Interplanetary Field Research Articles

Westward ionospheric electric field perturbations on the dayside associated with substorm processes

A controversy has risen in the direction of ionospheric electric field perturbation on the dayside caused by substorm expansion phase in recent years, i.e., eastward or westward. To exclude the effect of interplanetary magnetic field northward turning, the substorms without interplanetary field (IMF) trigger are required to investigate this issue. Previous works, such as that by Huang et al. (2004), showed that the eastward electric field perturbations caused by substorms can be observed. However, our case suggests that some substorms can produce strong westward electric field perturbations and drive westward equatorial electrojets on the dayside ionosphere. This westward electric field is created by an overshielding‐like imbalance state of field‐aligned currents (FACs), Region 2 (R2) FAC greater than Region 1 (R1) FAC, which is built up through R2 FAC enhancement rather than R1 FAC reduction due to IMF northward turning. The substorm processes should be responsible for the westward electric field especially through polar cap shrinkage and magnetic field dipolarization.

Other climate-change inputs

A vigorous round of correspondence appeared in Physics Today (October 2008, page 10) regarding the Opinion piece “Is Climate Sensitive to Solar Variability?” by Nicola Scafetta and Bruce West (Physics Today, March 2008, page 50). One letter writer, Peter Foukal, pointed out that neither total nor UV solar irradiance can account for most of the climate variance that correlates with solar activity. In view of the quantitative problems in using irradiance to account for the correlated climate variations, the question can be asked, Are the cosmic-ray variations, which are mostly due to solar activity, themselves drivers of climate change, or are they—as generally assumed—merely proxies for irradiance variations?Not mentioned in the discussion was observational evidence for greater long-term and short-term climate sensitivity to solar activity than irradiance can account for. Proxies for climate change on the centennial and millennial time scales—proxies such as glacier-carried debris and the oxygen-18 isotope—show strong correlations with the cosmic-ray-generated cosmogenic isotopes carbon-14 and beryllium-10 in stratified geological repositories. 1 1. G. Bond et al. , Science 294, 2130 (2001), and references therein. https://doi.org/10.1126/science.1065680 One little-known mechanism coupling solar activity to the atmosphere has been shown to respond to cosmic-ray changes as well as to other inputs, as documented and reviewed in recent publications. 2 2. G. B. Burns et al. , J. Geophys. Res. 113, D15112 (2008), https://doi.org/10.1029/2007JD009618 , 3 3. B. A. Tinsley, Rep. Prog. Phys. 71, 066801 (2008). https://doi.org/10.1088/0034–4885/71/6/066801 Clear evidence of meteorological responses, including changes in cloud cover, has been reported for five disparate short-term solar or terrestrial inputs that modulate the flow of the downward electric current density Jz of the global electric circuit through the atmosphere. For example, recent analysis of measurements in both the Antarctic and Arctic high-magnetic-latitude regions shows correlations between surface pressure and the north–south component of the interplanetary electric field. Changes in Jz due to low-latitude thunderstorms produce a similar effect on polar surface pressure. 2 2. G. B. Burns et al. , J. Geophys. Res. 113, D15112 (2008), https://doi.org/10.1029/2007JD009618 There are other consistent, statistically significant atmospheric responses to the effects of cosmic-ray, solar-proton, and relativistic-electron precipitation on J z. 3 3. B. A. Tinsley, Rep. Prog. Phys. 71, 066801 (2008). https://doi.org/10.1088/0034–4885/71/6/066801 The Jz flow deposits electric charge on droplets and aerosol particles in gradients of droplet concentration, humidity, and, therefore, resistivity in clouds in accordance with Ohm’s law and Gauss’s law. Such charges could affect clouds through the scavenging rates for cloud-condensation and ice-forming nuclei. Consequent changes in the concentration of such nuclei and in ice-nucleation rates can affect droplet concentration, precipitation rate, and cloud cover and can potentially explain the observations. But to model the effects of the cloud changes on global mean temperature on the century time scale, it will be necessary to separately evaluate the effects of solar-induced Jz changes on clouds at low and high altitudes, at high and low latitudes, over ocean and land, by day and night, and for stratus versus cumulus clouds. Such work has not been done, but uncertainties appear much larger than those shown for the solar irradiance effect in the reports of the Intergovernmental Panel on Climate Change, and can thus accommodate the observed changes in global temperature that correlate with solar activity. REFERENCESSection:ChooseTop of pageREFERENCES <<1. G. Bond et al. , Science 294, 2130 (2001), and references therein. https://doi.org/10.1126/science.1065680 , Google ScholarCrossref2. G. B. Burns et al. , J. Geophys. Res. 113, D15112 (2008), https://doi.org/10.1029/2007JD009618 , Google ScholarCrossref3. B. A. Tinsley, Rep. Prog. Phys. 71, 066801 (2008). https://doi.org/10.1088/0034–4885/71/6/066801 , Google ScholarCrossref© 2009 American Institute of Physics.

