Following the initial phase the ionospheric flow speeds increased rapidly over the next 20 min to more than 2000 m/s, in agreement with an increased effective coupling of t

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15

Sun, Weijie, Ryan M. Dewey, Sae Aizawa, et al. "Review of Mercury’s dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres." Science China Earth Sciences 65, no. 1 (2021): 25–74. http://dx.doi.org/10.1007/s11430-021-9828-0.

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AbstractThis review paper summarizes the research of Mercury’s magnetosphere in the Post-MESSENGER era and compares its dynamics to those in other planetary magnetospheres, especially to those in Earth’s magnetosphere. This review starts by introducing the planet Mercury, including its interplanetary environment, magnetosphere, exosphere, and conducting core. The frequent and intense magnetic reconnection on the dayside magnetopause, which is represented by the flux transfer event “shower”, is reviewed on how they depend on magnetosheath plasma β and magnetic shear angle across the magnetopaus

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16

Chu, W., and G. Qin. "The geomagnetic cutoff rigidities at high latitudes for different solar wind and geomagnetic conditions." Annales Geophysicae 34, no. 1 (2016): 45–53. http://dx.doi.org/10.5194/angeo-34-45-2016.

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Abstract. Studying the access of the cosmic rays (CRs) into the magnetosphere is important to understand the coupling between the magnetosphere and the solar wind. In this paper we numerically studied CRs' magnetospheric access with vertical geomagnetic cutoff rigidities using the method proposed by Smart and Shea (1999). By the study of CRs' vertical geomagnetic cutoff rigidities at high latitudes we obtain the CRs' window (CRW) whose boundary is determined when the vertical geomagnetic cutoff rigidities drop to a value lower than a threshold value. Furthermore, we studied the area of CRWs an

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17

Jankovičovà, D., Z. Vörös, and J. Šimkanin. "The influence of solar wind turbulence on geomagnetic activity." Nonlinear Processes in Geophysics 15, no. 1 (2008): 53–59. http://dx.doi.org/10.5194/npg-15-53-2008.

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Abstract. The importance of space weather and its forecasting is growing as interest in studying geoeffective processes in the Sun – solar wind – magnetosphere – ionosphere coupled system is increasing. In this paper higher order statistical moments of interplanetary magnetic field and geomagnetic SYM-H index fluctuations are compared. The proper description of fluctuations in the solar wind can elucidate important aspects of the geoeffectivity of upstream turbulence and contribute to our understanding of space weather. Our results indicate that quasi-stationary intervals during both quiet and

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18

Adebesin, B. Olufemi, S. Oluwole Ikubanni, and J. Stephen Kayode. "On the Geoeffectiveness Structure of Solar Wind-Magnetosphere Coupling Functions during Intense Storms." ISRN Astronomy and Astrophysics 2011 (January 17, 2011): 1–13. http://dx.doi.org/10.5402/2011/961757.

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The geoeffectiveness of some coupling functions for the Solar Wind-Magnetosphere Interaction had been studied. 58 storms with peak Dst < −100 nT were used. The result showed that the interplanetary magnetic field Bz appeared to be more relevant with the magnetic field B (which agreed with previous results). However, both the V (solar wind flow speed) and Bz factors in the interplanetary dawn-dusk electric field (V×Bz) are effective in the generation of very intense storms (peak Dst < −250 nT) while “intense” storms (−250 nT ≤ peak Dst < −100 nT) are mostly enhanced by the Bz factor al

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19

Saunders, Mark. "The polar cusp ionosphere: a window on solar wind–magnetosphere coupling." Antarctic Science 1, no. 3 (1989): 193–203. http://dx.doi.org/10.1017/s0954102089000313.

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The polar cusp ionosphere is an important part of near-Earth space which is best monitored by ground-based observations made in the remote polar regions. Antarctica seems certain to play a key role in its future exploration. The region is characterized by the direct entry of solar wind particles along magnetic field lines projecting to the dayside magnetopause (outer boundary of the magnetosphere). Thus the polar cusp ionosphere provides a splendid window for examining processes transferring solar wind mass and momentum to the magnetosphere. The review will emphasize this aspect of polar cusp

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20

Oprea, C., M. Mierla, D. Beşliu-Ionescu, O. Stere, and G. Mariş Muntean. "A study of solar and interplanetary parameters of CMEs causing major geomagnetic storms during SC 23." Annales Geophysicae 31, no. 8 (2013): 1285–95. http://dx.doi.org/10.5194/angeo-31-1285-2013.

