SM31B-1717
Cluster and Double Star Multipoint Observations of a Plasma Bubble
Depleted flux tubes, or plasma bubbles, are one possible explanation of bursty bulk flows, transient high speed flows thought to be responsible for a large proportion of flux transport in the magnetotail. Here we report observations of one such plasma bubble, made by the four Cluster spacecraft and Double Star TC-2 around 14:00 UT on 21 September 2005, a period of southward, but BY-dominated IMF. In particular the first direct observations of return flows around the edges of a plasma bubble, and the first observations plasma bubble features within 8 RE, consistent with MHD simulations (Birn et al., 2004) are presented. The implications of the presence of a strong BY in the IMF and magnetotail on the propagation of the plasma bubble and development of the associated current systems in the magnetotail and ionosphere are discussed.
SM31B-1718
Spatial Distribution of Dense Plasma in the Near-Earth Plasma Sheet and its Transport Into the Inner Magnetosphere
We investigate the cold-dense plasma sheet (CDPS) on November 12 and 13, 2007 by using THEMIS, Geotail, and LANL satellite. During the last extend period of northward IMF, 2-component CDPS in the duskside plasma sheet (PS), single component CDPS in the dawnside PS, and hot-dense ions (HDIs) at the inner edge of the PS on the dawnside were observed by Geotail, THC, and THA simultaneously. Then, super-dense plasma sheet (SDPS) was detected near the midnight region at geosynchronous orbit (GEO) (i) 1 hour after the southward turning of the IMF and (ii) at the rapid enhancement of the solar wind density (4 hours after (i)). Focusing on (i), duskward moving HDIs and earthward fast flow were encountered by Geotail in the pre-midnight PS. The appearance of SDPS and energetic electrons was in good association with this fast flow. We suggest that HDIs on the dawnside moved to the pre-midnight PS and they were pushed into GEO by the fast flow. After both observations of SDPS, the dense plasma was not seen on the dawnside where THA had detected HDIs (X < ~-5 Re), while it existed earthward of the region. Although these periods were front parts of corotating interaction region (CIR), geomagnetic activity was very weak. We discuss the transport mechanism and the geoeffectiveness of the dense plasma.
SM31B-1719
Properties of Cold Plasma Flow in the Magnetotail
Cold ionospheric ions (energy below a few tens of eV) in the tenuous magnetotail lobes are difficult to measure by particle detectors due to the high spacecraft potential (tens of volts). Consequently, few studies exist of plasma flows like the polar wind above a few thousand km altitude. By combining data from two different electric field instruments we can study the formation of a wake behind the Cluster satellites, to show the existence of cold plasma flows and to determine their flow velocity. Combining with plasma density from the spacecraft potential, we also get the ion flux. The database thus obtained vastly exceeds any previous study of cold magnetotail ions. We present maps of the cold ion density, velocity and flux in the tail lobes, showing that the cold plasma flows observed at a few thousands of km altitude continue at least as far as the Cluster apogee around 20 RE.
SM31B-1720
Kinetic Simulations of Magnetic Reconnection in the Geomagnetic tail with Oxygen, Using Physical Mass Ratios
Kinetic simulations of the magnetic reconnection in the geomagnetic tail have been completed including the presence of Oxygen and using physical mass ratio for electrons, protons and Oxygen ions. The possibility to achieve full kinetic treatment with the physical mass ratios for O+ and H+ is made possible by a new parallel implicit Particle-in-Cell (PARSEK). The approach is used to investigate the different time scales and low-frequency phenomena, associated to heavy ions in the geomagnetic tail. The role of Oxygen and real mass ratio for the different species is studied. Two types of processes are investigated in 2D: the drift instabilities in the current direction (LHDI) and reconnection. The effect of the presence of substantial populations of oxygen ions is considered for both type of processes. The combined effect of the two types of processes is then considered in fully 3D simulations demonstrating the effect of drift waves on the reconnection process.
SM31B-1721
Vlasov simulation of GEM magnetic reconnection challenge
A detailed procedure of full-electromagnetic Vlasov simulation technique is presented. Our new unsplitting conservative scheme exactly satisfies the continuity equation for charge. The implicit Finite Difference Time Domain method is also adopted for computation of electromagnetic fields, which is not restricted by the CFL condition for light. The Geospace Environment Modeling magnetic reconnection challenge problem is adopted as a benchmark test. The characteristics of the present Vlasov code are studied by varying the resolution in configuration space.