On the SuperDARN cross polar cap potential saturation effect

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 threshold values starting from which the non-linearity was evident were estimated to be IEF*~EKL*~3 mV/m, PCN*~3–4, and EC*~1.5×104. The data indicate that saturation starts at larger values of the above parameters and reaches larger (up to 10 kV) saturation levels during summer. Conclusions are supported by a limited data set of simultaneous SuperDARN observations in the Northern (summer) and Southern (winter) Hemispheres. It is argued that the SuperDARN CPCP saturation levels and the thresholds for the non-linearity to be seen are affected by the method of the CPCP estimates.

Evolution of the large-scale magnetic field over three solar cycles

AbstractObservations of the large-scale magnetic field show that the current extended solar cycle minimum is different from the three previous well-observed minima. The weaker polar fields increase the relative influence of middle and low-latitude flux patterns on the configuration of the corona and heliosphere. A much larger portion of the open flux originates in equatorial coronal holes. Even though the mean magnetic field of the Sun as a star is the weakest since measurements began, the sector structure of the interplanetary field, though smaller in magnitude, reached fairly high latitude until 2009. The emergence of active regions through the cycle and transport of flux from low to high latitudes also show quite different patterns, providing insight into the dynamo that drives the cycle. Long records of synoptic observations provide a rich source of information about solar activity that must be maintained.

On the response of the equatorial and low latitude ionospheric regions in the Indian sector to the large magnetic disturbance of 29 October 2003

Abstract. The present paper investigates the response of the equatorial and low latitude ionosphere over the Indian longitudes to the events on 29 October 2003 using ionosonde data at Trivandrum (8.5° N (0.5° N geomagnetic), 77° E) and SHAR (13.7° N (5.7° N geomagnetic), 80.2° E), ground-based magnetometer data from Trivandrum and Total Electron Content (TEC) derived from GPS data at the locations of Ahmedabad (23° N (15° N geomagnetic), 72° E), Jodhpur (26.3° N (18.3° N geomagnetic), 73° E) and Delhi (28° N (20° N geomagnetic), 77° E). Following the storm sudden commencement, the TEC at all the three stations showed an overall enhancement in association with episodes of inter-planetary electric field penetration. Interestingly, real ionospheric height profiles derived using the ionosonde data at both Trivandrum and SHAR showed significant short-term excursions and recoveries. In the post noon sector, these features are more pronounced over SHAR, an off equatorial station, than those over Trivandrum indicating the increased effects of neutral winds.

Relationship between the PC and AL indices during repetitive bay-like magnetic disturbances in the auroral zone

To study the relations of the polar cap (PC) magnetic activity (characterized by the PC index) to magnetic disturbances in the auroral zone (AL index) the behavior of 62 repetitive bay-like magnetic disturbances has been analyzed. It was found that the PC index, derived as a proxy of the geoeffective interplanetary electric field Em, starts to increase, on average, about 30 min ahead of the magnetic disturbance onset. Value of Em and PC∼2 mV/m seems to be necessary for development of the repetitive bay-like disturbances with peak AL exceeding 400 nT. Growth phase duration (the time interval between the start of PC increase and AL sudden onset) and intensity of magnetic disturbances in the auroral zone (AL max) highly correlate with the PC growth rate. The growth phase reduces to a few minutes, if the PC index suddenly jumps above ∼6–8 mV/m. The sharp development of Birkeland current wedge during expansion phase insignificantly influences the polar cap activity: the corresponding PC index increase does not exceed 10–20% of the PC value. It is concluded that the PC index may be considered as a convenient proxy of the solar wind energy input into the magnetosphere.

