adsabs/AstroCLIMB huggingface dataset:
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: The color scale shows the integrated intensity of the o‐H2D+(11,0–11,1) line, where pixels below the 3σ level have been masked. The mean uncertainty on the map is 1σ = 60 mK km s−1. The contours show the continuum emission at levels from 2 to 11σ, in steps of 3σ. Both continuum and line data are shown prior to primary-beam correction. The beam size and scale bar are indicated in the bottom left and right corners, respectively.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Results of the ACORNS clustering algorithm run on the results of the multicomponent Gaussian fitting of the N2H+ (1–0) transition, shown graphically as a dendrogram. The different colors represent distinct trees, labeled with letters, and they correspond to the structures shown in Figure D2. The four trees labeled with capital letters contain more than 70% of all data and 80% of the total flux.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Ppv diagram with the complete set of trees identified by ACORNS. The coordinates axes are expressed as offsets (in arcsec) with respect to the position R.A. = 18h17m22.ˢ0, decl. = −16°25′01.″7. Each color represent a different tree, and have correspondence in the dendrogram shown in Figure D1. Gray points do not belong to any cluster.
Paper: The Core Population and Kinematics of a Massive Clump at Early Stages: An Atacama Large Millimeter/submillimeter Array View
Authors: Elena Redaelli, Stefano Bovino, Patricio Sanhueza, Kaho Morii, Giovanni Sabatini, Paola Caselli, Andrea Giannetti, Shanghuo Li
Figure caption: Comparison of the o‐H2D+(11,0–11,1) spectra obtained toward AG14 with the APEX single-dish telescope (red histogram) and the ALMA interferometer (black histogram). See the text for the technical details about how the spectra were extracted.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Galactocentric radius variation of the integrated (total) monochromatic MIR luminosities of candidate star-forming regions per parental cloud mass (L MIR/M CO). Red circles and yellow squares show clouds with candidates with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). The sizes of these markers indicate the respective masses of their parental molecular clouds (small: M CO <103 M ⊙, medium: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). Magenta solid and dotted lines respectively indicate median and mean values of only candidates with contamination rates of less than 30% (reliable). Cyan solid and dotted lines indicate median and mean values of all candidates. These values are calculated in a 0.5 kpc binning from R G of 13.5 to 20.0 kpc. The gray areas indicate the concentrated areas considered to be spiral arms. Correlation coefficients (CC) are noted in the bottom right corners. Right: Galactocentric radius variation of the individual monochromatic MIR luminosities of candidate star-forming regions per parental cloud mass (L MIR/M CO). Notations are the same as in the left panels.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: The total (left) and individual (right) L MIR/M CO plotted against galactocentric radius. The adopted completeness limit is W-1 and F-1 (see Table 2). Cyan circles and light cyan squares show the star-forming regions with contamination rates <30% and ≥30%, respectively. The sizes of these markers indicate the respective masses of their parental molecular clouds (small: ≤ M CO <103 M ⊙, medium: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). Orange solid and dotted lines indicate the respective median and mean values of only candidates with contamination rates of less than 30% (reliable). Green solid and dotted lines respectively indicate the median and mean values of all candidates. These values are calculated in a 0.5 kpc binning from R G of 13.5 to 20.0 kpc. The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: The total (left) and individual (right) L MIR/M CO plotted against galactocentric radius. The adopted completeness limit is W-3 and F-1 (see Table 2). Green circles and right green squares show the star-forming regions with contamination rates <30% and ≥30%, respectively. The sizes of these markers indicate the respective masses of their parental molecular clouds (small: ≤ M CO <103 M ⊙, medium: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). Yellow solid and dotted lines indicate median and mean values of only candidates with contamination rates of less than 30% (reliable), respectively. Blue solid and dotted lines indicate median and mean values of all candidates. These values are calculated in a 0.5 kpc binning from R G of 13.5 to 20.0 kpc. The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: The total (left) and