adsabs/AstroCLIMB huggingface dataset:
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: (a): Relativistic mirror instability thresholds (anisotropy η as a function of β ∥,e ) defined by Equations (B27)–(B28) calculated for different ϵ ⊥ represented by different colors from darkest (ϵ ⊥ = 0.01) to brightest (ϵ ⊥ = 100). The dotted black line represents a nonrelativistic limit. (b): Ratio of relativistic mirror instability threshold value β ∥,e  and its nonrelativistic limit β ∥,e,nr as a function of η. (c): Ratio of relativistic mirror instability threshold value β ∥,e  and its ultrarelativistic limit β ∥,e,ur, defined by Equation (B30) as a function of η.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Time evolution of accretion rate ﹩\dot{M}﹩ (panel (a)), magnetic flux Φ (panel (b)), and normalized magnetic flux ﹩{{\rm{\Phi }}}_{\mathrm{BH}}/\sqrt{\dot{M}{r}_{g}^{2}c}﹩ (panel (c)) after 8000r  g /c measured at 2r  g  for two spin parameters: a = 0.98 (black) and a = 0.5 (blue). Shaded regions correspond to quiescent periods of 1000r  g /c chosen for GR radiative transfer analysis: 14,300 − 15,300r  g /c for a = 0.98 and 16,000–17,000r  g /c for a = 0.5.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The survey areas of Orion B. The areas observed with various molecular lines are marked in white (13CO and C18O), red (N2H+ and HCO+), yellow (CS and SO), and green (NH2D and H13CO+) boxes on the Herschel 250 μm continuum image.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Same as Figure 12 but for ϵ ⊥ = 3 and ν/ν  c  = 10.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Models used in the radiative transfer of GRMHD simulation, represented by different colors: mirror and whistler (T ⊥,e  > T ∥,e ) and firehose (T ⊥,e  < T ∥,e ).
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Numerically calculated λ as a function of ϵ ⊥ for T ⊥,e /T ∥,e  = η  λ  for an anisotropic relativistic bi-Maxwellian distribution function. A simple fit for λ is given in Equation (C1).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Virial parameters for the filaments with (left panel) and without (right panel) dense cores. The virial parameters for the filaments derived considering thermal support only, nonthermal support only, and both thermal plus nonthermal support are represented by a red asterisk, green plus, and blue circle symbols, respectively. The horizontal lines indicate the filament’s virial parameter (﹩{M}_{\mathrm{line}}^{\mathrm{crit}}/{M}_{\mathrm{line}}﹩) of 2 (blue dashed line) and unity (red dashed line).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Defining the main properties of the identified velocity-coherent filament. Here, F20 is given as an example. (a) The integrated intensity (for Gaussian area) image. (b) The velocity centroids distribution. (c) The distribution of velocity dispersion. (d) Spine and branch, filament length, and radial cuts of the filament to produce the radial profiles. The path of the spine and branch are indicated with red points and blue points in panel (d). The red dots indicate the path of the spine, blue dots indicate an additional branch, and the curve (sky blue color) indicates the smoothed path of the spine, which is used for estimating the length of the filament. The black straight thin lines in panel (d) are drawn perpendicularly across the spine at the evenly sampled data points for drawing radial profiles in Figure 12.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Number of dense cores in each filament as a function of the ratio between M line and ﹩{M}_{\mathrm{line}}^{\mathrm{th},\mathrm{crit}}﹩. The cyan vertical line indicates the location where the M line equals ﹩{M}_{\mathrm{line}}^{\mathrm{th},\mathrm{crit}}﹩ and the black dashed line shows the location where the filament does not contain any dense core. The circle and asterisk symbols indicate that the filaments do not contain any YSOs and do contain YSOs, respectively. Colors distinguish the filaments with dense cores (red) from the filaments without dense cores (green). The numbers indicate the filament’s ID.