On the origin of pre-reversal enhancement of the zonal equatorial electric field

Abstract. In November 2004, a large and variable interplanetary electric field (IEF) was felt in the reference frame of the Earth. This electric field penetrated to the magnetic equator and, when the Jicamarca Radio Observatory (JRO) was in the dusk sector, resulted in a reversal of the normal zonal component of the field. In turn, this caused a counter-electrojet (CEJ), a westward current rather than the usual eastward current. At the time of the normal pre-reversal enhancement (PRE) of the eastward field, the Jicamarca incoherent scatter radar (ISR) observed that the westward component became even more westward. Two of the three current explanations for the PRE depend on the neutral wind patterns. However, this unique event was such that the neutral wind-driven dynamos could not have changed. The implication is that the Haerendel-Eccles mechanism, which involves partial closure of the equatorial electrojet (EEJ) after sunset, must be the dominant mechanism for the PRE.

Study of the long‐term variability of interplanetary plasma and fields as a link for solar‐terrestrial relationships

Often the interplanetary parameters used for the study of solar‐terrestrial relationships are solar wind speed (V), the total interplanetary magnetic field (B), and the southward component of IMF (Bz). Both hourly and daily values of these parameters have usually been employed to associate with parameters defining terrestrial effects. For our study, we have used the daily values of the interplanetary indices (V, B, and Bz), as well as the daily values of the geomagnetic disturbance index Ap, for the years 1965–2007. The long‐term averages have been calculated for the days when simultaneous data are available for all the four parameters (V, B, Bz, and Ap). These include their yearly averages, as well as the averages on the basis of the phases of the solar activity cycle. The statistical relationship between them has been investigated on these long‐term averages, as well as on the day‐to‐day basis. These sets have been further divided and studied on the basis of days with Bz being &lt;0 or ≥0. The results obtained can be summarized as follows: (1) the magnitudes of the values of Ap are observed to be always enhanced significantly for the case of Bz &lt; 0, as compared to days with Bz ≥ 0, and (2) V versus Ap has always low values of correlation coefficient (r). (3) On the contrary, B versus Ap has high values of “r”; (4) the product of V and B versus Ap always yields much better correlations than for V or B alone, either on an average basis or on a day‐to‐day basis, and (5) although, the long‐term variations of V are not very significant, the variations of B follow solar activity cycle and has a continuously increasing trend during the solar cycles 20 and 21. The statistical results obtained here signify that the product of V and B is more significantly effective in producing large‐scale geomagnetic disturbances.

Dynamics of North American sector ionospheric and thermospheric response during the November 2004 superstorm

We present a study of ionospheric and thermospheric response during a November 9–10, 2004 major geomagnetic storm event (DsT ∼−300 nT). We utilize the North American sector longitude chain of incoherent scatter radars at Arecibo, Millstone Hill, and Sondrestrom, operating as part of a coordinated international mesosphere/lower thermosphere coupling study experiment. Total electron content (TEC) determinations from global positioning system (GPS) ground receivers, ground magnetometer traces from the Canadian CANOPUS array, Defense Meteorological Satellite Platform (DMSP) topside data, and global convection patterns from the SuperDARN radar network are analyzed to place the detailed radar data in proper mesoscale context. The plasmaspheric boundary layer (PBL) expanded greatly in the dusk sector during ring current intensification to span more than 25° of magnetic latitude, reaching as far south as 30° invariant latitude. Strong sub-auroral polarization stream velocities of more than 1 km/s were accompanied by large upwards thermal O+ fluxes to the overlying magnetosphere. The large PBL expansion subsequently exposed both Millstone Hill and Sondrestrom to the auroral convection pattern, which developed a complex multicell and reverse convection response under strongly northward IMF conditions during a period of global interplanetary electric field penetration. Large traveling atmospheric and ionospheric disturbances caused significant neutral wind and ion velocity surges in the mid-latitude and tropical ionosphere and thermosphere, with substorm activity launching equatorward neutral wind enhancements and subsequent mid-latitude dynamo responses at Millstone Hill. However, ionosphere and thermosphere observations at Arecibo point to significant disturbance propagation modification in the post-dusk sector PBL region.