individual (right) L MIR/M CO plotted against galactocentric radius. The adopted completeness limit is W-2 and F-1 (see Table 2). Red circles and yellow squares show the star-forming regions with contamination rate <30% and ≥30%, respectively. The sizes of these markers indicate the respective masses of their parental molecular clouds (small: ≤ M CO <103 M ⊙, medium: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). Magenta solid and dotted lines indicate the respective median and mean values of only candidates with contamination rates of less than 30% (reliable). Cyan solid and dotted lines indicate median and mean values of all candidates. These values are calculated in a 0.5 kpc binning from R G of 13.5 to 20.0 kpc. The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Galactocentric radius variation of N SF/N all derived from three threshold values of each of the WISE and FCRAO data. The details of adopted threshold values (symbol names: W-1, W-2, W-3, F-1, F-2, and F-3) are described in Table 2. The circles and squares show the respective ratios for clouds with associated candidates with contamination rates less than 30% (reliable) and all clouds with associated candidates. The error bars represent Poisson errors (1σ). The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Same plot as Figure 14 but in three cloud mass ranges: M CO <103 M ⊙ (a, d), 103 M ⊙ ≤ M CO <104 M ⊙ (b, e), and 104 M ⊙ ≤ M CO (c, f). Only clouds with M CO ≥ 183.6 M ⊙ are plotted in (a, d). The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Identical to Figure 18, but for the threshold values W-1 and F-3.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Identical to Figure 18, but for the threshold values W-1 and F-2.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Identical to Figure 21, but for the threshold values W-2 and F-3.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: The stellar XUV and FUV/NUV SED, which is the spectrum of ε Eri taken from the MUSCLES Treasury Survey (France et al. 2016) and scaled at the orbital distance of WASP-52b. In panel (a), different solid lines represent the constructed spectra of different β  m . β  m  = 0.22 corresponds to the reference spectrum, which is taken from the MUSCLES Treasury Survey.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Three critical angles ϑ 1, ϑ 2, ϑ 3. Here the green line represents the tangent plane of the stellar sphere at the emission point B. R  S , R  P , and R  A  are the radii of the star, planet, and atmosphere, respectively.  e   i (s) and  e   i (p) are the basis vectors of the rest frames of the star and the planet, respectively.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: The solid angle ΔS(ϑ) of the planet subtended by a point located at a polar coordinate ϑ on the stellar surface. The dotted vertical lines denote the three critical angles defined in the text: cosϑ 1 (red), cosϑ 2 (green), and cosϑ 3 (blue). Here R  S  = 6.06697R  P , R  A  = 10R  P , and L = 44.8611856R  P  for WASP-52b.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: The geometrical relationships between vectors  r ,  r   s ,  r  0, and  p .
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: An illustration of Case 1, as 0 ≤ ϑ ≤ ϑ 1. The top panel is a schematic of the photon generation. The bottom panel shows the μ–ϕ plane, in which the solid angle of the effective photons is denoted by the gray area. The blue line represents the curve μ(ϕ). The gray area denotes the valid region in the μ–ϕ plane. Here ﹩{\mu }_{\alpha }=\cos {\theta }_{1}﹩ when ϑ = 0.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Same as Figure 4, but for Case 2, as ϑ 1 ≤ ϑ ≤ ϑ 2.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Same as Figure 4, but for Case 3, as ϑ 2 ≤ ϑ ≤ ϑ 3.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: (a) Source and sink terms related to the population of He(23 S) for the model with H/He = 98/2, F XUV = 0.5F 0, and β  m  = 0.3. The source terms plotted with the black dashed and dotted lines are in units of cm−3 s−1, and the sink terms plotted with the solid lines are in units of s−1. The dotted red lines and dashed green and cyan lines represent n  e  q 13a , n  e  q 31a , and n  e  q 31b  calculated using constant rate coefficients q 13a  = 4.5 × 10−22 cm3 s−1, q 31a  = 2.3 × 10−8 cm3 s−1, and q 31b  = 3.6 × 10−9 cm3 s−1. (b) The number density profile of He(23 S). The red solid and black dashed lines are calculated by using a temperature-dependent q  ij  and constant q  ij , respectively. (c) The transmission spectra of He 10830. The red solid and black dashed lines are calculated by using a temperature-dependent q  ij  and constant q  ij , respectively.