adsabs/AstroCLIMB huggingface dataset:
Paper: Unusual Martian Foreshock Waves Triggered by a Solar Wind Stream Interaction Region
Authors: Zhenpeng Su, Yuming Wang, Tielong Zhang, Zhiyong Wu, Long Cheng, Zhuxuan Zou, Chenglong Shen, Jingnan Guo, Sudong Xiao, Guoqiang Wang, Zonghao Pan, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yutian Chi, Mengjiao Xu
Figure caption: Unusual Martian foreshock waves observed by Tianwen-1. (a) Empirical bow-shock configuration (Trotignon et al. 2006; black dashed line) and Tianwen-1's orbit (gray dashed line) and bow-shock crossing point (orange dot) in the X MSO–﹩\sqrt{{Y}_{\mathrm{MSO}}^{2}+{Z}_{\mathrm{MSO}}^{2}}﹩ plane. (b) Magnetic field components (B x, B y, B z) and magnitude B t with a 1 Hz sampling rate in the MSO coordinate system. (c) and (d) Compressional and transverse magnetic power spectral densities (color-coded) from the wavelet transform of the magnetic fields with a sampling rate of 32 Hz.
Paper: Unusual Martian Foreshock Waves Triggered by a Solar Wind Stream Interaction Region
Authors: Zhenpeng Su, Yuming Wang, Tielong Zhang, Zhiyong Wu, Long Cheng, Zhuxuan Zou, Chenglong Shen, Jingnan Guo, Sudong Xiao, Guoqiang Wang, Zonghao Pan, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yutian Chi, Mengjiao Xu
Figure caption: Overview of solar wind upstream of Martian bow shock. (a) Magnetic field components (B x, B y, B z) and magnitude B t in the Mars-centered Solar Orbital (MSO) coordinate system. (b)–(d) Proton velocity V p, density N p, and temperature T p. The two vertical dashed lines mark the time points around which the solar stream interface and the unusual foreshock waves occurred.
Paper: Unusual Martian Foreshock Waves Triggered by a Solar Wind Stream Interaction Region
Authors: Zhenpeng Su, Yuming Wang, Tielong Zhang, Zhiyong Wu, Long Cheng, Zhuxuan Zou, Chenglong Shen, Jingnan Guo, Sudong Xiao, Guoqiang Wang, Zonghao Pan, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yutian Chi, Mengjiao Xu
Figure caption: Martian foreshock wave properties. (a)–(c) Three representative segments of waveforms in the MSO coordinate system. Colors help differentiate among three magnetic field components. (d) and (e) Hodogram of bandpass waveform on the basis of minimum variance analysis.
Paper: Unusual Martian Foreshock Waves Triggered by a Solar Wind Stream Interaction Region
Authors: Zhenpeng Su, Yuming Wang, Tielong Zhang, Zhiyong Wu, Long Cheng, Zhuxuan Zou, Chenglong Shen, Jingnan Guo, Sudong Xiao, Guoqiang Wang, Zonghao Pan, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Yutian Chi, Mengjiao Xu
Figure caption: The same format as Figure 2, except for MAVEN with two bow-shock crossing points over a longer time period.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Examples of galaxies dominated by long, often continuous SFHs extending back to z = 11–12, either level or declining. There are several cases of order-of-magnitude changes in stellar mass added (more or less), but most of the data are consistent smooth SFHs. These are not the most common SFHs in our sample; galaxy 4144, not shown, is the only additional example. Panels, lines, and symbols are the same as in Figure 1.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Example of the main output of the SEDz* code run on galaxy 1423, which has an S/N of 5.1. The three panels show the observed SED from the seven-band NIRCam imaging and NNLS fit (middle), the run of ﹩{\tilde{\chi }}^{2}﹩ for the fit (left), and the SFH corresponding to the best fit (right). In the middle panel, the SEDz* fit is the magenta band, showing the “quartile range” of 21 trials, with observed fluxes perturbed by 1σ random errors. The positions of prominent emission lines are indicated in blue labels above the SED, with a larger green font marking a possible detection by excess compared to the best fit. (C IV is