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The dust temperatures obtained using the Herschel data toward the filamentary structures. The column densities for the filaments were calculated using these dust temperatures. The cyan vertical line indicates the median value (14.8 K) of the Herschel dust temperature distribution toward the filaments.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Virial parameters for the dense cores with (left panel) and without (right panel) YSOs. The horizontal line marks the location of the critical value of the virial parameter, α crit = 2. The blue line indicates the best fit of data points with a power-law index of −0.7. Magenta and cyan circles are to indicate the starless dense cores C14 and C22 with NH2D detection (see Section 4.7).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The radial profiles of F20 drawn along the black line cuts in Figure 11(d), which are evenly made with an interval of 25″. The gray lines represent individual radial profiles and the black line represents the average profile. The red line depicts the Gaussian-fitted profile. The number in the figure is the FWHM of the Gaussian-fitted profile in the unit of pc.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Virial parameters for the dense cores and filaments as a function of their characteristic scales. The characteristic scale is given as the deconvolved core radius R core for dense cores and the filament length L for filaments. Red and green-filled circles indicate dense cores with and without YSOs, respectively. Blue-filled and black open circles indicate filaments with and without dense cores, respectively. The horizontal line marks the virial parameter of 2.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The distribution of N2H+ dense cores identified by the FellWalker algorithm in the Orion B region (blue polygons). The color tones indicate the integrated intensity image of the N2H+. Asterisks denote YSOs from Furlan et al. (2016) represented regardless of evolutionary stage. The dense core ID is labeled in a decreasing sequence of peak brightness.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The velocity-coherent filaments and Herschel continuum filaments. The velocity-coherent filaments identified with the C18O (1–0) line emission in this study are presented by colored shades with their filament names. The Herschel continuum filaments defined by Arzoumanian et al. (2019) using a Herschel column density map are indicated with curved lines.
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: The PSP observations of switchbacks. The panels in the top half are from 2018 November 5, during the first encounter at about 35 R  s  from the Sun, and the rest are from 2022 May 30 to June 1 during the 12th encounter between 30 and 13.3 R  s  distance. The top and bottom middle panels show the radial field B  r  with 0.22 s time cadence containing switchbacks where the black line is inside the blue areas. The panels in the middle show hourly averages of radial velocity u  r , magnitude of B  r , number density, radial wave speed v = u  r  + v A, and the Alfvénic Mach number M A = u  r /v A. For the 12th encounter, the 24 hr period prior 19:00 UT May 31 is shown, as there are no public plasma data after that. The wave speed varies along the PSP orbit in both cases. The panels on the right show the high-cadence observations of the three components of the magnetic field for half-hour periods. The background is removed by subtracting a 7.4 minute sliding average. During the first encounter, all three components vary with similar amplitudes. For the second encounter, dBR is multiplied by 4 to make its variation similar to the perpendicular oscillations. The correlation coefficients r(dBR, dBT) and r(dBR, dBN) are calculated over a 2 minute sliding window. The light red rectangles highlight where dBR is highly correlated with dBT or dBN. The yellow rectangles highlight anticorrelation, where the signs are opposite. The green rectangles indicate times when B  r  is approximately constant. The bottom left panel shows one of these times, when dBT and dBN vary with similar amplitudes consistent with roughly circularly polarized Alfvén waves. The top left panel shows BR, the magnetic field magnitude B, the density n (all smoothed over 9.6 s), and the correlation coefficient r(B, n) for a selected short time period with many switchbacks.