UNDERSTANDING THE GEOMAGNETIC PRECURSOR OF THE SOLAR CYCLE

Geomagnetic activity late in the sunspot cycle has been used successfully to forecast the amplitude of the following cycle. This success is somewhat surprising, however, because the recurrent high-speed wind streams that trigger the activity are not proxies of the Sun's polar fields, whose strength is a critical factor in many solar dynamo models. Instead, recurrent geomagnetic activity signals increases in the Sun's equatorial dipole moment, which decays on the ~1-2 yr timescale of the surface meridional flow and does not survive into the next cycle. In accordance with the original empirical method of Ohl, we therefore argue that solar cycle predictions should be based on the minimum level of geomagnetic activity, which is determined by the Sun's axial dipole strength, not on the peak activity during the declining phase of the cycle. On physical grounds, we suggest that an even better indicator would be the total open flux (or strength of the radial interplanetary field component) at sunspot minimum, which in turn can be derived from the historical aa index by removing the contribution of the solar wind speed. This predictor yields a peak yearly sunspot number R max = 97 ± 25 for solar cycle 24.

Dayside ionospheric uplift during strong geomagnetic storms as detected by the CHAMP, SAC-C, TOPEX and Jason-1 satellites

Ionosphere response to severe geomagnetic storms that occurred in 2001–2003 was analyzed using data of global ionosphere maps (GIM), altimeter data from the Jason-1 and TOPEX satellites, and data of GPS receivers on-board CHAMP and SAC-C satellites. This allowed us to study in detail ionosphere redistribution due to geomagnetic storms, dayside ionospheric uplift and overall dayside TEC increase. It is shown that after the interplanetary magnetic field turns southward and intensifies, the crests of the equatorial ionization anomaly (EIA) travel poleward and the TEC value within the EIA area increases significantly (up to ∼50%). GPS data from the SAC-C satellite show that during the main phase of geomagnetic storms TEC values above the altitude of 715 km are 2–3 times higher than during undisturbed conditions. These effects of dayside ionospheric uplift occur owing to the “super-fountain effect” and last few hours while the enhanced interplanetary electric field impinged on the magnetopause.

Low-latitude geomagnetic response to the interplanetary conditions during very intense magnetic storms

The variations in the horizontal and declination components of the geomagnetic field in response to the interplanetary shocks driven by fast halo coronal mass ejections, fast solar wind streams from the coronal hole regions and the dynamic pressure pulses associated with these events are studied. Close association between the field-aligned current density ( j ∥) and the fluctuations in the declination component (Δ D ABG) at Alibag is found for intense storm conditions. Increase in the dawn-dusk interplanetary electric field ( E y ) and Δ D ABG are generally in phase. However, when the magnetospheric electric field is directed from dusk to dawn direction, a prominent scatter occurs between the two. It is suggested that low-latitude ground magnetic data may serve as a proxy for the interplanetary conditions in the solar wind.

Geoeffectiveness of magnetic cloud, shock/sheath, interaction region, high-speed stream and their combined occurrence

A subset of CMEs, called interplanetary magnetic clouds (MCs), are observed to have systematic rotation [northward to southward (NS) or southward to northward (SN)] in their field structures. These MCs identified in the heliospheric plasma and field data at 1 AU may have different features associated with them. These structures (NS/SN) may be isolated MC moving with the ambient solar wind. MCs (NS/SN) may also be associated with shock/sheath region, formed due to compression of the ambient plasma/field ahead of them. A fraction from each of these four types of MCs have additional features, being ‘pushed’ by fast solar wind streams from coronal holes, forming interaction region (IR) between MCs and high-speed solar wind streams (HSS). Using these different sets of MCs, we have done a detailed study of the geoeffectiveness of NS and SN turning MCs and their associated features (shock/sheath, IR and HSS). To study the process that produces the geomagnetic disturbances and influences its amplitude/duration, we have utilized the interplanetary plasma and field parameters, namely, plasma velocity, density, temperature, pressure, field strength and its north–south component, during the passage of these structures with different associated properties. Differences in the geoeffectiveness of MCs with different structural and dynamical properties have been identified. The possible role of high-speed stream in influencing the recovery time (and hence duration) of geomagnetic disturbance has also been investigated. A best-fit equation representing the relation between level of the geomagnetic activity (due to MCs) and interplanetary plasma/field parameter has been obtained.

