Interball Tail Probe Research Articles

ANISOTROPY OF THE BACKGROUND MICROWAVE RADIATION OF THE UNIVERSE AND MASSIVE PHOTON PAIRS

The paper considers the issue of the anomalously low temperature dispersion of the cosmic microwave background (CMB) of the Universe, which was discovered by researchers R. Penrose and V. Gurzadyan according to the data of the WMAP and Planck missions. A new explanation of this phenomenon is given as evidence of residual traces in the CMB after the occurrence of multiple instabilities in the vacuum phase of matter in the first moments of the development of our Universe. It is these instabilities that have become the centers of the emergence of the fundamental mass of matter – massive photon pairs (ultralight scalar bosons). Theoretical and experimental evidence of the connection of CMB with massive photon pairs is presented using data from the Interball-Tail Probe, RHESSI and XMM-Newton missions.

Variations in the X-ray Intensity of the Solar Corona and Heating of the Coronal Plasma in the Context of the Quantum Theory of Photon Pairs

Data obtained in the framework of the INTERBALL–Tail Probe (1995–2000) and RHESSI (from 2002 to the present) projects have revealed variations in the X-ray intensity of the solar corona in the photon energy range of 2−15 keV during the period of the quiet Sun. Previously, a hypothesis was proposed that this phenomenon could be associated with the effect of coronal heating. In the present study, a new mechanism of coronal plasma heating is proposed on the basis of the experimental data and the quantum theory of photon pairs that are produced from vacuum in the course of the Universe’s expansion. A similar mechanism based on the splitting of photon pairs in the interplanetary and intergalactic space is also proposed to explain the observed microwave background radiation.

Observation of narrow energy spectrum electron flows on the INTERBALL Tail Probe and their possible relation with the spacecraft charging

The paper describes cases of observations of narrow energy spectrum electron flows up to 500 eV on the INTERBALL Tail Probe. About 30 events were registered in 1996 on the night side of the Earth predominantly in 03h–06h local time sector. Quasimonochromatic electrons (QME) were registered by all 8 spectrometer channels oriented along the spacecraft meridian with angles of the field of view centers relative to sunward direction from 11° to 169°. Quasimonochromatic electrons were observed simultaneously with large fluxes of high temperature magnetospheric electrons. The dependences of QME energy on both fluxes and energy of high-energy magnetospheric electrons were observed in every event. The ratio of full width at half height (FWHH) to mean energy of QME was ~20%. This electron component with quasimonochromatic energy probably was originated on the spacecraft surface. The registered energy of QME was apparently due to difference of potentials between spacecraft surface from which electron beam originated and the location of electron spectrometer.

Weak solar events

Soft X-ray solar bursts were investigated in the framework of the Interball—Tail Probe project by using an RF-15I-2 X-ray photometer. When studying microflares over the period from September to December 1995, weak bursts with intensities of less than 10−8 W/m2 were detected. All these data are confirmed by observations performed in the framework of the GOES project. The characteristics of solar microflares were determined, and the physical mechanism of weak solar events was considered. The distribution of microflares over their intensities was obtained. It is found that the distribution of solar flares over released energies do not obey a power law, and a lower limit is revealed in this distribution. This result is confirmed by the data obtained in the framework of the RHESSI project. Correlation between the daily average values of the maximum intensities of X-ray bursts of different classes of microflares and the daily average values of the thermal background of the solar corona is revealed.

A Panoramic Plasma Spectrometer: An All-Sky Camera for Charged Particles

The necessity of the high temporal resolution measurements of the complete velocity distribution function of charged particles in space leads to the invention of analyzers of new types including top-hat analyzers [2] for operation onboard rotating spacecraft and instruments with electrostatic scanning [3] for operation onboard slowly rotating spacecraft or onboard spacecraft with tri-axial stabilization. The instrument SKA-1 with electrostatic scanning [3] mounted on the Interball Tail Probe satellite had a temporal resolution of 10 s. There were two electrostatic mirrors and 36 Thomson parabola analyzers in the mass-spectrometer FONEMA for the Mars-96 mission [4], which guaranteed full coverage of 4 π angle and a temporal resolution of ~0.2 s. However, the failure of launching the Mars96 project did not allow one to use this unique instrument. The highest temporal resolution in measurements of the three-dimensional velocity distribution function of charged particles ( ~3 s) is achieved by employing a tophat analyzer on a rotating spacecraft. In this case, the temporal resolution is determined by the velocity of rotation of a spacecraft around its axis. Further improvement of the temporal resolution requires either arrangement of many detectors (which in turn causes many technical problems) or employment of new approaches. Earlier [1] we proposed a miniature electro-optic system that guarantees complete 2 π field of view ( 4 π with two analyzers) with a single coordinate-sensitive detector: an all-sky camera for charged particles. The feed optics can be modified for specific conditions of experiments and for different analyzers of the second stage. The suggested concept can guarantee very fast, flexible, and complete three-dimensional measurements of charged particles (ions or electrons).

