MAGNETIC FIELD STRENGTH FLUCTUATIONS AND THE<i>q</i>-TRIPLET IN THE HELIOSHEATH:<i>VOYAGER 2</i>OBSERVATIONS FROM 91.0 TO 94.2 AU AT LATITUDE 30° S

Burlaga, L. F.; Ness, N. F.

doi:10.1088/0004-637x/765/1/35

Cited by 27 publications

(20 citation statements)

References 42 publications

(61 reference statements)

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“…Therefore, if the LISM flow speed is 25 km s −1 , then it is weakly super-Alfvénic, suggesting that a magnetosonic bow shock might exist, at least over a small region in front of the heliosphere. However, the existence of a stronger magnetic field (∼4.6 μG; Burlaga & Ness 2013) in the LISM would yield an even larger Alfvén speed, v A ∼ 35 km s −1 , which could preclude a fast magnetosonic shock ahead of the heliosphere. Additionally, Scherer & Fichtner (2014) include LISM He + , which reduces the Alfvén and fast magnetosonic speeds, and Zank et al (2013) demonstrate the importance of ENAs in mediating the bow shock or bow wave.…”

Section: Discussionmentioning

confidence: 99%

DETERMINATION OF INTERSTELLAR He PARAMETERS USING FIVE YEARS OF DATA FROM THE IBEX : BEYOND CLOSED FORM APPROXIMATIONS

Schwadron

Möbius

Leonard

et al. 2015

ApJS

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Interstellar He represents a key sample of interstellar matter that, due to its high first ionization potential, survives the journey from beyond our solar system's heliospheric boundaries to Earth. Ongoing analysis of interstellar neutral (ISN) He atoms by the Interstellar Boundary Explorer (IBEX) has resulted in a growing sophistication in our understanding of the local interstellar flow. A key feature of the IBEX observations near perihelion of the ISN trajectories is a narrow "tube" of approximately degenerate interstellar parameters. These degenerate solutions provide a tightly coupled relationship between the interstellar flow longitude and latitude, speed, and temperature. However, the IBEX analysis resulting in a specific solution for the inflow longitude, inflow speed, temperature, and inflow latitude was accompanied by a sizeable uncertainty along the parameter tube. Here, we use the three-step method to find the interstellar parameters: (1) the ISN He peak rate in ecliptic longitude uniquely determines a relation (as part of the tube in parameter space) between the longitude ISN l ¥ and the speed V ISN¥ of the He ISN flow at infinity; (2) the ISN He peak latitude (on the great circle swept out in each spin) is compared to simulations to derive unique values for ISN l ¥ and V ISN¥ along the parameter tube; and (3) the angular width of the He flow distributions as a function of latitude is used to derive the interstellar He temperature. For simulated peak latitudes, we use a relatively new analytical tool that traces He atoms from beyond the termination shock into the position of IBEX and incorporates the detailed response function of IBEX-Lo. By varying the interstellar parameters along the IBEX parameter tube, we find the specific parameters that minimize the chi-square difference between observations and simulations. The new computational tool for simulating neutral atoms through the integrated IBEX-Lo response function makes no assumptions or expansions with respect to the spin-axis pointing or frame of reference. Thus, we are able to move beyond closed-form approximations and utilize observations of interstellar He during the complete five year period from 2009 to 2013 when the primary component of interstellar He is most prominent. Chi-square minimization of simulations compared to observations results in a He ISN flow longitude of 75 6 ± 1 4, latitude of −5 12 ± 0 27, speed of 25.4 ± 1.1 km s −1 , and temperature of 8000 ± 1300 K, where the uncertainties are related and apply along the IBEX parameter tube. This paper also provides documentation for a new release of ISN data and associated model runs.

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Section: Discussionmentioning

confidence: 99%

DETERMINATION OF INTERSTELLAR He PARAMETERS USING FIVE YEARS OF DATA FROM THE IBEX : BEYOND CLOSED FORM APPROXIMATIONS

Schwadron

Möbius

Leonard

et al. 2015

ApJS

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“…Theoretical and experimental illustrations in natural systems include long-range-interacting many-body classical Hamiltonian systems [13][14][15][16][17][18][19][20] (see also [21,22] [47,48], chemistry [49], earthquakes [50], biology [51,52], solar wind [53,54], anomalous diffusion in relation to central limit theorems and overdamped systems [55][56][57][58][59][60][61][62][63][64], quantum entangled systems [65,66], quantum chaos [67], astronomical systems [68,69], thermal conductance [70], mathematical structures [71][72][73][74][75][76] and nonlinear quantum mechanics [77][78][79][80][81][82][83][84]…”