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: Numerical solutions of sheared circularly polarized Alfvén waves in a double periodic box. Colors show the components of the magnetic field and velocity. Black lines are field lines and streamlines. In the top left panels, the long-wavelength λ  y /λ  r  = 10 shear produces a highly distorted Alfvén wave. Only a part of the domain is shown where the shear is maximal. The parameters are B  r  = 1, p = 1, v 1 = 0.5 (by perturbing B  r ), and time t = 20. In the top middle panels, the comparable wavelength shear λ  y /λ  r  = 1.25 results in a complex spherically polarized Alfvén wave solution. The parameters are B  r  = 0.5, p = 1, v 1 = 0.5 (by perturbing u  r ), and t = 6.6. In the top right panels, the small wavelength shear λ  y /λ  r  = 0.25 results in distorted field lines but no switchbacks. The parameters are B  r  = 0.5, p = 1, v 1 = 0.2 (by perturbing u  r ), and t = 40. Bottom row: cuts along r = 0 in the full domain for the three simulations. Solid lines show the −B  r  magnetic field component, while the dotted lines are the u  r  velocity components in the coordinate system moving with the wave.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: CS (2–1), HCO+ (1–0), C18O (1–0), H13CO+ (1–0), and the isolated hyperfine component of N2H+ (1–0) line profiles of dense cores. All the profiles shown here are the average ones for the spectra over the dense core. The vertical dashed line is the systemic velocity obtained from N2H+ hyperfine fitting.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The integrated intensity maps of HCO+ (1–0) (red), H13CO+ (1–0) (green), and CS (2–1) (blue) lines. The contour levels for HCO+ (1–0) are 0.041 K km s−1 × [5, 10, 15, 20, 30, 40, 70, 100, 130], those for H13CO+ (1–0) are 0.026 K km s−1 × [5, 8, 13, 18, 25, 30, 40], and those for CS (2–1) are 0.037 K km s−1 × [5, 10, 15, 20, 30, 45, 60, 80, 100]. The grayscale and color-shaded regions in the background indicate Herschel H2 column density distribution and observing regions for each line, respectively.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Distribution of filaments and the N2H+ cores. The contours in various colors are the same as the filaments presented in Figure 7(a) and the shaded box and gray tones indicate the N2H+ observed region and N2H+ (1–0) integrated intensity.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Time evolution of Maxwell stress (top) and variation rates of ﹩[{B}_{\phi }^{2}]﹩ (middle and bottom) averaged over the domain in the rising and saturated phases of the most active period in the cylindrical simulation with H 0/R 0 = 0.1. The middle panel compares the radial compression (red solid) and shear (blue dotted) terms. The bottom panel presents the total compression (red solid) and shear (black dashed) terms.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: An example for the amplification of a magnetic field by shearing terms. The magnetic field is distributed with −B  R  B  ϕ  > 0, which is the usual situation in the system with inner-fast differential rotation. B  ϕ  increases by radial differential rotation of v  ϕ , which is represented by (R                      ﹩\displaystyle \mathop{\Rightarrow }\limits_{R}﹩                      ϕ) (blue). B  R  increases by the inward (outward) motion of the inner (outer) region as a result of the outward transport of angular momentum, which is represented by (ϕ                      ﹩\displaystyle \mathop{\Rightarrow }\limits_{\phi }﹩                      R) (red).
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Conceptual cartoon for the role of the compressible term in the amplification of B  ϕ  (or B  z ) (red lines). The initial uniform field (left panel) is amplified in converging flows (shaded regions of right panel) and diluted in diverging flows (white regions of right panel) by the radial component of epicyclic oscillations. The magnetic energy ﹩\propto [{B}_{\phi }^{2}]﹩ in the right panel is double the initial value, while the magnetic field strength =[B  ϕ ] is conserved (see text).
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Time evolution of magnetic energy (top) and the variation rate of B  z  2 by shearing from ϕ to z (bottom) averaged over the domain in the declining phase of the same active period shown in Figure 7. What are shown in the top panel are the three components of ﹩[{B}_{i}^{2}]﹩ with i = R (black dotted), ϕ (blue solid), and z (red dashed), normalized by the respective time-averaged values, ﹩\overline{[{B}_{i}^{2}]}﹩, during t = 25–300 rotations. ﹩[{B}_{i}^{2}]/\overline{[}{B}_{i}^{2}]=1﹩ is plotted by the black thin solid line. In the bottom panel, the time average, ﹩\overline{[\phi \displaystyle \mathop{\Rightarrow }\limits_{\phi }z]}=+9.71﹩, is also plotted by the black dotted line.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Left: the shearing term, [i                      ﹩\mathop{\Rightarrow }\limits_{i}﹩                      j], stands for the generation (or decay) of B  j  from B  i  by the i derivative of v  j . Right: the compressible term, [i                      ﹩\mathop{\Rightarrow }\limits_{j}﹩                      i], represents the convergent amplification (or divergent disperse) of B  i  by the j derivative of v  j .