SM31B-1722
Is Magnetic Reconnection Different in the Magnetotail than at the Magnetopause?
Our recent full particle simulations have shown that the electron diffusion region elongates in time, giving rise to formation of secondary islands and time-dependent reconnection rate. Islands of many sizes are formed in the process. However, these simulations were performed for a limited set of parameters. The natural question is whether the obtained results are generic. Given that the conditions are very different at the Earth's magnetopause and in the magnetotail, we have started a study of the reconnection process accounting for differences in the tail and at the magnetopause. Some of the questions that we address in this presentation include: (i) Can slow shocks ever be formed?, (ii) Can flux pile up occur in the collisionless limit? (iii) Can reconnection shut off? (iv) How does the length of the electron layer scale with the upstream plasma conditions?
SM31B-1723
Simulation of Current Sheet Instabilities Using Gygokinetic Electron and Fully Kinetic Ion Particle Code
A novel gyrokinetic electron and fully kinetic ion (GKe/FKi) particle simulation model has been developed [Lin et al., PPCF, 2005] for the purpose of investigation of magnetic reconnection in collisionless plasmas. In this model, the rapid electron cyclotron motion is removed, while retaining the finite electron Larmor radii, wave-particle interaction, and off-diagonal components of the electron pressure tensor. This treatment results in a larger time step and allows one to treat the realistic ion-to-electron mass ratio mi/me in a large-scale system. The model is particularly suitable for ω < Ωe and k∥/ k⊥<1, and for problems in which the wave modes ranging from Alfven waves to lower-hybrid/whistler waves need to be handled on an equal footing. In this talk, we introduce the GKe/FKi model and present our simulation of instabilities of Harris sheet under a broad range of finite guide field BG and with a realistic mi/me using the linearized δ f GKe/FKi code [Wang et al., PoP, 2008]. The simulation is carried out in the 2-D plane containing the guide field in the y direction and the current sheet normal along z. For a finite BG/Bx0<1, where Bx0 is the asymptotic anti-parallel field component, quasi-electrostatic modified two-stream instability/whistler mode are found on the edge of current sheet. In addition, a new mode is found to be confined in the sheet center and carry a compressional δ By along the direction of electron drift, and may contribute directly to the electron anomalous resistivity in reconnection. For BG/Bx0≫1, the wave modes evolve to a globally propagating instability. The presence of finite BG is found to modify the physics of current sheet significantly.
SM31B-1724
Guide Field Reconnection: Energy Transfer and Global Constraints in PIC and MHD Simulations
Using PIC and resistive MHD simulations of the Newton challenge problem with a guide field, we investigate energy conversion in low and high beta current sheets. The energy transfer from reconnection mainly consists of a redirection of Poynting flux and a generation of enthalpy flux, involving compressional heating and Joule dissipation, whereas only a small amount of energy gets converted to bulk flow energy. Joule heating appears to play a relatively larger role in low-beta current sheets than for high beta. We also investigate the conservation of global quantities on moving and reconnected field lines, such as mass, entropy and the displacement of field line footpoints.
SM31B-1725
Dipolarization Front: A Distinctive Feature of the Reconnection Onset in the Magnetotail
Recent particle simulations with open boundaries revealed interesting new effects in collisionless magnetic reconnection, including its intermittent regimes with the formation of the secondary plasmoids in the outflow regions. In this presentation we show that, apart from rather conventional plasmoids forming near the electron diffusion region of the central X-line, there is another group of the secondary reconnection structures that strongly resemble the dipolarization fronts, reported in Geotail, Cluster, and Themis observations of bursty bulk flows and substorm activations in the terrestrial magnetotail. These structures are characterized by a strong and quick increase of the original tail field Bz, normal to the neutral plane, up a half of the lobe field, in contrast to a relatively small and shallow negative dip of Bz in the front precursor, comparable in amplitude to the field Bz prior to the dipolarization onset. Both electrons and ions are magnetized at the front of the dipolarization wave. In contrast, in its trail, ions are unmagnetized and move slower compared to the ExB drift, whereas the magnetized electrons either follow that drift or move even faster, forming super-Alfvenic jets. In spite of drastically different motions of electrons and ions, the formation and growth of the dipolarization front is not accompanied by the corresponding growth of the electrostatic field. This suggests that the electron compressibility effect, stabilizing the ion tearing mode in the tail-like systems with trapped magnetized electrons [Lembege and Pellat, 1982], is strongly attenuated in open systems.
