Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

The aim of this paper is to structure and extend the knowledge of solar chromospheric sources of oscillations in the solar wind and their relationships with pulsations registered in the magnetosphere. We compare the oscillation spectra that we observe using instruments of the Institute of Solar-Terrestrial Physics in different chromospheric structures with those observed in the solar wind and magnetosphere. We explore the possibility that the observed periodic variations of the chromospheric line widths can be interpreted as torsional Alfvén wave manifestation—this mode can propagate long distances without dissipating in the interplanetary space; it can penetrate into Earth’s magnetosphere directly or due to processes occurring at the plasmapause. We emphasize the similarities in the oscillation characteristics observed in different media, the similarities in the parameters of the media themselves and the processes developing in them. We believe that similar approaches can be applied to studying these media.

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Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

Solar-Terrestrial Physics ◽

10.12737/stp-44201802 ◽

2018 ◽

Vol 4 (4) ◽

pp. 12-18

Author(s):

Андрей Челпанов ◽

Andrey Chelpanov ◽

Максим Челпанов ◽

Maksim Chelpanov ◽

Николай Кобанов ◽

...

Keyword(s):

Solar Wind ◽

Interplanetary Space ◽

Alfven Wave ◽

Solar Chromosphere ◽

Earth's Magnetosphere ◽

The Media ◽

Line Widths ◽

Chromospheric Line ◽

Oscillation Characteristics ◽

Made In

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Space Weather, SuperDARN and the Tasmanian Tiger

Australian Journal of Physics ◽

10.1071/p96115 ◽

1997 ◽

Vol 50 (4) ◽

pp. 773 ◽

Cited By ~ 1

Author(s):

Raymond A. Greenwald

Keyword(s):

Solar Wind ◽

Electric Fields ◽

Space Weather ◽

Interplanetary Space ◽

Rapid Evolution ◽

Upper Atmosphere ◽

Global Network ◽

Pressure Gradients ◽

Earth’S Magnetosphere ◽

Earth's Magnetosphere

The plasma environment extending from the solar surface through interplanetary space to the outermost reaches of the Earth’s atmosphere and magnetic field is dynamic, often disturbed, and capable of harming humans and damaging manmade systems. Disturbances in this environment have been identified as space weather disturbances. At the present time there is growing interest in monitoring and predicting space weather disturbances. In this paper we present some of the difficulties involved in achieving this goal by comparing the processes that drive tropospheric-weather systems with those that drive space-weather systems in the upper atmosphere and ionosphere. The former are driven by pressure gradients which result from processes that heat and cool the atmosphere. The latter are driven by electric fields that result from interactions between the streams of ionised gases emerging from the Sun (solar wind) and the Earth’s magnetosphere. Although the dimensions of the Earth’s magnetosphere are vastly greater than those of tropospheric weather systems, the global space-weather response to changes in the solar wind is much more rapid than the response of tropospheric-weather systems to changing conditions. We shall demonstrate the rapid evolution of space-weather systems in the upper atmosphere through measurements with a global network of radars known as SuperDARN. We shall also describe how the SuperDARN network is evolving, including a newly funded Australian component known as the Tasman International Geospace Environmental Radar (TIGER).

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On the Origin of ULF Magnetic Waves Before the Taiwan Chi-Chi 1999 Earthquake

Frontiers in Earth Science ◽

10.3389/feart.2021.730162 ◽

2021 ◽

Vol 9 ◽

Author(s):

Georgios Anagnostopoulos

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Interplanetary Space ◽

Solar Rotation ◽

Rotation Period ◽

Wave Activity ◽

Alfven Wave ◽

Ulf Waves ◽

Storm Activity ◽

Data Set

The ultra low frequency (ULF) electromagnetic (EM) wave activity usually recorded on Earth’s ground has been found to depend on various types of space weather. In addition ULF waves observed before an earthquake have been hypothesized to be a result of geotectonic processes. In this study we elaborate for the first time the origin of sub-ULF (<1 msec) magnetic field waves before an earthquake (Chi-Chi/Taiwan, 20.9.1999) by comparing simultaneously obtained measurements in the interplanetary space (ACE satellite) and on the Earth’s ground (Taiwan). The most striking result of our data analysis, during a period of 7 weeks, is that the detection of four groups of sub-ULF waves in Taiwan coincide in time with the quasi-periodic detection of two solar wind streams by the satellite ACE with approximately the solar rotation period (∼28 days). The high speed solar wind streams (HSSs) in the interplanetary space were accompanied by sub-ULF Alfvén wave activity, quasi-periodic southward IMF and solar wind density perturbations, which are known as triggering agents of magnetic storm activity. The four HSSs were followed by long lasting decreases in the magnetic field in Taiwan. The whole data set examined in this study strongly suggest that the subULF magnetic field waves observed in Taiwan before the Chi-Chi 1999 earthquake is a normal consequence of the incident of HSSs to the magnetosphere. We provide some observational evidence that the sub-ULF electromagnetic radiation on the Earth was most probably a partner to (not a result of) geotectonic processes preparing the Taiwan 1999 earthquake.