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Abstract. In this paper we analyse 25 Earth-directed and strongly geoeffective interplanetary coronal mass ejections (ICMEs) which occurred during solar cycle 23, using data provided by instruments on SOHO (Solar and Heliospheric Observatory), ACE (Advanced Composition Explorer) and geomagnetic stations. We also examine the in situ parameters, the energy transfer into magnetosphere, and the geomagnetic indexes. We compare observed travel times with those calculated by observed speeds projected into the plane of the sky and de-projected by a simple model. The best fit was found with the project

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Kozelov, B. V., and T. V. Kozelova. "Cellular automata model of magnetospheric-ionospheric coupling." Annales Geophysicae 21, no. 9 (2003): 1931–38. http://dx.doi.org/10.5194/angeo-21-1931-2003.

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Abstract. We propose a cellular automata model (CAM) to describe the substorm activity of the magnetospheric-ionospheric system. The state of each cell in the model is described by two numbers that correspond to the energy content in a region of the current sheet in the magnetospheric tail and to the conductivity of the ionospheric domain that is magnetically connected with this region. The driving force of the system is supposed to be provided by the solar wind that is convected along the two boundaries of the system. The energy flux inside is ensured by the penetration of the energy from the

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Lakka, Antti, Tuija I. Pulkkinen, Andrew P. Dimmock, et al. "GUMICS-4 analysis of interplanetary coronal mass ejection impact on Earth during low and typical Mach number solar winds." Annales Geophysicae 37, no. 4 (2019): 561–79. http://dx.doi.org/10.5194/angeo-37-561-2019.

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Abstract. We study the response of the Earth's magnetosphere to fluctuating solar wind conditions during interplanetary coronal mass ejections (ICMEs) using the Grand Unified Magnetosphere-Ionosphere Coupling Simulation (GUMICS-4). The two ICME events occurred on 15–16 July 2012 and 29–30 April 2014. During the strong 2012 event, the solar wind upstream values reached up to 35 particles cm−3, speeds of up to 694 km s−1, and an interplanetary magnetic field of up to 22 nT, giving a Mach number of 2.3. The 2014 event was a moderate one, with the corresponding upstream values of 30 particles cm−3

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Myllys, M., E. Kilpua, and T. Pulkkinen. "Solar-wind control of plasma sheet dynamics." Annales Geophysicae 33, no. 7 (2015): 845–55. http://dx.doi.org/10.5194/angeo-33-845-2015.

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Abstract. The purpose of this study is to quantify how solar-wind conditions affect the energy and plasma transport in the geomagnetic tail and its large-scale configuration. To identify the role of various effects, the magnetospheric data were sorted according to different solar-wind plasma and interplanetary magnetic field (IMF) parameters: speed, dynamic pressure, IMF north–south component, epsilon parameter, Auroral Electrojet (AE) index and IMF ultra low-frequency (ULF) fluctuation power. We study variations in the average flow speed pattern and the occurrence rate of fast flow bursts in

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Dai, Lei, Yimin Han, Chi Wang, et al. "Geoeffectiveness of Interplanetary Alfvén Waves. I. Magnetopause Magnetic Reconnection and Directly Driven Substorms." Astrophysical Journal 945, no. 1 (2023): 47. http://dx.doi.org/10.3847/1538-4357/acb267.

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Abstract In particular during the descending phase of the solar cycle, Alfvén waves in the high-speed solar wind streams are a major form of interplanetary disturbances. The fluctuating southward interplanetary magnetic field (IMF) of Alfvén waves has been suggested to induce geomagnetic activities through intermittent magnetic reconnection at the magnetopause. In this study, we provide in situ observational evidence for dayside magnetopause reconnection induced by such interplanetary Alfvén waves. Using multipoint conjunction observations, we show that the IMF B z from interplanetary Alfvén w

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Østgaard, N., J. Moen, S. B. Mende, et al. "Estimates of magnetotail reconnection rate based on IMAGE FUV and EISCAT measurements." Annales Geophysicae 23, no. 1 (2005): 123–34. http://dx.doi.org/10.5194/angeo-23-123-2005.