The ion differential spectra in outer boundary of the ring current: November 17, 1995 case study

The analysis of the ion spectra variations is presented for the particles in the energy range from 0.5 keV to 3 MeV during INTERBALL-Tail Probe crossing of the plasma sheet-ring current region on November 17, 1995. The CORALL, DOK-2 and SKA-2 instrument data were used for spectra restoring. It is shown ion spectra have the same smooth shape (with the averaging time ∼2 min ) by traversing the satellite from 20 R e up to 6 R e . In particular, the spectra shape was almost constant with decreasing of geocentric distance from R e =11 to 6. Possible reasons of spectra variations are discussed.

Turbulence in the Plasma Sheet during Substorms: A Case Study for Three Events Observed by the INTERBALL Tail Probe

Variations of turbulence properties of the plasma sheet during geomagnetic substorms are investigated using observations of the INTERBALLTail Probe satellite. The periods are chosen when the satellite was inside the plasma sheet. Fluctuations of the plasma bulk velocity across the plasma sheet are studied for the growth, expansion, and recovery phases of geomagnetic substorms on October 14, 1997; October 30, 1997; and December 16, 1998. It was demonstrated that the level of turbulence increases considerably after the onset of the substorm expansion phase and slowly decreases nearly to the presubstorm level later. The correlation times of plasma fluctuations in the Z-direction are estimated, and diffusion coefficients in the Z-direction are calculated.

The Structure of Ion Spectra in Outer Regions of the Ring Current: The November 13, 1995 Event

We present the results on variations of ion spectra in the energy range from 1 keV to 3 MeV. The spectra measured onboard the INTERBALL Tail Probe satellite on November 13, 1995, during the satellite's passage from the dipole field lines to the lines stretched into the magnetotail are analyzed. The data of the CORALL, DOK-2, and SKA-2 instruments are used to reconstruct the ion spectra. It is shown that, when the ion spectrum along the satellite trajectory is averaged over 2-min intervals, it is smooth up to geocentric distances of 6RE. With decreasing distances, the form of the particle spectra in the region under consideration remained virtually unchanged (region from L = 11RE down to L= 6RE) and only insignificant variations of the energy of the spectral maxima are observed. Possible reasons for the observed regularities are discussed.

The dawn‐dusk plasma sheet asymmetry of energetic particles: An Interball perspective

We systematically study the energetic particle (∼25 to 850 keV) dawn‐dusk plasma sheet asymmetry using both ion and electron spectra composed of 56 energy channels. These spectra, corresponding to an average duration of ∼8 hours, have been provided by the Interball tail probe and cover the extent between 15 and 28 RE away from the Earth. The events are classified in four Y coordinate categories: the “dawnside” with YGSM<−13 RE, the “center dawn” with 0>Y>−13 RE, the “center dusk” with 0<Y<13 RE, and the “duskside” with Y>13 RE. The asymmetry is profound between the two extreme dawn‐dusk flanks and weaker between the two central plasma sheet regions. In all the energy channels the dusk flank ion fluxes exceed those of electrons. At the dawnside the energetic electron fluxes frequently outnumber those of ions above a bottom energy threshold. During quite times (Kp<2) the ion (electron) fluxes in the duskside (dawnside) plasma sheet exceed by far those in the dawn (dusk) flank. In general, the ion and electron fluxes significantly increase as the Kp index steps upward. However, owing to the dawn‐dusk asymmetry, one can observe higher electron fluxes at dawn with low Kp than at dusk with high Kp. On the basis of two case studies, it is shown that ongoing substorm processes and plasma temperature transitions temporarily affect the spatial dawn‐dusk asymmetry and the associated spectra. In one case study, via successive spectra it was concluded that the betatron acceleration mechanism is probably the dominant energization process, although the observed spectra did not preserve their spectral shape. This is interpreted as due to the action of energy‐dependent large‐scale drifts across the tail that strongly modify the initial source spectra. The dawn‐dusk asymmetry and all the spectral characteristics from inside the plasma sheet are transmitted out into the magnetosheath, and this may help us (in the future) to discriminate between merging and leakage processes taking place over the magnetopause.