highlighted here, though its detection is marginal.) The dashed purple line and green dotted line show NNLS fits at z + 2 and z − 2, respectively, which are the values straddling the dip in ﹩{\tilde{\chi }}^{2}﹩ seen in the left panel. In the inset, the color composite image of the galaxy, based on the long-wavelength camera (B = F277W, G = F356W, R = F444W), is shown. The RGB image is 3″ on a side. Left: run of ﹩{\tilde{\chi }}^{2}﹩ for the SEDz* fit, with the primary minimum and a secondary minimum, if detected, marked by magenta and black triangles, respectively. The preferred redshift, marked with a green star, corresponds to the prominent drop in ﹩{\tilde{\chi }}^{2}﹩ at z ∼ 7. Right: SFH for this NNLS solution. Green boxes mark the mass contributed at each epoch. The bars are quartile errors in mass that arise from the random flux errors of the 21 models. Systematic errors in general should be comparable in magnitude to random errors and unlikely to significantly change the SED shape and, with it, the SFH (see text). The red dot in the blue circle marks the mass accumulated through the OE.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Examples of galaxies characterized by the most common type of SFHs found in this early study: runs of star formation over three contiguous epochs. This might be how the most common M* galaxies are born and grow. Panels, lines, and symbols are the same as in Figure 1.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Examples of galaxies characterized by bursty or widely separated episodes of star formation. The star formation episodes of the top two appear to be single bursts of ∼5 × 109 M ⊙; five others of the 33 galaxy sample resemble these. Further examples appear to be multiple bursts that could be associated (see text). Panels, lines, and symbols are the same as in Figure 1.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Color composite image based on the long-wavelength camera (B = F277W, G = F356W, R = F444W) for the 33 galaxies discussed in detail in this paper. Individual images are degraded to the lower resolution of F444W. Postage stamps are 3″ on a side. Pixels are 63 mas. The letter next to ID identifies the main characteristic of the SFH: S = short, L = long, and B = bursty.
Paper: The Empirical Limits of Gyrochronology
Authors: Luke G. Bouma, Elsa K. Palumbo, Lynne A. Hillenbrand
Figure caption: Open cluster data and models. The top panel shows the data that we aim to model, and the bottom panel focuses on the first gigayear. Gray lines in the top panel show the mean model for the rotation period distribution and are uniformly spaced at integer multiples of 100 Myr. They are evaluated using a seventh-order polynomial for each cluster (colored lines, bottom panel) and interpolated piecewise between those reference loci. The model is defined over temperatures of 3800–6200 K and ages of 0.08–2.6 Gyr. Data behind the figure are available as a machine-readable table.(The data used to create this figure are available.)
Paper: The Empirical Limits of Gyrochronology
Authors: Luke G. Bouma, Elsa K. Palumbo, Lynne A. Hillenbrand
Figure caption: Data, model, and goodness of fit. Top: Cluster rotation periods, minus the corresponding slow-sequence mean model at each cluster’s age. The lower gray envelope corresponds to a zero-day rotation period. Middle: Probabilistic model for rotation period as a function of age and temperature (Equation (5)), fitted to the 120 Myr, 300 Myr, and 670 Myr clusters. Bottom: Fraction of stars in 350 K bins that rotate “fast,” as a function of temperature. “Fast” and “slow” stars are squares and circles on the top panel; “very slow” outliers are the crosses. “Slow” stars show a uniform scatter of σ ≈0.51 days around the mean model at t ≥ 120 Myr. The assumed uncertainties for Praesepe are smaller than the markers (see Section 3.5).