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Abstract. Dayside merging between the interplanetary and terrestrial magnetic fields couples the solar wind electric field to the Earth's magnetosphere, increases the magnetospheric convection and results in efficient transport of solar wind energy into the magnetosphere. Subsequent reconnection of the lobe magnetic field in the magnetotail transports energy into the closed magnetic field region. Combining global imaging and ground-based radar measurements, we estimate the reconnection rate in the magnetotail during two days of an EISCAT campaign in November-December 2000. Global images from t

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Jankovičová, D., Z. Vörös, and J. Šimkanin. "The effect of upstream turbulence and its anisotropy on the efficiency of solar wind – magnetosphere coupling." Nonlinear Processes in Geophysics 15, no. 4 (2008): 523–29. http://dx.doi.org/10.5194/npg-15-523-2008.

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Abstract. The importance of space weather and its forecasting is growing as interest in studying geoeffective processes in the Sun – solar wind – magnetosphere – ionosphere coupled system is increasing. This paper introduces the proper selection criteria for solar wind magnetic turbulence events during duskward electric field and southward Bz driven geomagnetic storms. Two measures for the strength of solar wind fluctuations were investigated: the standard deviations of magnetic field components and a proxy for the so-called Shebalin anisotropy angles. These measures were compared to the stren

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Adhikari, Binod, and Narayan P. Chapagain. "Polar Cap Potential and Merging Electric Field during High Intensity Long Duration Continuous Auroral Activity." Journal of Nepal Physical Society 3, no. 1 (2016): 6. http://dx.doi.org/10.3126/jnphyssoc.v3i1.14437.

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<p>The polar cap potential (PCV) has long been considered as a key parameter for describing the state of the magnetosphere/ionosphere system. The relationship between the solar wind parameters and the PCV is important to understand the coupling process between solar wind-magnetosphere-ionosphere. In this work, we have estimated PCV and merging electric field (Em) during two different high intensity long duration continuous auroral activity (HILDCAA) events. For each event, we examine the solar wind parameters, magnitude of interplanetary magnetic field (IMF), interplanetary electric fiel

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Sumod, Sukumarn N. G. K., Tarun K. Pant, and Asokan P. Ajesh. "Signatures of Sudden Storm Commencement on the equatorial thermospheric dayglow." Journal of Space Weather and Space Climate 9 (2019): A31. http://dx.doi.org/10.1051/swsc/2019026.

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It has been observed that the OI 630.0 nm dayglow emission over a dip equatorial station, Trivandrum (8.5° N, 77° E, dip 0.5° N), India registered an abrupt increase of ~ 2000 R during the compression phase of the magnetosphere as dictated by a sudden increase in solar wind ram pressure. Furthermore, an unusual depletion of these emissions has been observed during the eastward interplanetary electric field (IEF), concomitant with southward excursion of IMF Bz. The ionosonde and magnetometer observations confirmed the effects of prompt penetration electric field (PPEF). Associated with the east

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Echer, Ezequiel, Axel Korth, Mauricio José Alves Bolzan, and Reinhard Hans Walter Friedel. "Global geomagnetic responses to the IMF <i>B</i><sub>z</sub> fluctuations during the September/October 2003 high-speed stream intervals." Annales Geophysicae 35, no. 4 (2017): 853–68. http://dx.doi.org/10.5194/angeo-35-853-2017.

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Abstract. In this paper, we follow the coupling from the solar wind to the Earth's magnetotail, geosynchronous orbit, auroral zone and to the ground, during periods of Alfvénic fluctuations in high-speed solar wind streams (HSSs) and their corotating interaction regions (CIRs). We employ cross-wavelet analysis of magnetic field, particle flux and auroral electrojet (AE) index data for the HSSs of September and October 2003. Our results show a remarkably consistent periodic response among all of these regions and across multiple substorm indicators, indicating a possible driven substorm respons

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Vörös, Z., and D. Jankovičová. "Neural network prediction of geomagnetic activity: a method using local Hölder exponents." Nonlinear Processes in Geophysics 9, no. 5/6 (2002): 425–33. http://dx.doi.org/10.5194/npg-9-425-2002.