SM31B-1726
Does Reconnection Onset Require Thin Current Sheets?
One mechanism for the onset of magnetic reconnection in a current sheet is accelerated growth of a tearing mode in the presence of a lower hybrid drift instability (LHDI). The LHDI causes current sheet thinning and anisotropic electron heating, both of which increase tearing mode growth far beyond normal nonlinear saturation levels. Implicit particle simulations in three dimensions yield noise initiated reconnection for thin current sheets with ρi/L ≈ 1.7-2.2, where ρi is the ion cyclotron radius and L is the current sheet thickness [1]. One asks, in more realistic current sheets with ρi/L ≤ 1 will there be spontaneous reconnection? The answer is interesting from two perspectives. Can the action of the LHDI explain onset in realistic current sheets? If so, why isn't reconnection always happening? Highly resolved explicit particle simulations of the LHDI in two dimensions with ρi/L =1, a more realistic value for the Earth's magnetotail, show smaller but still significant thinning and heating [2]. Recent implicit simulations in three dimensions show that reconnection onset is delayed in current sheets with ρi/L = 1, but that reconnection, once begun, proceeds rapidly. The delay is consistent with the expected decreased growth rates for both the LHDI and tearing modes. In simulations with even thicker current sheets, ρi/L ≤ 0.5, the time scales are longer and the signal to noise ratio less favorable. However, the results suggest either that onset does not occur at all or is long delayed, and possibly that reconnection onset occurs only in a sufficiently thin current sheet. 1. P. Ricci, J. U. Brackbill, W. Daughton, G. Lapenta, Phys. Plasmas 11, 4489 (2004). 2. W. Daughton, G. Lapenta, P. Ricci, Phys. Rev. Lett. 93(2004).
SM31B-1727
The Structure of the Electron Outflow Jet in Collisionless Magnetic Reconnection
Particle-in-cell simulations and analytic theory are applied to the study of the electron outflow jet in collisionless magnetic reconnection. In these jets, which have also been identified in spacecraft observations, electron flow speeds in thin layers exceed the ExB drift, suggesting that electrons are unmagnetized. In this study, we find the surprising result that the electron flow jets can be explained by a combination of ExB drifts and of diamagnetic effects, through the combination of the gradients of particle pressure and of the magnetic field. In a suitably rotated coordinate system, the electron motion is readily decomposed into ExB drift and the motion to support the required current density, consistent with electron gyrotropy. This process appears to be nondissipative.
SM31B-1728
THEMIS burst mode observations of reconnection and flux ropes in the magnetotail current sheet: Sites of energetic electron production
THEMIS burst mode observations of the onset of reconnection and flux rope (secondary island) formation in the magnetotail are presented and analyzed. The burst mode observations show in new detail the substructure of the reconnection generated secondary island, including large electric field fluctuations and density variations. The 3D structure of the thermal electron distributions are discussed in the context of guide field reconnection. We also examine the distribution of energetic electrons through this event; although a number of theories and observations have been presented exploring the role magnetic reconnection plays in producing energetic electrons, the relative importance of these different theories is still unclear. The data are used to explore the relative importance of the different models.
SM31B-1729
Electron Scale Structures in Collisionless Magnetic Reconnection
Recent advances in collisionless magnetic reconnection (like formation of the electron diffusion region (EDR) of scale size of electron skin depth de=c/ωpe embedded inside ion diffusion region of the scale size of ion skin depth di=c/ωpi, identification of EDR in laboratory plasma, satellite observations of electron scale structures in magnetopause (few tenth of de) and magnetotail (few de) etc.) emphasize the crucial role of electron scale physics. In this work, the electron scale processes during collisionless reconnection are simulated using the simplified electron-magnetohydrodynamic (EMHD) model, in which electron inertia provides the non-ideal effect in Ohm's law and breaks the frozen-in condition. The simulations are performed for the two cases when the simulations are initialized with (a) the longest wavelength perturbation leading to only one reconnection site in the system, and (b) with many modes leading to multiple reconnection sites in the system corresponding to the maximally growing mode. Key differences in the structures and their scale lengths in the two cases arise due to the important roles of electron flows. In case of one reconnection site, highly directed electron out flow jets lead to the bifurcation of the out of plane electron current and the length of the central reconnecting current sheet depend on the wavelength of the mode which initiated the reconnection. In the case of multiple reconnection sites, interaction of outflow jets from the neighboring reconnection sites leads to secondary instabilities which split these jets. The outflow region develops turbulence and electron vortices as a consequence of the electron Kelvin-Helmholtz instability which grows on the shear flow pattern formed by the split jets. This limits the length of the current sheet and defines the scale sizes observable by spacecraft in the Earth's magnetotail. The development of electron vortices lead to modification in the basic quadrupole structure of the out of plane magnetic field. These results has implications for the upcoming NASA's MMS mission which is designed to resolve the short scale structures ~ de. Three-dimensional studies are in progress and will be compared with these results.