Section: Introductionmentioning

confidence: 99%

Economics and Finance: q-Statistical Stylized Features Galore

Tsallis

2017

Entropy

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Abstract:The Boltzmann-Gibbs (BG) entropy and its associated statistical mechanics were generalized, three decades ago, on the basis of the nonadditive entropy S q (q ∈ R), which recovers the BG entropy in the q → 1 limit. The optimization of S q under appropriate simple constraints straightforwardly yields the so-called q-exponential and q-Gaussian distributions, respectively generalizing the exponential and Gaussian ones, recovered for q = 1. These generalized functions ubiquitously emerge in complex systems, especially as economic and financial stylized features. These include price returns and volumes distributions, inter-occurrence times, characterization of wealth distributions and associated inequalities, among others. Here, we briefly review the basic concepts of this q-statistical generalization and focus on its rapidly growing applications in economics and finance.

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“…For all q = 1, one has that Φ( x, t) is distinct from Ψ * ( x, t), with the fields Φ( x, t) and Ψ( x, t) being related by Equation (44). Now, if one substitutes the q-plane wave solution of Equation (6) in Equation (44), one finds,…”

Section: Continuity Equation and Classical Field Theorymentioning

confidence: 99%

“…The extension of these results to the d-dimensional case is straightforward. We remind that the solutions for the pair of Equations (23) and (44) in d dimensions can also be decomposed into spatial and temporal parts. However, in contrast to the linear case, the spatial part cannot be decomposed into d different coordinate components.…”

Section: Solutions With the Separation Of Variablesmentioning

confidence: 99%

“…This q-generalized thermostatistical theory has been useful in the study of a considerable number of physical systems, including long-range-interacting many-body Hamiltonian systems [11][12][13][14], low-dimensional dynamical systems [15][16][17][18][19], cold atoms [20][21][22], plasmas [23,24], trapped atoms [25], spin-glasses [26], power-law anomalous diffusion [27,28] and granular matter [29], high-energy particle collisions [30][31][32][33], black holes and cosmology [34,35], chemistry [36], economics [37][38][39], earthquakes [40], biology [41,42], solar wind [43,44], anomalous diffusion and central limit theorems [45][46][47][48][49][50][51][52][53], quantum entangled and non-entangled systems [54,55], quantum chaos [56], astronomic...…”

Section: Introductionmentioning

confidence: 99%

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Nonlinear q-Generalizations of Quantum Equations: Homogeneous and Nonhomogeneous Cases—An Overview

Nobre

Rego-Monteiro

Tsallis

2017

Entropy

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Recent developments on the generalizations of two important equations of quantum physics, namely the Schroedinger and Klein-Gordon equations, are reviewed. These generalizations present nonlinear terms, characterized by exponents depending on an index q, in such a way that the standard linear equations are recovered in the limit q → 1. Interestingly, these equations present a common, soliton-like, traveling solution, which is written in terms of the q-exponential function that naturally emerges within nonextensive statistical mechanics. In both cases, the corresponding well-known Einstein energy-momentum relations, as well as the Planck and the de Broglie ones, are preserved for arbitrary values of q. In order to deal appropriately with the continuity equation, a classical field theory has been developed, where besides the usual Ψ( x, t), a new field Φ( x, t) must be introduced; this latter field becomes Ψ * ( x, t) only when q → 1. A class of linear nonhomogeneous Schroedinger equations, characterized by position-dependent masses, for which the extra field Φ( x, t) becomes necessary, is also investigated. In this case, an appropriate transformation connecting Ψ( x, t) and Φ( x, t) is proposed, opening the possibility for finding a connection between these fields in the nonlinear cases. The solutions presented herein are potential candidates for applications to nonlinear excitations in plasma physics, nonlinear optics, in structures, such as those of graphene, as well as in shallow and deep water waves.

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MAGNETIC FIELD STRENGTH FLUCTUATIONS AND THEq-TRIPLET IN THE HELIOSHEATH:VOYAGER 2OBSERVATIONS FROM 91.0 TO 94.2 AU AT LATITUDE 30° S

Cited by 27 publications

References 42 publications

DETERMINATION OF INTERSTELLAR He PARAMETERS USING FIVE YEARS OF DATA FROM THE IBEX : BEYOND CLOSED FORM APPROXIMATIONS

DETERMINATION OF INTERSTELLAR He PARAMETERS USING FIVE YEARS OF DATA FROM THE IBEX : BEYOND CLOSED FORM APPROXIMATIONS

Economics and Finance: q-Statistical Stylized Features Galore

Nonlinear q-Generalizations of Quantum Equations: Homogeneous and Nonhomogeneous Cases—An Overview

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