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Abstract. Local scaling and singularity properties of solar wind and geomagnetic time series were analysed using Hölder exponents . It was shown that in analysed cases due to the multifractality of fluctuations, α changes from point to point. We argued there exists a peculiar interplay between regularity/irregularity and amplitude characteristics of fluctuations which could be exploited for the improvement of predictions of geomagnetic activity. To this end, a layered back-propagation artificial neural network model with feedback connection was used for the study of the solar wind magnetospher

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Grandin, Maxime, Markus Battarbee, Adnane Osmane, et al. "Hybrid-Vlasov modelling of nightside auroral proton precipitation during southward interplanetary magnetic field conditions." Annales Geophysicae 37, no. 5 (2019): 791–806. http://dx.doi.org/10.5194/angeo-37-791-2019.

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Abstract. Particle precipitation plays a key role in the coupling of the terrestrial magnetosphere and ionosphere by modifying the upper atmospheric conductivity and chemistry, driving field-aligned currents, and producing aurora. Yet quantitative observations of precipitating fluxes are limited, since ground-based instruments can only provide indirect measurements of precipitation, while particle telescopes aboard spacecraft merely enable point-like in situ observations with an inherently coarse time resolution above a given location. Further, orbit timescales generally prevent the analysis o

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Namuun, B., Battuulai Tsegmed, L. Y. Li, and G. M. Leghari. "Differences in the response to CME and CIR drivers of geomagnetic disturbances." Solar-Terrestrial Physics 9, no. 2 (2023): 31–36. http://dx.doi.org/10.12737/stp-92202304.

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Utilizing 1-minute resolution data on the geomagnetic indices SYM-H, AE, solar wind parameters (velocity Vsw and density Np), and z-component Bz of the interplanetary magnetic field (IMF) during solar cycles 23 and 24, we have statistically analyzed the correlations between geomagnetic activity (storms and substorms), Vsw, Np, Bz, and energy coupling functions of solar wind and Earth’s magnetosphere. For the selected 131 CME-driven storms, SYM-H stronger depends on Vsw and B than other parameters, whereas the selected 161 CIR-driven storms have nearly the same dependence on the solar wind elec

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Namuun, B., Battuulai Tsegmed, L. Y. Li, and G. M. Leghari. "Differences in the response to CME and CIR drivers of geomagnetic disturbances." Solnechno-Zemnaya Fizika 9, no. 2 (2023): 35–40. http://dx.doi.org/10.12737/szf-92202304.

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Utilizing 1-minute resolution data on the geomagnetic indices SYM-H, AE, solar wind parameters (velocity Vsw and density Np), and z-component Bz of the interplanetary magnetic field (IMF) during solar cycles 23 and 24, we have statistically analyzed the correlations between geomagnetic activity (storms and substorms), Vsw, Np, Bz, and energy coupling functions of solar wind and Earth’s magnetosphere. For the selected 131 CME-driven storms, SYM-H stronger depends on Vsw and B than other parameters, whereas the selected 161 CIR-driven storms have nearly the same dependence on the solar wind elec

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McWilliams, K. A., G. J. Sofko, T. K. Yeoman, et al. "Simultaneous observations of magnetopause flux transfer events and of their associated signatures at ionospheric altitudes." Annales Geophysicae 22, no. 6 (2004): 2181–99. http://dx.doi.org/10.5194/angeo-22-2181-2004.

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Abstract. An extensive variety of instruments, including Geotail, DMSP F11, SuperDARN, and IMP-8, were monitoring the dayside magnetosphere and ionosphere between 14:00 and 18:00 UT on 18 January 1999. The location of the instruments provided an excellent opportunity to study in detail the direct coupling between the solar wind, the magnetosphere, and the ionosphere. Flux transfer events were observed by Geotail near the magnetopause in the dawn side magnetosheath at about 4 magnetic local time during exclusively northward interplanetary magnetic field conditions. Excellent coverage of the ent

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Longden, N., F. Honary, A. J. Kavanagh, and J. Manninen. "The driving mechanisms of particle precipitation during the moderate geomagnetic storm of 7 January 2005." Annales Geophysicae 25, no. 9 (2007): 2053–68. http://dx.doi.org/10.5194/angeo-25-2053-2007.

