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Papers by daniel berdichevsky

IntechOpen eBooks, Sep 21, 2023

Bulletin of the American Physical Society, Apr 5, 2014

Submitted for the APR14 Meeting of The American Physical Society On the Thermodynamics and other ... more Submitted for the APR14 Meeting of The American Physical Society On the Thermodynamics and other Constitutive Properties of a Class of Strongly Magnetized Matter Observed In Astrophysics DANIEL BERDICHEVSKY, NASA/GSFC-It is shown that the occurrence of magnetic field work is a consistent thermodynamic explanation of the property of anticorrelation between temperature and density of the electrons gas in a class of magnetic field dominated structures observed in the interplanetary medium. In this model, a 7 to 4 scaling ratio for magnetic-work to electron-gas-work explains the observed anomalous polytropic exponent γ = 1/2. 1 This interpretation is built on the theoretical conjecture of a matter-state having spatial-confinement of most hadronic-elements of matter, i.e., matter held in place by the action of what is here denominated "super-strong" magnetic field, which together with the plasma it contains satisfies ideal magnetohydrodynamics. 2 We further show that, within the resolution and sensitivity of the instrumentation used, that the assumptions made in this model are consistent with the coherence observed in changes of magnetic field and electron distribution moments for a case study, the flux-rope (FR) structure passing Earth on June 2, 1998. Here, the intervals of coherence extend in a range of 12 to 30 s for plasma data with a resolution of 3s. Further, the diamagnetic nature of this superconductive state of matter is confirmed for a case study, and an estimate of its permeability and permittivity consistent with space plasma observations made.

Aeronautics and aerospace open access journal, Mar 7, 2023

With no criticism to special relativity theory it is demonstrated with the help of a lattice with... more With no criticism to special relativity theory it is demonstrated with the help of a lattice with certain features, that it is feasible to reintroduce the 'aether' as a Lorentz invariant media. Such features lie on strings made of fibers at rest in a preferred reference system and analyzes its role as a transmission medium for the propagation both a fermion and a boson. For the approach it is used a sub algebra of Poincare that recovers the Lorentz transformation. Such sub algebra leads to a special type of graphs in which we place at ultra microscopic scale a fermion over one Euclidian space-speed graph coordinates instead of the Minkowski space-time. Finally we locate macroscopic objects and light rays in this graph and show that everything is always in a particular place at a corresponding time and discuss the anisotropy of space and the reversion of the time arrow.

AIP Conference Proceedings, 1999

ABSTRACT

Advances in Space Research, 2001

We examine a 3-hour long interval on December 24, 1996, containing a magnetic hole associated wit... more We examine a 3-hour long interval on December 24, 1996, containing a magnetic hole associated with an interplanetary magnetic cloud. Two sets of perturbations are observed by the Wind spacecraft at 1 AU. In the first, the field and flow rotate at constant field strength, and the plasma is accelerated to the local Alfven speed. We show this to be a rotational discontinuity. In the second, observed 25 min later, the plasma is heated and the field decreases. We show this to be a slow shock. The whole structure is in pressure balance. We interpret the observations as MHD discontinuities arriving with varying delays from a reconnection site closer to the Sun. Energetic particle observations suggest further that ejecta material is present for many hours prior to the magnetic cloud observation and separated from it by the layer. This suggests that reconnection took place between field lines of a CME of which the magnetic cloud formed a part.

We revisit the transient events of January and September 1978. In the January event the ejecta (a... more We revisit the transient events of January and September 1978. In the January event the ejecta (an interplanetary magnetic cloud, IMC) was studied using multiple spacecraft observations [Burlaga et al., 1981]. In the September event Reames et al., 1997 studied the spectral characteristics of the energetic particles of this big particle event with a driven shock passage observed at longitudes nearly 180° apart. Here we present a combined analysis of the overall solar wind and energetic particles (EP) features of the shock and the driver, observed at different locations in longitude. We further evaluate the Rankine-Hugoniot properties of the shock at the locations its passage is observed and add modeling of the driven shock using a three dimensional MHD code which, at this stage of the analysis, does not include the magnetic structure of the ejecta. For the study of the shock velocity we use remote type II radio burst observations from near Earth (the September event), and at different longitude locations we examine: (a) flux intensity of the energetic particles, (b) shock strength, (c) timing of the shock structure and the driver passage at each spacecraft to infer the possible location of the nose of the shock. A preliminary assessment on the connection between the global nature of the shock and the observed level of energetic particle flux will be presented. The data sets include the kilometric radio measurements on ISEE3, and the 3 to 80 MeV energetic proton flux data from IMP-8, and a similar energy range from Helios at wide longitudinal locations relative to Earth. For the solar wind parameters we use magnetic field and plasma parameters from instruments at Helios 1, and 2, and ISEE3 and IMP-8. The data set is completed with the Dst index (Kyoto). We acknowledge partial support from NSF and NASA grants, and the NSSDC for on-line access to their space science data archives. Burlaga LF, E. Sittler, F. Mariani, and R. Schwenn, Magnetic loop behind an interplanetary shock: Voyager, Helios, and IMP-8 observations, J. Geophys. Res., 86, 6673, 1981. Reames, DV, SW Kahler,, and CK Ng, Spatial and temporal invariance in the spectra of gradual particles in gradual solar events, Astrophys. J., 491, 414, 1997.

