adsabs/AstroCLIMB huggingface dataset:
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: NFW halo fits to the lensing signal and correlations in the fitted parameters. The lower panels show the Pearson product-moment correlation coefficient ρ between the concentration c and the halo mass Mhalo, with the 68th and 95th percentile contours indicated. The nominal (i.e., median) values of these parameters are marked with dashed gold lines. Note that the fit and all its derived parameters (including the uncertainties, χ2, and ρ) only consider the data points not in the shaded region, as discussed in Section 3.5. The stellar masses quoted in the top plots do not include systematic uncertainties in the stellar population modeling, but the impact of these systematic effects on our derived halo masses and concentrations is minimal (see Section 3.5).
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: TS (top) and PS (bottom) maps around NGC 3281. The black plus and blue cross indicate the optical and X-ray position of NGC 3281, respectively. The black circle marks the 95% error circle of the γ-ray localization. The color bars indicate the range of the TS/PS values. The TS map has a pixel size of 0﹩\mathop{.}\limits^{^\circ }﹩03 and shows a pointlike source consistent with the optical/X-ray position. We note that the maximum TS is different from that reported in the text (42.73) as the power-law photon index is fixed at 2 in generating the map. The PS map has a pixel size of 0﹩\mathop{.}\limits^{^\circ }﹩1 and shows no value above 6.24 (5σ).
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: The RΔΣ signal of our lenses (postmergers and nonmerging controls). R is the distance from the center of the lens and ΔΣ is the excess surface density. The lensing amplitudes include boost correction and random subtraction.
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: The X-ray and γ-ray spectra and best-fit models assuming two different NH in the context of the corona model. The thin and thick lines represent the intrinsic and attenuated models, respectively.
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: X-ray and γ-ray light curves of NGC 3281. The BAT light curve in the unit of 10−4 counts s−1 is binned at a step of 100 days. The LAT light curve in the unit of 10−11 erg s−1 cm−2 is binned at a step of 1 yr. Gray arrows represent the 95% upper limit if TS < 4.
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: Sky coverage of the true lenses (left) and random lenses (right).
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: ASKAP image at 1.4 GHz. The contours are 3, 6, 12, 24, 48, 96, and 192σ (0.144 mJy beam−1), respectively.
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: Gamma-ray vs. radio luminosities for AGNs in Y. Fukazawa et al. (2022) and this source.
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: Optical depth of pair production (left) and fraction of transmission (right) as a function of γ-ray frequency/energy for the corona model.
Paper: Testing the Kerr Paradigm via Synchrotron Radiation
Authors: M. Ghasemi-Nodehi, Fatemeh S. Tabatabaei, Lang Cui
Figure caption: Flux density spectrum with different αn for Kerr and CPR metric. Here we fixed the spin as 0.9, the viewing angle as 17°, B = 15 G, l = 300 pc, and K = 100. For the Kerr/CPR case with different αn, the lines are not parallel; for higher αn values, the lines decrease faster.
Paper: Testing the Kerr Paradigm via Synchrotron Radiation
Authors: M. Ghasemi-Nodehi, Fatemeh S. Tabatabaei, Lang Cui
Figure caption: Flux density at 10 GHz as a function of αn. We fix frequency in Figure 1 at 10 GHz as an example. Then we plot flux density vs. αn. The CPR spacetime produces higher flux than that of Kerr spacetime.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Contour plot of the two-dimensional covariance function for PSR B1937+21 observed with the FAST on MJD 58725. The 1D ACFs in time and frequency are presented in the lower and right panels, respectively. The diffractive scintillation timescale, exponential index, and decorrelation bandwidth are estimated from the best fit indicated with the blue solid curves, where the red stars are the measured values.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Time series of spectral indices derived from power-law fits to the diffractive scintillation parameters determined from the FAST observations: parabolic arc curvature (η), decorrelation bandwidth (Δνd), spectral exponent (α), and scintillation timescale (Δτd).
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Frequency dependence of the basic measurements of diffractive scintillation determined from the FAST observations: parabolic arc curvature (η), decorrelation bandwidth (Δνd), spectral exponent (α), and scintillation timescale (Δτd).
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: The one-dimensional ACFs along time and frequency lags are presented in the left and right panels, respectively. The scintillation timescale, spectral exponent, and decorrelation bandwidth at multiple frequency bands are estimated from the best fit indicated with the blue solid curves.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Secondary spectrum from a FAST observation of PSR B1937+21 on MJD 58725. The ordinate and abscissa are the Fourier conjugates of time and frequency, respectively. The red dashed curve and shaded region show the best-fit curvature and 1σ error overlaid on the secondary spectrum.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: The secondary spectra of PSR B1937+21 observed with the FAST on MJD 58725. The central frequency and arc curvature are indicated in each panel. The ordinate and abscissa are the Fourier conjugates of time and frequency, respectively.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Example of a dynamic spectrum of PSR B1937+21 observed with the FAST on MJD 58725, which shows apparent variation in the intensity received at the telescope at a given frequency and time. The color-coded intensity as a function of time and frequency is given in arbitrary units in the bar on the right side.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: The correlation between parabolic arc curvature (η), decorrelation bandwidth (Δνd), spectral exponent (α), diffractive timescale (Δτd), and refractive timescale (Δτr). The red dashed lines represent the linear function fitting. The value of ρ in each panel is the Pearson product-moment correlation coefficient.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Time series of basic measurements of diffractive scintillation determined from the FAST observations: parabolic arc curvature (η), decorrelation bandwidth (Δνd), spectral exponent (α), diffractive timescale (Δτd), and refractive timescale (Δτr).