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Abstract. The arrival of an interplanetary coronal mass ejection (ICME) triggered a sudden storm commencement (SSC) at ~09:22 UT on the 7 January 2005. The ICME followed a quiet period in the solar wind and interplanetary magnetic field (IMF). We present global scale observations of energetic electron precipitation during the moderate geomagnetic storm driven by the ICME. Energetic electron precipitation is inferred from increases in cosmic noise absorption (CNA) recorded by stations in the Global Riometer Array (GLORIA). No evidence of CNA was observed during the first four hours of passage o

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Prikryl, P., R. Ghoddousi-Fard, L. Spogli, et al. "GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 2: Interhemispheric comparison." Annales Geophysicae 33, no. 6 (2015): 657–70. http://dx.doi.org/10.5194/angeo-33-657-2015.

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Abstract. During the ascending phase of solar cycle 24, a series of interplanetary coronal mass ejections (ICMEs) in the period 7–17 March 2012 caused geomagnetic storms that strongly affected high-latitude ionosphere in the Northern and Southern Hemisphere. GPS phase scintillation was observed at northern and southern high latitudes by arrays of GPS ionospheric scintillation and TEC monitors (GISTMs) and geodetic-quality GPS receivers sampling at 1 Hz. Mapped as a function of magnetic latitude and magnetic local time (MLT), the scintillation was observed in the ionospheric cusp, the tongue of

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Rostoker, G., and F. Pascal. "Dependence of the response of the magnetosphere–ionosphere current systems on the preconditioning of the auroral oval and on the level of the solar–terrestrial interaction." Canadian Journal of Physics 68, no. 1 (1990): 74–80. http://dx.doi.org/10.1139/p90-011.

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It is now well accepted that the impulse response time of the magnetosphere to sudden changes in the interplanetary medium is of the order of 2 h with the shape of the impulse response function approximating a Rayleigh function with a peak near 50 min. In a recent study, Bargatze et al. (J. Geophys. Res. 90, 6387 (1985)) examined the response of the magnetosphere for varying activity levels and found that the impulse response function has two well-defined peaks for moderate activity and a single broad peak for low and high activity levels. They explain the two peaks in the response function as

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Murphree, J. S., L. L. Cogger, R. D. Elphinstone, and D. Hearn. "The response of the quiet-time auroral configuration to short- and long-term interplanetary magnetic field variations." Canadian Journal of Physics 69, no. 8-9 (1991): 1040–46. http://dx.doi.org/10.1139/p91-161.

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Observations from the IMP-8 satellite of the interplanetary magnetic field (IMF) are compared with areas of the polar region bounded by the aurora as observed by the Viking spacecraft during quiet-time conditions (IMF Bz northward). A variety of energy-coupling functions are investigated and it is determined that the auroral distribution can be best described by the inclusion of azimuthal terms in addition to standard energy-coupling functions. The auroral distributions for Bz northward support antiparallel merging as a mechanism whereby energy is transferred to the magnetosphere from the sola

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Schmölter, Erik, and Jens Berdermann. "North–South IMF Disturbance Detection via an Adaptive Filter Approach." Atmosphere 13, no. 9 (2022): 1482. http://dx.doi.org/10.3390/atmos13091482.

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Geomagnetic storm-detection algorithms are important for space-weather-warning services to provide reliable warnings (e.g., ionospheric disturbances). For that reason, a new approach using an adaptive filter (least mean squares algorithm) for the detection of geomagnetic storms based on the volatility of the north–south interplanetary magnetic field Bz is presented. The adaptive filter is not dependent on solar wind plasma measurements, which are more frequently affected by data gaps than Bz, and is less dependent on the magnitude of Bz disturbances compared with other detection algorithms (e.

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Korth, H., B. J. Anderson, H. U. Frey, and C. L. Waters. "High-latitude electromagnetic and particle energy flux during an event with sustained strongly northward IMF." Annales Geophysicae 23, no. 4 (2005): 1295–310. http://dx.doi.org/10.5194/angeo-23-1295-2005.

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Abstract. We present a case study of a prolonged interval of strongly northward orientation of the interplanetary magnetic field on 16 July 2000, 16:00-19:00 UT to characterize the energy exchange between the magnetosphere and ionosphere for conditions associated with minimum solar wind-magnetosphere coupling. With reconnection occurring tailward of the cusp under northward IMF conditions, the reconnection dynamo should be separated from the viscous dynamo, presumably driven by the Kelvin-Helmholtz (KH) instability. Thus, these conditions are also ideal for evaluating the contribution of a vis

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Parkinson, M. L. "Dynamical critical scaling of electric field fluctuations in the greater cusp and magnetotail implied by HF radar observations of F-region Doppler velocity." Annales Geophysicae 24, no. 2 (2006): 689–705. http://dx.doi.org/10.5194/angeo-24-689-2006.