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: (a) Pα as a function of atmosphere altitude for the plane–plane model. (b) Comparison of Hα transmission spectrum between the plane–plane, plane–spherical, and spherical–spherical models. (c) Pα of the plane–spherical model. (d) Pα of the spherical–spherical model with isotropic illumination. (e) Comparison of Hα transmission spectrum between three spherical–spherical models: a limb-darkened model with an atmosphere outer boundary size of 6R  P , a limb-darkened model with an atmosphere size of 10R  P , and an isotropic model with an atmosphere size of 10R  P . (f) Similar to panel (b), but for the He 10830 transmission spectrum. (g) Pα of the spherical–spherical model with an outer boundary size of 6R  P . Note that in panel (g) the value of Pα is slightly larger than 30 in the gray regions.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: (a–c) Absorption depth at the He 10830 line center as a function of F XUV and β  m  for the models of various H/He ratios. (d) He 10830 transmission spectra of the models, which describe the observation well. Here the models with F XUV = 0.5F 0 are the best-fit models, and the others are those calculated for experiments.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: Electron number densities as functions of the distance from Geminga for the slow-diffusion (D 0 = 5 × 1025 cm2 s−1) and fast-diffusion (D 0 = 2 × 1029 cm2 s−1) scenarios. Both the relativistic and nonrelativistic diffusion models are presented. The conversion efficiency is set to 100% for all the cases in this figure.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: Left: minimal χ 2 of best fit to the γ-ray halo profiles as a function of the diffusion coefficient at 1 GeV. Right: efficiency of energy transfer from the pulsar spin-down energy to electron/positron pairs for different values of D 0.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: Comparison of the γ-ray profiles for LHAASO J0621+3755 before and after PSF convolution.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: The γ-ray profiles of the Geminga halo (left) and LHAASO J0621+3755 (right) with D 0 corresponding to the two local minimal χ 2.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Hα and He 10830 transmission spectra of the best-fit model.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: ΣSFR as a function of estimated weight P DE, comparing the TIGRESS numerical results (Equation (26c), solid, as shown in Figure 13) to observations from several recent surveys of galaxies resolved at ∼kiloparsec scale. Observational results shown are from Leroy et al. (2008), Herrera-Camus et al. (2017), Sun et al. (2020a), and Barrera-Ballesteros et al. (2021). The previous numerical result from KOK13, Equation (27) is also shown (dashed). Also overlaid for reference is Equation (28) with constant ϒtot = 200, 1000, 5000 km s−1 (light gray lines, top to bottom).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: ΣSFR (40 Myr average) as a function of measured total midplane pressure P tot,2p, measured ISM weight ﹩{{ \mathcal W }}_{2p}﹩, and estimated weight P DE. Individual points from 1 Myr intervals as well as median values and 25th and 75th percentiles from the sampling intervals are also shown for each model. Solid lines show best-fit power laws and dotted and dashed lines show the results from KOK13 (see text).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Thermal, turbulent, and total pressure as a function of ΣSFR. Here, the ΣSFR for each point is based on an average over the past 40 Myr in the simulation, and the pressures represent horizontal midplane averages. Median values and 25th and 75th percentiles are also shown for each model. Solid lines show best-fit power laws, dotted lines show the results from KOK13, and black triangles show the analytic predictions for the thermal and turbulent pressures (see the main text).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Total pressure P tot ≡ P th + P turb + Πmag versus hydrogen density n H in the two-phase gas for all models. Midplane-averaged values at intervals of 1 Myr are shown with individual small circles, together with medians and 25th and 75th percentiles from the sampling intervals shown as large points. The best-fit power-law with slope 1.43 is shown as a dashed line. Dotted lines indicate isotherms of ﹩{T}_{\mathrm{eff}}={P}_{\mathrm{tot},2{\rm{p}}}/{({n}_{{\rm{H}},2{\rm{p}}}{k}_{B})=1.7\,\times \,{10}^{4}\,{\rm{K}}({\sigma }_{\mathrm{eff},2{\rm{p}}}/10\,\mathrm{km}\,{{\rm{s}}}^{-1})}^{2}﹩.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Thermal, turbulent, and total feedback yields as a function of P DE. Median values and 25th and 75th percentiles are also shown for each model. Solid lines show the best-fit power laws (see the main text).