Different types of low‐latitude boundary layer as observed by Interball Tail probe

Interball Tail probe crossed dayside magnetopause during late winter to middle autumn months. The high‐latitude magnetopause was crossed outbound orbit, while the low‐latitude magnetopause was crossed inbound. We analyze 31 low‐latitude magnetopause/low‐latitude boundary layer (LLBL) crossings recorded in 1996 in the fast mode of SCA‐1 ion spectrometer. Data from the MIF/FM‐3 magnetometers and ELECTRON spectrometer are also used. The majority of magnetopause/LLBL crossings fall into two categories: (1) highly structured LLBL (14 cases) and (2) weakly structured LLBL (9 cases). The highly structured LLBL usually consists of short‐time (0.5–5 min) transients including fast‐moving (of an order of magnetosheath velocity) plasma as well as density transients that are nearly stationary relative to the magnetospheric plasma. The observed ensemble of transients shows evolution of plasma parameters from magnetosheath‐like to magnetosphere‐like. Fast‐moving transients frequently have flux transfer event (FTE) magnetic signatures. This type of LLBL is usually accompanied by various reconnection signatures and is more frequently observed when the interplanetary magnetic field (IMF) and/or magnetosheath magnetic field has a negative Bz component. The weakly structured LLBL shows a significantly smaller variation of number density and hotter plasma temperature. Strong velocity shear is frequently observed at the magnetopause in the weakly structured case. Dispersed ion signatures are often seen within this type of LLBL. The ion and electron temperatures within the weakly structured LLBL are more elevated in respect to the magnetosheath values compared to the highly structured LLBL. The weakly structured LLBL has a tendency to occur at positive IMF and/or magnetosheath magnetic field Bz. The cause of significant differences between the two kinds of LLBL lies, apparently, in the significantly larger distance of the plasma entry site from the observation point, for weakly structured LLBL, as opposed to highly structured LLBL. While the highly structured LLBL originates at low latitudes, the weakly structured LLBL is most probably formed at high latitudes.

Cusp energetic particles observed by INTERBALL-tail probe in 1996

The protons with energies of 1 – 3 MeV were observed in the dayside cusp by INTERBALL-Tail Probe. The flux increases lasting for several tens of minuttes were recorded up to the magnetopause. These energetic particle enhancements were accompanied by low-frequency wave turbulence.

Reconnection driven lobe convection: Interball tail probe observations and global simulations

We present Interball Tail Probe observations from the high latitude mid-tail magnetopause which provide evidence of reconnection between the interplanetary magnetic field (IMF) and lobe field lines during a 6 h interval of stable northward and dawnward IMF on October 19, 1995. Results from a global magnetohydrodynamic simulation for this interval compare well with the Interball observations. With the simulations, we provide an extended global view of this event which gives us insight into the reconnection and convection dynamics of the magnetosphere. We find that reconnection occurs in a region of limited spatial extent near the terminator and where the IMF and the lobe field are anti-parallel. Reconnected IMF field lines drape over the dayside magnetosphere, convect along the flanks into the nightside, and enter the magnetotail through a small entry window that is located in the flank opposite to the reconnection site. Ionospheric convection is consistent with previous observations under similar IMF conditions and exhibits a two cell pattern with a dominant lobe cell over the pole. The magnetic mapping between the ionosphere and the lobe boundary is characterized by two singularities: the narrow entry window in the tail maps to a 6 h wide section of the ionospheric lobe cell. A singular mapping line cuts the lobe cell open and maps to almost the entire tail magnetopause. By this singularity the magnetosphere avoids having a stagnation point, i.e., the lobe cell center maps to a tailward convecting field line. The existence of singularities in the magnetic mapping between the ionosphere and the tail has important implications for the study of tail–ionosphere coupling via empirical magnetic field models. Because the lobe–IMF reconnection cuts away old lobe flux and replaces it with flux tubes of magnetosheath origin, solar wind plasma enters the lobes in a process that is similar to the one that operates during southward IMF.