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Abstract. Akasofu's solar wind ε parameter describes the coupling of solar wind energy to the magnetosphere and ionosphere. Analysis of fluctuations in ε using model independent scaling techniques including the peaks of probability density functions (PDFs) and generalised structure function (GSF) analysis show the fluctuations were self-affine (mono-fractal, single exponent scaling) over 9 octaves of time scale from ~46 s to ~9.1 h. However, the peak scaling exponent α0 was a function of the fluctuation bin size, so caution is required when comparing the exponents for different data sets sampl

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Prikryl, P., R. Ghoddousi-Fard, E. G. Thomas, et al. "GPS phase scintillation at high latitudes during geomagnetic storms of 7–17 March 2012 – Part 1: The North American sector." Annales Geophysicae 33, no. 6 (2015): 637–56. http://dx.doi.org/10.5194/angeo-33-637-2015.

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Abstract. The interval of geomagnetic storms of 7–17 March 2012 was selected at the Climate and Weather of the Sun-Earth System (CAWSES) II Workshop for group study of space weather effects during the ascending phase of solar cycle 24 (Tsurutani et al., 2014). The high-latitude ionospheric response to a series of storms is studied using arrays of GPS receivers, HF radars, ionosondes, riometers, magnetometers, and auroral imagers focusing on GPS phase scintillation. Four geomagnetic storms showed varied responses to solar wind conditions characterized by the interplanetary magnetic field (IMF)

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Milan, S. E., T. A. Evans, and B. Hubert. "Average auroral configuration parameterized by geomagnetic activity and solar wind conditions." Annales Geophysicae 28, no. 4 (2010): 1003–12. http://dx.doi.org/10.5194/angeo-28-1003-2010.

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Abstract. Average proton and electron auroral images are compiled from three years of observations by the IMAGE spacecraft, binned according to concurrent KP and upstream solar wind conditions measured by the ACE spacecraft. The solar wind parameters include solar wind velocity, density, and pressure, interplanetary magnetic field (IMF) magnitude and orientation, and an estimate of the magnetopause reconnection rate. We use both (a) the overall variation in brightness in the images and (b) the variation in location of the aurorae with respect to the binning parameters to determine which parame

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Sandholt, P. E., C. J. Farrugia, and W. F. Denig. "Detailed dayside auroral morphology as a function of local time for southeast IMF orientation: implications for solar wind-magnetosphere coupling." Annales Geophysicae 22, no. 10 (2004): 3537–60. http://dx.doi.org/10.5194/angeo-22-3537-2004.

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Abstract. In two case studies we elaborate on spatial and temporal structures of the dayside aurora within 08:00-16:00 magnetic local time (MLT) and discuss the relationship of this structure to solar wind-magnetosphere interconnection topology and the different stages of evolution of open field lines in the Dungey convection cycle. The detailed 2-D auroral morphology is obtained from continuous ground observations at Ny Ålesund (76° magnetic latitude (MLAT)), Svalbard during two days when the interplanetary magnetic field (IMF) is directed southeast (By>0; Bz<0). The auroral activity co

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Matsui, H., P. A. Puhl-Quinn, V. K. Jordanova, Y. Khotyaintsev, P. A. Lindqvist, and R. B. Torbert. "Derivation of inner magnetospheric electric field (UNH-IMEF) model using Cluster data set." Annales Geophysicae 26, no. 9 (2008): 2887–98. http://dx.doi.org/10.5194/angeo-26-2887-2008.

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Abstract. We derive an inner magnetospheric electric field (UNH-IMEF) model at L=2–10 using primarily Cluster electric field data for more than 5 years between February 2001 and October 2006. This electric field data set is divided into several ranges of the interplanetary electric field (IEF) values measured by ACE. As ring current simulations which require electric field as an input parameter are often performed at L=2–6.6, we have included statistical results from ground radars and low altitude satellites inside the perigee of Cluster in our data set (L~4). Electric potential patterns are d

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Koustov, A. V., G. Ya Khachikjan, R. A. Makarevich, and C. Bryant. "On the SuperDARN cross polar cap potential saturation effect." Annales Geophysicae 27, no. 10 (2009): 3755–64. http://dx.doi.org/10.5194/angeo-27-3755-2009.