Penetration characteristics of the interplanetary electric field to the daytime equatorial ionosphere

Using 8 years of ionospheric drift measurements from the low‐latitude JULIA (Jicamarca Unattended Long‐term Investigations of the Ionosphere and Atmosphere) radar and the solar wind and interplanetary magnetic field data from the ACE (Advance Composition Explorer) satellite, we study the characteristics of the prompt penetration of electric fields to the equatorial ionosphere. A large database allowed us to bring out statistically significant characteristics of electric field penetration as a function of frequency. The coherence between the interplanetary electric field (IEF) and the equatorial electric field (EEF) peaks around a 2‐hour period with a maximum magnitude squared coherence of 0.6. The coherence is slightly higher (0.7) on magnetically active (Ap &gt; 20) days. The cross‐phase spectra between the ACE and JULIA variations, after elimination of the propagation delay, have negligible values. Correspondingly, the time shift between IEF and EEF is less than 5 minutes at all periods. We also find that the penetration efficiency is highest during local noon, as compared with that of morning and evening hours. The coherence is lower for days with high solar flux values. We find that the penetration of electric fields into the equatorial ionosphere has no significant dependence on season and on the polarity of IMF Bz. We propose a transfer function between IEF and EEF, which was validated on synthetic as well as observed IEF data. The use of this transfer function decreases the misfit of a climatological model with the measured equatorial electric field by 27%.

Roles of interplanetary and geomagnetic parameters in ‘intense’ and ‘very intense’ magnetic storms generation and their geoeffectiveness

This paper studies the probable roles of interplanetary and geomagnetic parameters in the generation of ‘intense’ and ‘very intense’ magnetic storms as well as the correlation between magnetic field B and flow speed V , southward turning of Bz ( Bs ) and Bs duration BT . 18 storm events were observed and for analysis were divided into two sections. This include 8 ‘intense’ magnetic storm (−250 nT ≤ peak Dst < −100 nT) events and 10 ‘Very intense’ storms (peak Dst < −250 nT); both spanning January 1976 until May 2005. From our analysis, it was observed that the interplanetary magnetic field Bz plays a prominent role alongside Dst in the generation of intense storms. So also is the interplanetary electric field associated with high-speed streams and the solar wind density Np in the ring current intensification. The result further shows that over 67% of the storm events under investigation are generated from magnetic clouds which are characterized by a low beta plasma, high IMF magnitude and large scale coherent field rotations often including large and steady north-south components.As regards the geoeffectiveness of the flow speed V , the Bs and Bs interval ( BT ) with the magnetic field B , it was observed that generally for all the selected storm events, the flow speed is the most correlated, showing a correlation coefficient of 50.9% with B, and hence the most geoeffective. However, the statistical significance of its correlation with B is not so directly implying a higher substorm occurrence during the faster solar wind, but that it is one of the causes of substorm occurrence at a value faster than 400 km/s. Furthermore, the result shows that ‘very intense’ storms whose main feature is a plasma flow speed greater than 550 km/s has a negligible or very low correlation between the flow speed and the magnetic field B ; whereas, ‘intense’ storms have a 58.7% correlation between the two parameters. Lastly, it could be argued that all ‘very intense’ storms are likely to have a plasma flow speed greater than 550 km/s within the storm interval, but not all flow speed greater than 550 km/s are ‘very intense’ storms.

Heliospheric sector boundaries: Single or multiple?

Solar wind data were examined for a period when the Ulysses spacecraft moved roughly parallel to the boundary between inward and outward interplanetary fields at a solar distance of 1.4 AU. Multiple crossings of the magnetic sector boundary were observed. Three tests were used to evaluate whether or not the crossings were due to multiple crossings of a single surface or single crossings of separate surfaces: (1) a correlation between the latitude and longitude directions of the normals to the surface, (2) the radius of curvature of the surface calculated from consecutive crossings, and (3) the variation of plasma parameters across the surfaces. Both multiple crossings of a single rippled surface and single crossings of multiple boundary surfaces were observed.

Access of solar wind electrons into the Martian magnetosphere

Abstract. Electrons with energy of ~40–80 eV measured by the instrument ASPERA-3 on Mars Express and MAG-ER onboard Mars Global Surveyor are used to trace an access of solar wind electrons into the Martian magnetosphere. Crustal magnetic fields create an additional protection from solar wind plasma on the dayside of the Southern Hemisphere by shifting the boundary of the induced magnetosphere (this boundary is often refereed as the magnetic pileup boundary) above strong crustal sources to ~400 km as compared to the Northern Hemisphere. Localized intrusions through cusps are also observed. On the nightside an access into the magnetosphere depends on the IMF orientation. Negative values of the ByIMF component assist the access to the regions with strong crustal magnetizations although electron fluxes are strongly weakened below ~600 km. A precipitation pattern at lower altitudes is formed by intermittent regions with reduced and enhanced electron fluxes. The precipitation sites are longitudinally stretched narrow bands in the regions with a strong vertical component of the crustal field. Fluxes ≥109 cm−2 s−1 of suprathermal electrons necessary to explain the observed aurora emissions are maintained only for the periods with enhanced precipitation. The appearance of another class of electron distributions – inverted V structures, characterized by peaks on energy spectra, is controlled by the IMF. They are clustered in the hemisphere pointed by the interplanetary electric field that implies a constraint on their origin.