Determination of the Turbulent Diffusion Coefficient in the Plasma Sheet Using the Project INTERBALL Data

The results of an analysis of velocity fluctuations in the plasma sheet of the Earth's magnetotail measured onboard INTERBALL Tail Probe satellite are presented. The hodographs of the velocity in directions (Y, Z) and correlation functions are presented for a number of passages when the satellite was in the plasma sheet for a long time. The turbulent diffusion coefficients are calculated. A comparison of the obtained diffusion coefficients with those predicted theoretically in [1] is carried out. It is shown that the results of observations confirm theoretical predictions.

The role of nonlinear interaction in the formation of LF whistler turbulence upstream of a quasi‐perpendicular shock

The role of the nonlinear interaction in developed low‐frequency turbulence has been experimentally studied upstream of the ramp of a quasiperpendicular shock. The study has been carried out by application of the methods of bispectral analysis and wavelet decomposition to the Active Magnetospheric Particle Tracer Explorer Ion Release Module and Interball Tail Probe magnetic field data. It is shown that three‐wave processes play a key role in the formation of the spectrum of the turbulence. Experimental results presented and previous theoretical considerations lead to the conclusion that energy is transfered from a narrow maximum frequency pumped by nonlinear dynamic processes to lower and higher frequencies.

Low frequency plasma waves observed in the outer polar cusp

The polar cusp being a region of the free access of the solar wind into the inner magnetosphere is also the site of turbulent plasma flow. Satellites Interball Tail probe and Prognoz-8 with their orbits with apogee about 30R E and an inclination of 65° crossed the polar cusps many times. Magion-4 being the subsatellite for Interball-1 (Tail Probe) had the same orbit as the main satellite. In this presentation we discuss results of measurements the spectra of magnetic field fluctuations in the frequency range 30–2000Hz registered onboard Magion-4. During many crossings of the outer polar cusp the broad band emissions, lower hybrid and electron cyclotron harmonics were registered. The correlation of these emissions with plasma spectra is also presented.

Observation of isolated structures of the low latitude boundary layer with the INTERBALL/tail probe

We analyze the structure of magnetospheric transients observed at the dusk‐side low‐latitude magnetopause with the Interball Tail Probe. Ion and magnetic field measurements are used to investigate one particular transient in more detail. This transient has distinct non‐symmetric structure with the plasma characteristics and the flow properties of the leading part of the transient being quite different from those in the trailing part of the transient. The region separating these two parts corresponds to the change of the sign in the Bn component. These observations support an earlier conclusion that some plasma irregularities within the Low Latitude Boundary Layer (LLBL), formed as a result of sporadic reconnection, disconnect from the magnetopause, propagate and dissipate in the magnetosphere, and form what we call Disconnected Magnetosheath Transfer Events (DMTEs).

First results from the plasma composition spectrometer PROMICS-3 in the Interball project

Abstract. PROMICS-3 is a plasma experiment flown in the Russian project Interball. It performs three-dimensional (3D) measurements of ions in the energy range 4 eV–70 keV with mass separation and of electrons in the energy range 12 eV–35 keV. The Interball project consists of two main satellites, the Tail Probe and the Auroral Probe, each with one subsatellite. The Interball Tail Probe was launched on 3 August 1995, into a 65° inclination orbit with apogee at about 30 RE. Both main satellites carry identical PROMICS-3 instruments and thus direct comparisons of the particle distributions will be possible once the Auroral Probe is launched. Furthermore, PROMICS-3-Tail is the first instrument measuring the 3D ion distribution function in the magnetospheric boundary layers at high latitudes. In this paper we describe the PROMICS-3 instrument and show initial results from the Tail probe, measurements of the magnetosheath, plasma sheet, and ring current plasmas.