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Posterior probability distributions for the parameters in the anisotropic scattering model using MCMC sampler. The contours in the 2D distributions indicate the 1σ, 2σ, and 3σ confidence levels, and the blue lines represent the mean values for each parameter.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Posterior probability distributions for the parameters in the isotropic model using MCMC sampler. The contours in the 2D distributions mark the 68%, 95%, and 99.7% confidence intervals, and the blue lines mark the mean for each parameter.
Paper: Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST
Authors: Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen, Chengbing Lyu
Figure caption: Annual curvature variations with best-fit anisotropic (upper panel) and isotropic (lower panel) scattering screen models.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Magnetic energy spectrum gradient, α(r), as a function of radius. We show the fitting for α(r) using 15–35 deg. In (a), the black dashed line shows β(r) for Jupiter’s spectrum. Color indicates the amplitude of the imposed axial dipole at the lower boundary, while each panel contains models with a specific helium rain location, where gray shading shows where ﹩d\tilde{s}/dr﹩ is positive, i.e., the subadiabatic region.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: (a) Schematic showing interior structure of Jupiter based on B. Militzer & W. B. Hubbard (2024) (five-layer reference model) in the left slice, and our numerical dynamo model setup in the right slice. (b) the areas of stable stratification in the various models, with the model names (Table 1)—referring to the helium rain layer extent—labeled.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Time-averaged Lowes spectra at model surface (ro = 0.97RJ) for six models with no imposed axial dipole field and varying helium rain layer locations. Green lines correspond to the total spectrum, orange includes only the axisymmetric component, m = 0, and purple is the nonaxisymmetric spectrum.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: (a) and (d) are schematic slices to put the results into the Jupiter context. They link with the two helium rain layer examples shown in schematic (b) to aid in the interpretation of (c), which shows inferred Lowes radius as a function of helium rain layer location, computed using ℓ = 15–35. Very similar rLowes are obtained for models with no helium rain layer, so an average is plotted (gray horizontal line).
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: 3D visualizations of two dynamo models, both with an imposed axial dipole of amplitude 1 with a shallow helium rain layer (0.826–0.887RJ, left) and a deep helium rain layer (0.772–0.833RJ, right). Top panels: radial magnetic field. Bottom panels: radial (green/purple color map) and zonal (red/blue color map) velocity.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Comparison of rLowes obtained via fitting of the nonaxisymmetric spectral components between ℓ = 3 and 18 (directly comparable to Jupiter measurements) and fitting of the total spectrum between ℓ = 15 and 35.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: (a) Horizontally averaged rms nonaxisymmetric velocity (Equation (29)), in units of Re, for the six models without an imposed dipole and varying helium rain layer location. (b) Left axis: relevant length scales, i.e., electrical conductivity scale height Hσ (black dashed line) and local layer thickness for each model; right axis: magnetic diffusivity. (c) Local magnetic Reynolds number based on nonaxisymmetric flow and Equation (31). Thicker lines are used in the regions where each model’s helium rain layer lies.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Estimation of local magnetic Reynolds number as a function of radius for Jupiter. The lower and upper bound of each envelope is based on a velocity of 1 mm s−1 and 1 cm s−1, respectively. The colors represent three different length scales used in the definition of Rm. Two conservative estimates of the dynamo radius, based on where Rm reaches 10 corresponding to 1 mm s−1 velocity, L = 0.1RJ and L = Hσ, are marked with a horizontal dashed line and a dotted line.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Schematic illustrating the effect of passing through a nonelectrically conducting zone on a magnetic spectrum. This idealized schematic assumes that the inferred dynamo radius rlowes is equal to the actual dynamo radius rd.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Time-averaged poloidal magnetic energy spectra for six models with no imposed axial dipole field and varying helium rain layer locations. Green lines correspond to the spectra at the model surface (ro = 0.97RJ), pink lines are the spectra at each model’s Lowes radius, and orange is the surface spectrum extrapolated down to the inferred Lowes radius.