SM31B-1730
Fast magnetic reconnection driven by intermittent resistive tearing modes
Magnetic reconnection is a key process of various bursty phenomena in space plasmas. In general, a magnetic Reynolds number of the space plasma is extremely high. Therefore, since magnetic reconnection rate becomes low as magnetic Reynolds number increases within the framework of the stationary resistive MHD model, kinetic effects have been considered to realize realistic fast magnetic reconnection in modern reconnection models. However, it is thought that the MHD description is valid within a very wide scale range since a scale gap between macro and micro is so large, e.g., in the solar corona, the ratio of macro to micro will be more than 107. In this situation, how an ion-scale thin current sheet can be realized from a macro scale magnetic structure? Conversely, how the microscopic processes can affect macroscopic MHD dynamics? From the analogy of hydrodynamics, we expect that the strong MHD turbulence will be developed in the wide range. Thus, in this case, fast magnetic reconnection might be driven by the turbulence other than the kinetic effects. In this study, a very high-resolution resistive MHD simulation is performed to clarify multi-scale dynamics of the resistive tearing instability at high magnetic Reynolds number. Results show that small scale plasmoids, which seem to have an internal structure by itself, are intermittently created and ejected by the secondary tearing instability. Moreover, it seems that fast magnetic reconnection is achieved by intermittent dynamics of the plasmoids. This might support that the MHD turbulence is essential for fast magnetic reconnection at very high magnetic Reynolds number.
SM31B-1731
Plasma entry into the tail at northward IMF
Plasma entry into northern tail lobe about 1.5 hours after onset of steady strong northward IMF was observed. Both tailward and Earthward flows are seen. Earthward flow is mainly observed closer to magnetopause while tailward flow dominates at larger distances from magnetopause. Ion velocity distribution is D-shaped indicating reconnection origin of the flows. Counterstreaming ion components are often observed suggesting closed magnetic flux tubes. We argue that these closed magnetic tubes formed as a result of reconnection both at northern and southern tail lobes and subsequently convected into the tail.
SM31B-1732
Particle-in-Cell Simulation of Collisionless Reconnection with Open Outflow Boundaries
A new method for applying open boundary conditions in particle-in-cell (PIC) simulations has been utilized to study magnetic reconnection. For this method, particle distributions are assumed to have zero normal derivatives at the boundaries. Advantages and possible limitations of this method for PIC simulations will be discussed. Results from a reconnection simulation study will be presented. A 2 ½-dimensional electromagnetic PIC simulation using open conditions at the outflow boundaries and simple reflecting boundaries to the inflow regions will be discussed. We define the electron diffusion region as that region where the out-of-plane electron inertial electric field is positive indicating acceleration and flux transfer; the evolution of this region has been analyzed. We have found that this region varies in the range 2.5-4 local electron inertial lengths in total width and in the range 10-15 local electron inertial lengths in total length for the mass ratio 25. The reconnection rate has been investigated in terms of the aspect ratio of this electron diffusion region plus inflow and outflow measures at its boundaries. We will show that a properly measured aspect ratio predicts the flux transfer rate, scaled to account for the decline in field strength and electron density at the inflow boundaries to the electron diffusion region. We conclude that this electron diffusion region either adjusts its aspect ratio for compatibility with the flux transfer rate that is set elsewhere, as in the Hall reconnection model, or that it is this region that controls the reconnection flux transfer rate.