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Radial distance (horizontal) vs. time (vertical) diagram for radial displacements taken from the numerical data of the cylindrical case with H 0/R 0 = 0.1.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Radial distance (horizontal) vs. time (vertical) diagram for radial displacements by epicyclic oscillations for H 0/R 0 = 0.1.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Physical picture of the viscous-type instability. See text for the detailed explanation.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Comparison of time-averaged radial profiles of various physical quantities of the case with H 0/R 0 = 0.1 in the inactive (left) and active (right) periods. The top panels show angular momentum fluxes carried by Maxwell stress (black solid), Reynolds stress (red dotted), and mean accretion flow (blue dashed). The middle panels compare rms B  R  (magenta dashed–dotted), B  ϕ  (blue dashed), and B  z  (black solid). The initial vertical field strength, B  z,init, is multiplied by a factor of 10 (red dotted), in order to compare with the field strength in the saturated state. The bottom panels show density (black solid) in comparison to the initial distribution (red dotted) and the inverse of plasma β = 8π p/B 2 (blue dashed). We note that the vertical scales of the top and middle panels are different for the left and right panels. See Section 2.1 for the physical units on the vertical axes.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Scatterplots of dimensionless Maxwell stress, α M, against ﹩{B}_{z}^{2}/4\pi \rho {c}_{{\rm{s}}}^{2}﹩ (left), ﹩{(\rho /{\rho }_{0})}^{-1}﹩ (middle), and ﹩{B}_{z}^{2}/4\pi ﹩ (right) at t = 82.4 rotations. The data are averaged over 2 radial and 16 azimuthal grid cells of the 2D plots in Figure 12. The slope of y ∝ x is overlaid in the left and middle panels by the red solid line, and y ∝ x 0.5 is shown in the left panel with the blue dashed line.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Shearing boundary condition in a local cylindrical box. The simulation domain, which is enclosed by the solid black line, is between R = R − and R +. R −,d  (R +,d ) is the radial location of the innermost (outermost) cells in the simulation domain, which are illustrated by gray shading. R −,g  (R +,g ) is the radial location of the inner (outer) ghost cells. The physical quantities of the ghost cell at R = R ±,g (red) are determined from those of the corresponding sheared cells at R = R ∓,d  (blue) and the radially adjacent cell(s) at R = R ±,d  (green). See text for details.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Same as Figure 15, but for cases with different f amp,± averaged over 25–300 rotations. The left, middle, and right panels are for (f amp,+, f amp,−) = (1.02, 0.93), (1.06, 0.96), and (1, 1), respectively. Note that the physical quantities in the left panels are the average of those in both active and inactive phases shown in Figure 15.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Same as Figure 2, but for cases with different f amp,± for H 0/R 0 = 0.1. The red dotted, black solid, and blue dashed lines are for (f amp,+, f amp,−) = (1.02, 0.93), (1.06, 0.96), and (1, 1), respectively. Note that the first case (red dotted) corresponds to the same one presented in the main text (the red solid line in Figure 2).
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Same as Figure 4, but for cases with different f amp,± for H 0/R 0 = 0.1. The left, middle, and right triangles correspond to those in Figure 20. Note that the left triangle is the same as the top right triangle in Figure 15.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Triangle diagrams for the cylindrical case with H 0/R 0 = 0.1 (top right triangle of Figure 4). The left and right triangles are the results of the active ([α M] > 0.13) and inactive ([α M] < 0.13) periods, respectively.