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Ion and electron temperatures. (a) Time evolution of the (simulation box) averaged perpendicular temperature, T  i,⊥, parallel temperature, T  i,∥, total temperature, T  i , and temperature anisotropy, A  i , for the ions. The latter is normalized to its initial value. The components are defined with respect to the local mean magnetic field. (b) Same quantities as in panel (a), but for the electrons. (c–e) Contour plots of T  i,⊥, T  i,∥, and A  i . (f–h) Contour plots of T  e,⊥, T  e,∥, and A  e . In panels (c)–(h), the maximum and minimum values of each quantity are reported in the lower left corner.
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Contour plots of the logarithm of the magnitude of the magnetic fluctuations, ∣δ  B ∣2 = ∣ B  −  B  0∣2 (left column), and of the current density, ∣ J ∣2 (right column), at t = t peak, both in the whole simulation box (top row) and in a subdomain (bottom row). Magnetic vortices are compared with circles of radius r = d  i,e , and current sheet widths are compared with lines of length l = d  i,e .
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Identification of magnetic reconnection events through the indicators C1–C4 from Agudelo Rueda et al. (2021). (a) Contour plot of the out-of-plane vector potential A  z . The black isocontours represent magnetic field lines. Green stars mark the saddle points, which represent potential reconnection sites. (b) Contour plot of the magnitude of the magnetic fluctuations, with arrows marking the direction of the local magnetic field. (c–h) Contour plots of Ψ/Ψth − 1, with Ψ = ∣ u   i ∣, ∣ u   e ∣, ∣ J  ·  E ∣, T  i , and T  e , respectively. These panels all have the same color scale as in panel (c). (h) Classification of some reconnection events as “standard” or “electron-only” by superimposing the areas where ∣ u   e,⊥∣ (red) and ∣ u   i,⊥∣ (blue) exceed their respective thresholds.
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Spectral behavior of the electromagnetic and plasma fluctuations. (a) Power spectra of the magnetic field  B , the electric field  E , the ion bulk velocity  u   i , and the electron bulk velocity  u   e  with the respective noise in dashed lines (top) and corresponding signal-to-noise ratio S/N (bottom). Vertical dashed black lines mark the particle characteristic scales, i.e., the ion and electron inertial length d  i,e  and gyroradius ρ  i,e . (b) Power spectra of the magnetic field  B  (top) and of the electron bulk velocity fluctuations  u   e  (bottom), compensated by different power laws (and by an exponential cutoff for  B ). The gray area marks the scales at which S/N < 3.
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Direct comparison between the power spectra of the kinetic simulation, P kin, and those of the hybrid simulation, P hyb, for (a) the magnetic field  B , (b) the electric field  E , (c) the ion bulk velocity  u   i , (d) the electron bulk velocity  u   e , (e) the ion density n  i , and (f) the parallel magnetic field  B  ∥. For each field, the ratio P hyb/P kin is also shown in the bottom panels.
Paper: Anisotropic Electron Heating in Turbulence-driven Magnetic Reconnection in the Near-Sun Solar Wind
Authors: Luca Franci, Emanuele Papini, Alfredo Micera, Giovanni Lapenta, Petr Hellinger, Daniele Del Sarto, David Burgess, Simone Landi
Figure caption: Time evolution of some global quantities. (a) The rms value of the out-of-plane and in-plane components of the current density,  J  ∥ and  J  ⊥. (b) Maximum of the magnitude of the current density, ∣ J ∣, in the whole simulation box. (c) The rms of the components of the magnetic fluctuations,  B  ⊥ and  B  ∥, and of ion bulk velocity,  u   i,⊥ and  u   i,∥. In all panels, a vertical dashed green line marks the time when the rms of  J  ∥ reaches a maximum, i.e., when turbulence has fully developed. In panel (b), a vertical dashed black line marks the time when reconnection events start occurring, which also corresponds to the time when  B  ⊥ starts decreasing, indicated by the vertical dashed red line in panel (c).