SM31B-1733
Kinetic properties of the electron current sheet and its neighbor magnetic islands
Kinetic physics of magnetic reconnection is key to the impulsive energy release of a current sheet in collisionless plasmas. We have developed a methodology combining multi-spacecraft data and PIC simulations to delineate inflow and exhaust regions within the reconnection layer, and reconstruct the time history and topology of reconnection. The methodology has been applied to a few magnetotail reconnection events, and enabled the following discoveries. One, bursts of energetic electrons are found in the interior of magnetic islands [Chen et al., Nature Physics, 4, 19-23, 2008]. Two, two reconnection layers, including a spatially extended electron current sheet (ecs), are separated by a non-stationary magnetic island with dimensions of a few ion inertial lengths (di). Three, the electron density decreases toward the ecs by a factor of 3-4 within one di, peaks at the ecs center, and increases by about an order of magnitude from the ecs toward the center of the neighbor magnetic island. Four, whistler waves and flat-topped electron distributions are observed simultaneously with energetic electrons at density compression sites within the di-scale island between two reconnection layers. Five, across the ecs, nonlinear Langmuir waves are abundant, but no electrostatic solitary waves are observed. Six, oxygen ions exhibit single beams in the inflow region, counter-streaming beams at the island boundary near the ecs, and triple beams in island interior near the ecs. In this paper, we present our methodology and new findings, and discuss the impact of these findings on our understanding of collisionless magnetic reconnection.
SM31B-1734
The Weibel instability during pair reconnection
Recent full-particle simulations of pair reconnection reveal that the Weibel instability plays an active role in controlling the current layer dynamics. The anisotropy arises as inflowing plasma mixes with outflow from the x-line. A 4-beam model is proposed to capture the Weibel instability inside a narrow current layer. Due to the mass and charge symmetry between electrons and positrons, we are able to obtain two coupled 2nd order differential equations, whose growing eigenmodes are obtained via either asymptotic approximation or finite difference method. Full particle simulations are conducted to confirm our linear theory, and further explore the nonlinear behavior of the Weibel instability inside a narrow Harris sheet. The scale size of the observed structures in the outflow jet in simulations of pair reconnection is linked to the gyro-radii of high-velocity streaming particles in the Weibel-generated, out-of-plane magnetic field. The associated momentum transport helps open the reconnection nozzle downstream from the x-line.
SM31B-1735
Perpendicular Localization of Electron Holes by Spatially Inhomogeneous Flows During Magnetic Reconnection*
Bipolar fields signaling the presence of electron phase space holes have been observed in situ by
satellites near regions of magnetic reconnection in Earth's magnetopause and magnetotail. In order to
identify possible origins for such holes, a recent numerical study [1] employed 1D and 2D electrostatic Vlasov
simulations initialized with electron and ion distributions taken from 2D electromagnetic Particle in Cell (PIC)
simulations of magnetic reconnection. Both electron-electron instabilities along the X-line and electron-ion
(i.e., Buneman) instabilities along the separatrix were found to be viable sources of electron holes. However,
long-lived coherent Buneman-driven holes only formed when the destabilizing current was restricted to a
narrow channel perpendicular to the local magnetic field vector B. In this presentation we extend the 2D
Vlasov study of electron holes driven by unstable distributions to include both e-e and e-i instabilities
localized in the direction perpendicular to B. Emphasis will be placed on how the ion/electron
mass and temperature ratios (mi/me and Ti/Te) and the magnetization ratios
(Ωe/ωe and Ωi/ωi) influence the properties of the resulting electron holes,
including their spatial size and aspect ratio. Distributions from recent implicit PIC reconnection simulations [2]
will be used to guide the initialization of the Vlasov simulations.
*Research supported by NASA, NSF, and DOE.
[1] M. V. Goldman, D. L. Newman, and P. L. Pritchett, "Vlasov
Simulations of Electron Holes Driven by Particle Distributions
from PIC Reconnection Simulations with a Guide Field,"
submitted to Geophys.~Res.~Lett. (2008).
[2] A. Divin, G. Lapenta, D. L. Newman and M. V. Goldman,
"Implicit PIC Simulations of Guide Field Magnetic
Reconnection," this meeting.