Vol. 55, Issue 3 (Heliophysics 2024 Decadal Whitepapers)

Journal of Geophysical Research, 2007

Journal of Geophysical Research, 2005

(''Halloween 2003'') epoch of intense solar flares provided an opportunity to test the results of... more (''Halloween 2003'') epoch of intense solar flares provided an opportunity to test the results of earlier parametric 1.5 MHD studies of interacting interplanetary shock waves. These preliminary studies used an adaptive numerical grid that made it possible to identify products of these interactions. During 28 October to 2 November 2003, three shocks generated by four solar flares were observed at the L1 libration point by ACE/SWEPAM/SWICS/MAG. Two very distinct geomagnetic storms, associated with two of these flares (X17/4B and X10/2B), rank as two of the largest storms of solar cycle 23. The purpose of this paper is to present the use of an adaptive grid 1.5-dimensional MHD model that is initiated at the solar surface to study in detail the three shocks observed at L1 that were generated by the four solar flares. Accordingly, four separate pressure pulses, at the appropriate times and with different strengths and duration, determined via a trial and error procedure, are introduced on the Sun to mimic the four flares. The results show that the simulated solar wind velocity temporal profiles successfully matched the observations at L1. The major objective, to demonstrate the detailed nature of interacting shocks and some of their products after origination from closely spaced solar events, is achieved. In addition, the MHD model is able to suggest the solar sources that are associated with specific geomagnetic storms at Earth.

Journal of Geophysical Research, 2003

We discuss the existence of large, complex merged interaction regions (MIRs) in the solar wind ne... more We discuss the existence of large, complex merged interaction regions (MIRs) in the solar wind near Earth. MIRs can have configurations that cause more prolonged geomagnetic effects than a single flow structure. A MIR or successive MIRs can produce relatively long lasting Forbush decreases at 1 AU. We illustrate MIRs at 1 AU with two examples (MIR-1 and MIR-2) seen by WIND and ACE in the interval from 18 March through 29 March 2002. We determined the probable structure and origin of each in terms of interacting flows and shocks using in situ and solar observations, but we emphasize that there are uncertainties that cannot be resolved with these data alone. The MIRs were relatively large structures with radial extent %2/3 and 3/4 AU, respectively. MIR-1 was formed by interactions related to at least two complex ejecta, a magnetic cloud, and two shocks. MIR-2 was related to a corotating stream, the heliospheric plasma sheet (HPS), two complex ejecta, a magnetic cloud and at least two shocks. A MIR can evolve significantly while it moves to 1 AU, and memory of the conditions near the Sun is lost in the process. Thus one cannot unambiguously determine the structure of a MIR and the manner in which it formed using observations from a single spacecraft at 1 AU. The magnetic field strength profiles in MIRs are not correlated with the speed and density profiles so that one cannot infer the magnetic field strength in MIRs from remote sensing observation that give density and speed information. It will be possible to better understand the dynamical processes leading to the formation of MIRs with remote sensing observations, but they cannot measure the magnetic fields in MIRs.

Journal of Geophysical Research, 1999

Several events have been identified of an ion foreshock extending up to 250 RE upstream of the Ea... more Several events have been identified of an ion foreshock extending up to 250 RE upstream of the Earth. These events occur mostly during periods of slowly drifting radial interplanetary magnetic field (IMF) when the 1-min average values of the strengths of the IMF and the solar wind (SW) speeds are mostly steady. For their analysis an analytical solution to the problem of the closest approach of an IMF line to two spacecraft is given. We used this method to find intervals of magnetic conjunction between the bow shock and the upstream regions at GEOTAIL and Wind. This solution is obtained by determining the minimum angle 0 (as a function of time) between the mean direction of the IMF (measured at Wind) and the vectordifference (rwI-r) of the locations of Wind and the point (attached on the field line) which went earlier by GEOTAIL. Here we take into account the mean drift of the flux lines with the SW, by assuming that the spacecraft were located in the same heliospheric magnetic domain. We have tested this method against a set of selected cases which show a steady presence of the ion foreshock close to the bow shock (GEOTAIL) and its sporadic presence far upstream (Wind). We have found our method to be accurate within a few Earth radii (RE). We have identified an outstanding candidate for the bow shock, GEOTAIL, and Wind sequential magnetic conjunction, which occurred on June 11, 1995. Additionally, this diagnostic technique has been applied to nine more intervals of simultaneous occurrences of intensity enhancements of broadband ultralow-frequency (ULF) waves, and fluctuating fluxes of scattered energetic ions (40-140 keV). Very broad ion foreshock regions (> 40 RE) are commonly observed during the subset of events characterized by a high-speed SW. The observed frequencies of the ULF waves are basically enhanced transversal modes in the range from-1/10 to 2/3 of proton cyclotron frequency, f. Fluctuations in the energetic ion fluxes were also observed in this frequency range for all the cp cases. Therefore we argue that the nature of the coupling between ULF waves and energetic ions is similar both in the near as well as far upstream regions of the Earth's bow shock.