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Abstract. Variation of the cross polar cap potential (CPCP) with the interplanetary electric field (IEF), the merging electric field EKL, the Polar Cap North (PCN) magnetic index, and the solar wind-magnetosphere coupling function EC of Newell et al. (2007) is investigated by considering convection data collected by the Super Dual Auroral Radar Network (SuperDARN) in the Northern Hemisphere. Winter and summer observations are considered separately. All variations considered show close to linear trend at small values of the parameters and tendency for the saturation at large values. The thresho

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McPherron, R. L., L. Kepko, T. I. Pulkkinen, T. S. Hsu, J. W. Weygand, and L. F. Bargatze. "Changes in the response of the AL Index with solar cycle and epoch within a corotating interaction region." Annales Geophysicae 27, no. 8 (2009): 3165–78. http://dx.doi.org/10.5194/angeo-27-3165-2009.

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Abstract. We use observations in the solar wind and on the ground to study the interaction of the solar wind and interplanetary magnetic field with Earth's magnetosphere. We find that the type of response depends on the state of the solar wind. Coupling functions change as the properties of the solar wind change. We examine this behavior quantitatively with time dependent linear prediction filters. These filters are determined from ensemble arrays of representative events organized by some characteristic time in the event time series. In our study we have chosen the stream interface at the cen

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Sandholt, P. E., C. J. Farrugia, and W. F. Denig. "Transitions between states of magnetotail–ionosphere coupling and the role of solar wind dynamic pressure: the 25 July 2004 interplanetary CME case." Annales Geophysicae 33, no. 4 (2015): 427–36. http://dx.doi.org/10.5194/angeo-33-427-2015.

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Abstract. In a case study, we investigate transitions between fundamental magnetosphere–ionosphere (M-I) coupling modes during storm-time conditions (SYM-H between −100 and −160 nT) driven by an interplanetary coronal mass ejection (ICME). We combine observations from the near tail, at geostationary altitude (GOES-10), and electrojet activities across the auroral oval at postnoon-to-dusk and midnight. After an interval of strong westward electrojet (WEJ) activity, a 3 h long state of attenuated/quenched WEJ activity was initiated by abrupt drops in the solar wind density and dynamic pressure.

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Sandholt, P. E., C. J. Farrugia, and W. F. Denig. "M–I coupling across the auroral oval at dusk and midnight: repetitive substorm activity driven by interplanetary coronal mass ejections (CMEs)." Annales Geophysicae 32, no. 4 (2014): 333–51. http://dx.doi.org/10.5194/angeo-32-333-2014.

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Abstract. We study substorms from two perspectives, i.e., magnetosphere–ionosphere coupling across the auroral oval at dusk and at midnight magnetic local times. By this approach we monitor the activations/expansions of basic elements of the substorm current system (Bostrøm type I centered at midnight and Bostrøm type II maximizing at dawn and dusk) during the evolution of the substorm activity. Emphasis is placed on the R1 and R2 types of field-aligned current (FAC) coupling across the Harang reversal at dusk. We distinguish between two distinct activity levels in the substorm expansion phase

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Chernogor, L. F., K. P. Garmash, Y. H. Zhdanko, S. G. Leus, and Y. Luo. "FEATURES OF IONOSPHERIC EFFECTS FROM THE PARTIAL SOLAR ECLIPSE OVER THE CITY OF KHARKIV ON 10 JUNE 2021." Radio physics and radio astronomy 26, no. 4 (2021): 326–43. http://dx.doi.org/10.15407/rpra26.04.326.

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Purpose: Solar eclipses pertain to high-energy sources of disturbance in the subsystems of the Sun–interplanetary-medium–magnetosphere–ionosphere–atmosphere–Earth and the Earth–atmosphere–ionosphere–magnetosphere systems. During the solar eclipse, the coupling between the subsystems in these systems activates, and the parameters of the dynamic processes become disturbed. Investigation of these processes contributes to understanding of the structure and dynamics of the subsystems. The ionospheric response to the solar eclipse depends on the season, local time, magnitude of the solar eclipse, ph

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