SM31B-1736
Implicit PIC Simulations of Magnetic Guide-Field Reconnection*
Implicit PIC simulations of magnetic reconnection starting from a Harris equilibrium with a guide field |Bg| =
|B0| have been carried out using the "PARSEK" implicit Particle in Cell (PIC) code. Conditions in 2D are
similar to those of explicit PIC simulations by Pritchett [1], with the following differences: An initial flux
perturbation is added to hasten island formation and a variety of mass ratios, Mi/me=64 and upward are
introduced and with results compared. Secondary island formation is found, as well as high parallel electron
velocities at magnetic island separatrices and in the electron diffusion region. Particle distributions are
analyzed in these regions with e-i (Buneman) and e-e instabilities found, respectively, in these two regions.
Vlasov simulations are used to follow the nonlinear evolution of these instabilities, including the formation of
electron phase space holes (bipolar fields) with different speeds and half-widths (Goldman, et al., [2]).
* Research supported by NASA
[1] P. L. Pritchett, Phys. Plasmas, 12, 062301, (2005).
[2] M.V. Goldman, D.L. Newman and P. L. Pritchett, "Vlasov Simulations of Electron Holes driven by
Particle Distributions from PIC Reconnection Simulations with a Guide Field," submitted to
Geophys.~Res.~Lett.(2008).
SM31B-1737
Kinetic Alfven wave turbulence and transport through a reconnection diffusion region
We demonstrate from observations that kinetic Alfven waves may play an important role in facilitating magnetic reconnection. These waves radiate outwards from the diffusion region oblique to the magnetic field in a cone-like pattern delimited by the X-line separatrices with outward energy fluxes equivalent to that contained in the outstreaming ions. It is shown that the wave-vectors reverse across the X and symmetry lines and have a large out of plane component. From a consideration of the local diffusion and non-local impedance these waves provide, we suggest that they may allow diffusion of the magnetic field through the plasma at the rate observed
SM31B-1738
O+ distributions near the reconnection X-line in the Earth's Magnetotail. CLUSTER observations.
The CLUSTER mission has provided a considerable number of in-situ observations of the formation of an X- line in the mid-tail region of the Earth's magnetotail shedding light on the physical processes underlying time- dependent collisionless reconnection during quiet as well as storm conditions. From these observations it has become evident that there are time periods where heavy ions (mainly O+ of ionospheric origin), in the vicinity of thin current sheets, can be the dominant contributor to the plasma pressure. A first step in understanding the role of these O+ ions in the reconnection process requires the identification of O+ distributions in the different regions (e.g. inflow, outflow, separatrix) of the ion and electron diffusion regions. Here we present a database of the observed O+ distributions from ~40 encounters of the CLUSTER spacecraft within the vicinity of an X-line in the near Earth magnetotail. The types of the observed distributions are classified as a function of the O+ content of the plasma sheet (i.e. of geomagnetic activity), the current sheet thickness and the region of ion diffusion region. The CLUSTER spacecraft separation differed over the years, covering distances from ~2000 km to ~500 km. These different separations will provide a great opportunity to estimate the scale lengths over which the various distributions appear. Creation of such a database will assist with future comparisons with simulations.
SM31B-1739
Particle energization during magnetic reconnection in coupled kinetic-global model of the magnetotail
The energization of particles during magnetic reconnection is usually studied using kinetic model of the thin current sheet and such studies ignore the effects of the global processes affecting the diffusion region. In a new coupled kinetic-global model the self-consistent kinetic models of thin current sheets are combined with a global magnetic field (Tsyganenko et al., 2002) to obtain a magnetospheric field suitable for the study of particle distributions for different conditions. The kinetic current sheets are obtained from the kinetic Grad- Shafranov equation, which yields three types of equilibria: field-reversed (Harris) sheet, magnetotail (finite Bn) and current sheets with embedded magnetic islands. These equilibria are then embedded into the global magnetic field model to obtain an integrated magnetic field in which the kinetic nature of the thin current sheet and the overall global (MHD) features are seamlessly coupled. The particle distributions in these cases are then studied using particle-in-cell techniques. While these simulations may not yield the self- consistent evolution, they yield a very good sampling of the particle distributions under the specified conditions of the magnetotail. In simulations using initial distributions that are Gaussian the electron energization is found to be most effective in current sheets with an embedded magnetic island. Although these simulations do not directly yield the evolution of the particle distribution function during the different stages of reconnection, they represent the energization process well, within the framework of studies using neighboring equilibria. For realistic values of the mass ratios the ion energization is weak but the scaling for different mass ratios can be obtained. The integrated kinetic-global equilibria will be used for the study of instabilities responsible for reconnection onset.