Journal of Geophysical Research, 2000

A list of the interplanetary shocks observed by Wind from its launch (in Nov 1994) to May 1997 is... more A list of the interplanetary shocks observed by Wind from its launch (in Nov 1994) to May 1997 is presented. The magnetohydrodynamic nature of the shocks is investigated, and the associated shock parameters and their uncertainties are accurately computed using two techniques. ...

Journal of Geophysical Research, 2001

Correction to: "Interplanetary fast shocks and associated drivers observed through the 23rd solar... more Correction to: "Interplanetary fast shocks and associated drivers observed through the 23rd solar minimum by Wind over its first 2.5 years" by D. B. Berdichevsky et al. In the paper "Interplanetary fast shocks and associated drivers observed through the 23rd solar minimum by Wind over its first 2.5 years" by Daniel B.

Journal of Atmospheric and Solar-Terrestrial Physics, 2001

Signiÿcant charged-particle precipitation occurs in the dayside auroral zone during and after int... more Signiÿcant charged-particle precipitation occurs in the dayside auroral zone during and after interplanetary shock impingements on the Earth's magnetosphere. The precipitation intensities and spatial and temporal evolution are discussed. Although the post-shock energy ux (10-20 erg cm −2 s −1) is lower than that of substorms, the total energy deposition rate may be considerably greater (∼ an order of magnitude) than nightside energy rates due to the greater area of the dayside portion of the auroral oval (deÿned as extending from 03 MLT through noon to 21 MLT). This dayside precipitation represents direct solar wind energy input into the magnetosphere=ionosphere system. The exact mechanisms for particle energization and precipitation into the ionosphere are not known at this time. Di erent mechanisms are probably occurring during di erent portions of the storm initial phase. Immediately after shock compression of the magnetosphere, possible precipitation-related mechanisms are: (1) betatron compression of preexisting outer zone magnetospheric particles. The anisotropic plasma is unstable to loss-cone instabilities, leading to plasma wave growth, resonant particle pitch-angle scattering and electron and proton losses into the upper ionosphere. (2) The compression of the magnetosphere can also lead to enhanced ÿeld-aligned currents and the formation of dayside double-layers. Finally (3) in the latter stages of the storm initial phase, there is evidence for a long-lasting viscous-like interaction occurring on the anks of the magnetopause. Ground-based observations identifying the types of dayside auroral forms would be extremely useful in identifying the speciÿc solar wind energy transfer mechanisms.

Journal of Atmospheric and Solar-Terrestrial Physics, 2011

We report a comprehensive analysis of in situ observations made by Wind and the STEREO probes (ST... more We report a comprehensive analysis of in situ observations made by Wind and the STEREO probes (STA, STB) of a complex interaction between a magnetic cloud (MC) and a corotating interaction region (CIR) occurring near the heliospheric current sheet (HCS) on November 19-21, 2007. The probes were separated by 0.7 AU ð $ 40 3 Þ with a spread in heliographic latitudes (4.8,1 2.2,1 and À 0.4,1 for STB, Wind and STA, respectively). We employ data from the MFI, SWE and 3DP instruments on Wind, and the PLASTIC and IMPACT suites on STEREO. STB, located east of Earth, observed a forward shock followed by signatures of a MC. The MC took the role of the HCS in that the polarity of the interplanetary magnetic field (IMF) on exit was the reverse of that on entry. A passage through a plasma sheet was observed. Along the Sun-Earth line Wind observed a stream interface (SI) between a forward and a reverse shock. A MC, compressed by the CIR, was entrained in this. STA, located 201 to the west of Earth, saw a MC which was not preceded by a shock. A SI trailed the transient. The shocks are examined using various methods and from this it is concluded that the forward shock at Wind-but not at STB-was driven by the MC. Examining the MC by Grad-Shafranov reconstruction, we find evidence of a double-flux rope structure at Wind and STA and possibly also at STB. The orientations are at variance with the notion of a large-scale flux tube being observed at the three spacecraft. We find consistency of this with the directional properties of the solar wind ''strahl'' electrons. We examine aspects of the geomagnetic response and find a double-dip storm corresponding to the two interplanetary triggers. The minimum Dst phase was prolonged and the geoeffects were intensified due to the interaction. We conclude that while the formation of compound streams is a common feature of interplanetary space, understanding their components when CIRs are involved is a complicated matter needing numerical simulations and/ or more in situ observations for its complete elucidation.

IEEE Transactions on Plasma Science, 2004

... A6, p. 1262, 2003. [21] CJ Eyles, GM Simnett, MP Cooke, BV Jackson, A. Buffington, P. P. Hick... more ... A6, p. 1262, 2003. [21] CJ Eyles, GM Simnett, MP Cooke, BV Jackson, A. Buffington, P. P. Hick, NR Waltham, JM King, PA Anderson, and PE Holladay, “The solar mass ejection imager (SMEI),” Solar Phys., vol. ... 20, 2003. Craig D. Fry was born in San Francisco, CA, in 1949. ...