Continuous penetration of the interplanetary electric field to the equatorial ionosphere over eight hours during intense geomagnetic storms

The interplanetary electric field penetrates to the low‐latitude ionosphere and has significant influence on the ionospheric electrodynamics during intense geomagnetic storms. It is critical to understand how much of the interplanetary electric field can penetrate to the ionosphere and how long penetration electric fields can exist. In this study, we present the Defense Meteorological Satellite Program (DMSP) satellite measurements of the equatorial ionospheric ion vertical velocity in the dusk sector during two intense geomagnetic storms. We find that the equatorial ionospheric electric field at dusk is approximately proportional to the interplanetary electric field for 8–10 hours during the storm main phase. The penetration efficiency is relatively constant over the entire interval and is 5% at dusk in one storm case. The long‐lasting storm‐time penetration electric field causes significant redistribution of the ionospheric plasma. This study reveals that penetration electric fields can last for 8–10 hours without effective shielding when the magnetic storm activity is strengthening during continuous southward interplanetary magnetic field. The result implies that the interplanetary electric field is linearly coupled with the dusk equatorial ionosphere during the entire main phase of intense magnetic storms, which is very important for understanding the storm‐time ionospheric electric field and electrodynamics.

On the Solar Origins of Open Magnetic Fields in the Heliosphere

A combination of heliospheric and solar data was used to identify open magnetic fields stretching from the lower corona to Earth orbit. 35 near-relativistic electron beams detected at the ACE spacecraft the heliospheric segments of the open fields. An X-ray flare occurred <20 minutes before injection of the electrons in 25 events. These flares labeled the solar segment of the open fields. The flares occurred in western-hemisphere active regions (ARs) with coronal holes whose polarity agreed with the polarity of the beam-carrying interplanetary fields in 23 of the 25 events. We conclude that electron beams reach 1 AU from open AR fields adjacent to flare sites. The Wang & Sheeley implementation of the potential-field source-surface model successfully identified the open fields in 36% of cases. Success meant that the open fields reached the source surface within 3 heliographic deg of the interplanetary magnetic field connected to ACE at 1 AU. Inclusion of five near misses improves the success rate to 56%. The success rate for the Schrijver & DeRosa PFSS implementation was 50%. Our results suggest that, even if the input magnetic data are updated frequently, the PFSS models succeed in only ~50% of cases to identify the coronal segment of open fields. Development of other techniques is in its infancy.

Solar wind influence on atmospheric processes in winter Antarctica

Galactic cosmic rays (GCRs) altered by solar wind are traditionally regarded as the most plausible agent of solar activity influence on the Earth's atmosphere. However, it is well known that severe reductions in the GCRs flux, known as Forbush decreases (FDs), are caused by solar wind of high speed and density, which sweeps away the GCRs on its way. Since the FD beginnings are registered at the Earth's orbit simultaneously with dramatic disturbances in the solar wind, the atmospheric effects, assigned to FDs, can be, in reality, the results of the solar wind influence on the atmospheric processes. This paper presents a summary of the experimental results demonstrating the strong influence of the interplanetary electric field on atmospheric processes in central Antarctica, where the large-scale system of vertical circulation is formed during winter seasons. The influence is realized through acceleration of the air masses, descending into the lower atmosphere from the troposphere, and the formation of cloudiness above the Antarctic Ridge, where the descending air masses enter the surface layer. The acceleration is followed by a sharp increase of the atmospheric pressure near-pole region, which gives rise to the katabatic wind strengthening above the entire Antarctica. The cloudiness formation results in the sudden warmings in the surface atmosphere, since the cloud layer efficiently backscatters the long wavelength radiation from the ice sheet, but does not affect the adiabatic warming process of the descending tropospheric air masses. When the drainage flow strengthening the circumpolar vortex around the periphery of the Antarctic continent decays, the surface easterlies typical of the coast stations during the winter season are replaced by southerlies and the cold Antarctic air masses flow out to the Southern ocean.