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The physics of space weather/solar-terrestrial physics (STP): what we know now and what the current and future challenges are

Nonlinear Processes in Geophysics ◽

10.5194/npg-27-75-2020 ◽

2020 ◽

Vol 27 (1) ◽

pp. 75-119 ◽

Cited By ~ 3

Author(s):

Bruce T. Tsurutani ◽

Gurbax S. Lakhina ◽

Rajkumar Hajra

Keyword(s):

Solar Wind ◽

Space Weather ◽

Energetic Particle ◽

High Speed ◽

Geomagnetic Storms ◽

Interplanetary Space ◽

Magnetic Clouds ◽

Slow Solar Wind ◽

Earth’S Magnetosphere ◽

Earth's Magnetosphere

Abstract. Major geomagnetic storms are caused by unusually intense solar wind southward magnetic fields that impinge upon the Earth's magnetosphere (Dungey, 1961). How can we predict the occurrence of future interplanetary events? Do we currently know enough of the underlying physics and do we have sufficient observations of solar wind phenomena that will impinge upon the Earth's magnetosphere? We view this as the most important challenge in space weather. We discuss the case for magnetic clouds (MCs), interplanetary sheaths upstream of interplanetary coronal mass ejections (ICMEs), corotating interaction regions (CIRs) and solar wind high-speed streams (HSSs). The sheath- and CIR-related magnetic storms will be difficult to predict and will require better knowledge of the slow solar wind and modeling to solve. For interplanetary space weather, there are challenges for understanding the fluences and spectra of solar energetic particles (SEPs). This will require better knowledge of interplanetary shock properties as they propagate and evolve going from the Sun to 1 AU (and beyond), the upstream slow solar wind and energetic “seed” particles. Dayside aurora, triggering of nightside substorms, and formation of new radiation belts can all be caused by shock and interplanetary ram pressure impingements onto the Earth's magnetosphere. The acceleration and loss of relativistic magnetospheric “killer” electrons and prompt penetrating electric fields in terms of causing positive and negative ionospheric storms are reasonably well understood, but refinements are still needed. The forecasting of extreme events (extreme shocks, extreme solar energetic particle events, and extreme geomagnetic storms (Carrington events or greater)) are also discussed. Energetic particle precipitation into the atmosphere and ozone destruction are briefly discussed. For many of the studies, the Parker Solar Probe, Solar Orbiter, Magnetospheric Multiscale Mission (MMS), Arase, and SWARM data will be useful.

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A review of the SCOSTEP’s 5-year scientific program VarSITI—Variability of the Sun and Its Terrestrial Impact

Progress in Earth and Planetary Science ◽

10.1186/s40645-021-00410-1 ◽

2021 ◽

Vol 8 (1) ◽

Author(s):

Kazuo Shiokawa ◽

Katya Georgieva

Keyword(s):

Solar Wind ◽

Interplanetary Space ◽

Solar Wind Plasma ◽

The Sun ◽

Scientific Program ◽

Solar Cycles ◽

Grand Minimum ◽

The Earth ◽

Earth Connection ◽

Near Future

AbstractThe Sun is a variable active-dynamo star, emitting radiation in all wavelengths and solar-wind plasma to the interplanetary space. The Earth is immersed in this radiation and solar wind, showing various responses in geospace and atmosphere. This Sun–Earth connection variates in time scales from milli-seconds to millennia and beyond. The solar activity, which has a ~11-year periodicity, is gradually declining in recent three solar cycles, suggesting a possibility of a grand minimum in near future. VarSITI—variability of the Sun and its terrestrial impact—was the 5-year program of the scientific committee on solar-terrestrial physics (SCOSTEP) in 2014–2018, focusing on this variability of the Sun and its consequences on the Earth. This paper reviews some background of SCOSTEP and its past programs, achievements of the 5-year VarSITI program, and remaining outstanding questions after VarSITI.