Paper: On the Meaning of the Dynamo Radius in Giant Planets with Stable Layers
Authors: Paula N. Wulff, Hao Cao, Jonathan M. Aurnou
Figure caption: Lowes–Mauersberger spectra for model HR0-B0. Colored lines are instantaneous spectra, while the black line shows the averaged spectrum, used for the Lowes analysis in this study.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Running perpendicular diffusion coefficient d⊥(t) at rg/Lc = 8.9 × 10−3 and for various turbulence levels η. The solid lines show the mean over the ensemble of turbulent magnetic fields, and the shaded band indicates the standard mean error. The dashed lines indicate the suppressed ballistic growth. The dotted horizontal lines show the asymptotic diffusion coefficients κ⊥ , and the vertical dotted–dashed lines show the scattering time ﹩{\tau }_{\,\rm{s}\,}^{{\prime} }﹩, increased due to the suppression of the ballistic growth.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Asymptotic parallel and perpendicular mean free paths λ∥ and λ⊥ as a function of reduced rigidity rg/Lc for different turbulence levels η = 0.2,  0.5,  0.8, and 1. We also compare the results of our test particle simulations with the data of G. Giacinti & J. G. Kirk (2017) (empty circles, squares, and pentagons) as well as R. López-Coto & G. Giacinti (2018) (empty hexagons). We have indicated power laws ﹩\propto {({r}_{\rm{g}\,}/{L}_{\,\rm{c}})}^{1/3}﹩ for rg/Lc < 10−1 and ﹩\propto {({r}_{\rm{g}\,}/{L}_{\,\rm{c}})}^{2}﹩ for rg/Lc > 1.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Running parallel diffusion coefficient d∥(t) at rg/Lc = 8.9 × 10−3 and for various turbulence levels η. The solid lines show the mean over the ensemble of turbulent magnetic fields, the shaded band indicates the standard mean error. The dashed lines indicate the suppressed ballistic growth. The dotted horizontal lines show the asymptotic diffusion coefficients κ∥ , and the vertical dotted–dashed lines show the scattering time ﹩{\tau }_{\,\rm{s}\,}^{{\prime} }﹩, increased due to the suppression of the ballistic growth.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Pitch-angle autocorrelation function C(t) for rg/Lc = 8.9 × 10−3 and different turbulence levels η. The dashed vertical line indicates Ωt = 2π. The dotted lines are fits of the form ﹩A\exp [-t/\tau ]﹩ to the different C(t) for Ωt > 2π.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Ratio λ⊥/λ∥ of the asymptotic perpendicular and parallel mean free paths as a function of reduced rigidity rg/Lc for different turbulence levels η. We have indicated a constant ratio at low rigidities and a ﹩{({r}_{\rm{g}\,}/{L}_{\,\rm{c}})}^{0.2}﹩ dependence at intermediate rigidities, as suggested by A. Dundovic et al. (2020).
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Same as Figure 5, but for fixed η = 0.5 and various reduced rigidities rg/Lc. The gray dashed line indicates the initial, unsuppressed ballistic phase.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Running parallel and perpendicular diffusion coefficients d∥(t) and d⊥(t), respectively, for η = 0.5 and for various reduced rigidities rg/Lc. The dotted and dashed–dotted lines indicate the asymptotic diffusion coefficients κ∥ and κ⊥, respectively.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Same as Figure 3, but for fixed η = 0.5 and various reduced rigidities rg/Lc. The gray dashed line indicates the initial, unsuppressed ballistic phase.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Pitch-angle autocorrelation function C(t) for η = 0.5 and different reduced rigidities rg/Lc. The dashed vertical line indicates Ωt = 2π.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Comparison of the running diffusion coefficients computed with the Boris push solver and an adaptive fourth-order Runge–Kutta solver. We have adopted a reduced rigidity of rg/Lc = 0.089 and the turbulence level η = 0.1. In the top panel, the running parallel diffusion coefficient d∥ is shown, in the bottom panel, the running parallel diffusion coefficient d⊥. The colors blue, orange, and green refer to three turbulent field realizations, with the results for the Boris push method shown with solid lines and dark colors and those for the Runge–Kutta solve with dashed lines and light colors. Note that the same random realizations have been used for the Boris push and the Runge–Kutta methods. We have used a linear ordinate axis in order to be able to appreciate the similarity between the results for both methods.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Comparison of the running diffusion coefficients using the harmonic and the grid-based methods for setting up the turbulent magnetic fields for rg/Lc = 0.089 and η = 0.5. The parallel (perpendicular) running diffusion coefficients are indicated by dashed (solid) lines, their asymptotic values by dotted (dotted–dashed) lines; shaded bands indicate the respective standard mean errors. The asymptotic values have been computed by averages beyond the time indicated by the dotted vertical lines.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Running field line diffusion coefficients dFL(s) with respect to arc length s (purple) and dFL(z) with respect to the z-coordinate (gray) for a turbulence level η = 0.091. The lines show the mean over the ensemble of turbulent magnetic fields, and the shaded bands indicate the standard mean error.
Paper: Diffusion of Relativistic Charged Particles and Field Lines in Isotropic Turbulence. I. Numerical Simulations
Authors: Marco Kuhlen, Philipp Mertsch, Vo Hong Minh Phan
Figure caption: Asymptotic parallel and perpendicular mean free paths λ∥ and λ⊥ as a function of turbulence levels η for a subset of reduced rigidities rg/Lc. The solid and dotted lines show the fitted λ∥ and λ⊥, respectively, see Equations (48) and (49).