The INTERBALL-Tail ELECTRON experiment: initial results on the low-latitude boundary layer of the dawn magnetosphere

Abstract. The Toulouse electron spectrometer flown on the Russian project INTERBALL-Tail performs electron measurements from 10 to 26 000 eV over a 4<pi> solid angle in a satellite rotation period. The INTERBALL-Tail probe was launched on 3 August 1995 together with a subsatellite into a 65° inclination orbit with an apogee of about 30 RE. The INTERBALL mission also includes a polar spacecraft launched in August 1996 for correlated studies of the outer magnetosphere and of the auroral regions. We present new observations concerning the low-latitude boundary layers (LLBL) of the magnetosphere obtained near the dawn magnetic meridian. LLBL are encountered at the interface between two plasma regimes, the magnetosheath and the dayside extension of the plasma sheet. Unexpectedly, the radial extent of the region where LLBL electrons can be sporadically detected as plasma clouds can reach up to 5 RE inside the magnetopause. The LLBL core electrons have an average energy of the order of 100 eV and are systematically field-aligned and counterstreaming. As a trend, the temperature of the LLBL electrons increases with decreasing distance to Earth. Along the satellite orbit, the apparent time of occurrence of LLBL electrons can vary from about 5 to 20 min from one pass to another. An initial first comparison between electron- and magnetic-field measurements indicates that the LLBL clouds coincide with a strong increase in the magnetic field (by up to a factor of 2). The resulting strong magnetic field gradient can explain why the plasma-sheet electron flux in the keV range is strongly depressed in LLBL occurrence regions (up to a factor of \\sim10). We also show that LLBL electron encounters are related to field-aligned current structures and that wide LLBL correspond to northward interplanetary magnetic field. Evidence for LLBL/plasma-sheet electron leakage into the magnetosheath during southward IMF is also presented.

Initial observations of fine plasma structures at the flank magnetopause with the complex plasma analyzer SCA-1 onboard the Interball Tail Probe

Abstract. The fast plasma analyzer EU-1 of the SCA-1 complex plasma spectrometer is installed onboard the Interball Tail Probe (Interball-1). It provides fast three-dimensional measurements of the ion distribution function on the low-spin-rate Prognoz satellite (about 2min). The EU-1 ion spectrometer with virtual aperture consists of two detectors with 16 E/Q narrow-angle analyzers and electrostatic scanners. This configuration allows one to measure the ion distribution function in three dimensions (over 15 energy steps in 50 eV/Q–5.0 keV/Q energy range in 64 directions) in 7.5 s, which makes it independent of the slow rotation speed of the satellite. A description of the instrument and its capabilities is given. We present here the preliminary results of measurements of ions for two cases of the dawn low- and mid-latitude magnetopause crossings. The properties of observed ion structures and their tentative explanation are presented. The 12 September 1995 pass at low latitude at about 90° solar-zenith angle on the dawn side of the magnetosphere is considered in more detail. Dispersive ions are seen at the edge of the magnetopause and at the edges of subsequently observed plasma structures. Changes in ion velocity distribution in plasma structures observed after the first magnetopause crossing suggest that what resembles multiple magnetopause crossings may be plasma blobs penetrating the magnetosphere. Observed variations of plasma parameters near magnetopause structures suggest nonstationary reconnection as the most probable mechanism for observed structures.

Cusp and boundary layer observations by INTERBALL

Interball Tail Probe was launched on August 2, 1995 together with its subsatellite MAGION-4 into a highly elliptical orbit with apogee at 31 R E and inclination 63 degrees. During the course of one year all local times are visited. In this paper we will present initial results obtained from measurements in the cusp, mantle and eveningside plasma sheet in January, 1996. It is found that the cusp was well defined and persistent at altitudes of 4–10 R E. In one case both the main satellite and the subsatellite were in the cusp proper for two uninterrupted hours. We believe this to be the first ever multi-point satellite observation of the high-altitude cusp. The data indicate that the cusp was very stable with a wide entry area and that plasma entry took place at high latitudes rather than at the subsolar point. Pressure pulses, possibly due to Alfvén waves were found. Sunward and antisunward moving plasma was measured simultaneously during a case of northward IMF but no convection was discovered. Plenty of plasma of cusp/magnetosheath type was also found mixed with plasma sheet plasma both equatorward of the cusp and in the eveningside plasma sheet.