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A Data-driven Model of the Solar Wind, Interstellar Pickup Ions, and Turbulence throughout Interplanetary Space

10.1002/essoar.b60497724eca58de.7c985d5380f54d2b.1 ◽

2018 ◽

Author(s):

Tae Kim ◽

Igor Kryukov ◽

Nikolai Pogorelov ◽

Heather Elliott ◽

Gary Zank

Keyword(s):

Solar Wind ◽

Interplanetary Space ◽

Data Driven ◽

Pickup Ions

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Nonlinear two-fluid hydromagnetic waves in the solar wind: Rotational discontinuity, soliton, and finite-extent Alfvén wave train solutions

Journal of Geophysical Research Atmospheres ◽

10.1029/ja094ia06p06523 ◽

1989 ◽

Vol 94 (A6) ◽

pp. 6523-6538 ◽

Cited By ~ 20

Author(s):

L. H. Lyu ◽

J. R. Kan

Keyword(s):

Solar Wind ◽

Wave Train ◽

Alfven Wave ◽

Rotational Discontinuity ◽

Hydromagnetic Waves ◽

Finite Extent ◽

Two Fluid

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Space weather: the solar perspective

Living Reviews in Solar Physics ◽

10.1007/s41116-021-00030-3 ◽

2021 ◽

Vol 18 (1) ◽

Author(s):

Manuela Temmer

Keyword(s):

Solar Wind ◽

Space Weather ◽

Weather Forecasting ◽

Interplanetary Space ◽

Three Dimensions ◽

Space Weather Forecasting ◽

Stereo Mission ◽

Interaction Regions ◽

Near Future ◽

First Time

AbstractThe Sun, as an active star, is the driver of energetic phenomena that structure interplanetary space and affect planetary atmospheres. The effects of Space Weather on Earth and the solar system is of increasing importance as human spaceflight is preparing for lunar and Mars missions. This review is focusing on the solar perspective of the Space Weather relevant phenomena, coronal mass ejections (CMEs), flares, solar energetic particles (SEPs), and solar wind stream interaction regions (SIR). With the advent of the STEREO mission (launched in 2006), literally, new perspectives were provided that enabled for the first time to study coronal structures and the evolution of activity phenomena in three dimensions. New imaging capabilities, covering the entire Sun-Earth distance range, allowed to seamlessly connect CMEs and their interplanetary counterparts measured in-situ (so called ICMEs). This vastly increased our knowledge and understanding of the dynamics of interplanetary space due to solar activity and fostered the development of Space Weather forecasting models. Moreover, we are facing challenging times gathering new data from two extraordinary missions, NASA’s Parker Solar Probe (launched in 2018) and ESA’s Solar Orbiter (launched in 2020), that will in the near future provide more detailed insight into the solar wind evolution and image CMEs from view points never approached before. The current review builds upon the Living Reviews article by Schwenn from 2006, updating on the Space Weather relevant CME-flare-SEP phenomena from the solar perspective, as observed from multiple viewpoints and their concomitant solar surface signatures.

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Empirical inner boundary conditions and rotation rates for solar wind models

10.5194/egusphere-egu21-782 ◽

2021 ◽

Author(s):

Huw Morgan

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Boundary Conditions ◽

Coronal Magnetic Field ◽

Height Range ◽

Rotation Rates ◽

Wind Structure ◽

Solar Wind Structure ◽

Coronal Electron ◽

Made In

<p>To date, the inner boundary conditions for solar wind models are either directly or indirectly based on magnetic field extrapolation models of the photosphere. Furthermore, between the photosphere and Earth, there are no other direct empirical constraints on models. New breakthroughs in coronal rotation tomography, applied to coronagraph observations, allow maps of the coronal electron density to be made in the heliocentric height range 4-12 solar radii (Rs). We show that these maps (i) give a new empirical boundary condition for solar wind structure at a height where the coronal magnetic field has become radial, thus avoiding the need to model the complex inner coronal magnetic field, and (ii) give accurate rotation rates for the corona, of crucial importance to the accuracy of solar wind models and forecasts.</p>

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Solar cycle changes of large-scale solar wind structure

Proceedings of the International Astronomical Union ◽

10.1017/s1743921309992912 ◽

2009 ◽

Vol 5 (S264) ◽

pp. 356-358 ◽

Cited By ~ 3

Author(s):

P. K. Manoharan

Keyword(s):

Solar Wind ◽

Solar Cycle ◽

Large Scale ◽

Interplanetary Space ◽

The Sun ◽

Wind Structure ◽

Level Of Activity ◽

Solar Wind Structure ◽

Current Minimum ◽

Inner Heliosphere

AbstractIn this paper, I present the results on large-scale evolution of density turbulence of solar wind in the inner heliosphere during 1985–2009. At a given distance from the Sun, the density turbulence is maximum around the maximum phase of the solar cycle and it reduces to ~70%, near the minimum phase. However, in the current minimum of solar activity, the level of turbulence has gradually decreased, starting from the year 2005, to the present level of ~30%. These results suggest that the source of solar wind changes globally, with the important implication that the supply of mass and energy from the Sun to the interplanetary space has significantly reduced in the present low level of activity.

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