Paper: The Empirical Limits of Gyrochronology
Authors: Luke G. Bouma, Elsa K. Palumbo, Lynne A. Hillenbrand
Figure caption: Different approaches for interpolating between reference clusters. P rot denotes the rotation period of the star if it were evolving exactly along the slow sequence. The top two and bottom two rows show identical data, but are scaled logarithmically and linearly in time. The “residual” is defined vs. the pchip_m67 interpolation method, calculated for each model i as (P rot,i − P rot,pchip_m67)/P rot,i. The “+” data points are evaluated from polynomial fits to the data in Figure 1. The fixed power laws (“skumanich_fix_n_0.XX”) are extrapolated based on the rotation period at 120 Myr. MH08: Mamajek & Hillenbrand (2008). A19: Angus et al. (2019). SL20: Spada & Lanzafame (2020).
Paper: The Empirical Limits of Gyrochronology
Authors: Luke G. Bouma, Elsa K. Palumbo, Lynne A. Hillenbrand
Figure caption: Precision of gyrochronal ages from our method. Top: Age posteriors across rotation–temperature space. In each subplot, each line represents a pair of P rot and T eff, and assumes a precision of 50 K in effective temperature and 1% in rotation period. The solid lines come from the best-fit model in Figure 2. The underplotted dotted lines come from a more rigorous approach that samples over the population-level hyperparameters discussed in Section 3.6. Bottom: +1σ (left) and −1σ uncertainty (right) of the age posterior, normalized by the median value. For instance, “±1σ  t /median(t) = 0.3” corresponds to 30% relative precision. Thick gray lines are at integer multiples of 500 Myr, and dotted lines are spaced every 100 Myr; labels are in units of gigayears.
Paper: The Empirical Limits of Gyrochronology
Authors: Luke G. Bouma, Elsa K. Palumbo, Lynne A. Hillenbrand
Figure caption: What if we loosened the quality cuts? This plot is the same as Figure 2, but systems that are known or suspected to be visual, photometric, astrometric, and spectroscopic binaries are now displayed along with the single stars. The model is the same as in Figure 2, as is the panel ordering.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Twenty-eight out of 50 simulations of bursts at 108.5 and 109.5 M ⊙; redshifts of z = 8, 9, 10, 11, or 12; and observed at z = 5, 6, or 7. For each pair, the SEDz* plot of the burst epoch (top) is compared to the OE (bottom). The SFH of the burst is usually resolved as one or two epochs at the burst redshift, and this commonly spreads to an unresolved three or four epochs around the burst redshift when viewed later, at OE. However, six of the 28 examples (enclosed in blue boxes) do show histories that appear to continue down almost to OE, presenting the appearance of a long SFH. But, in contrast to the observed long SFHs of Figure 3, a burst SED seen at OE is always red; it is an old stellar population lacking later star formation to moderate its color (see Figure 9). (Note that in the “simulation” plots, total mass is marked by a green dot with a red ring.)
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Left: six best examples of simulated higher-redshift bursts that might be mistaken for longer SFHs. (Total mass is marked by a green dot with a red ring.) Right: six observed examples from Figure 3, for comparison. (Total mass is a red dot with a blue ring.) In addition to being a small fraction of the burst simulations, the impersonators are distinguishable by their flat starts/steep falloffs in star formation, in contrast to the steady declines seen in the observed sample, and their steeper SEDs, which come naturally from the domination of older stellar populations.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: “Growth history” of three of the eight galaxies in Figure 3, showing a long, mostly continuous star formation from z = 12. These three—GLASS-5429, GLASS-3665, and GLASS-3459—are representative of all eight. We plot the operation of SEDz* epoch by epoch to show how contributions from each stellar population are calculated by NNLS, combining stellar population templates and steadily improving ﹩{\tilde{\chi }}^{2}﹩ from the poor fit of the observed SED using star formation only from the earliest epochs (starting at the bottom with z = 11) to the excellent fit of the SED at the top of each of the three columns (OE). Panels are labeled by galaxy number + epoch; for example, “G366508” is the best-fit SED produced by adding stellar templates up from z = 12 to 8. The red ring in each ﹩{\tilde{\chi }}^{2}﹩ plot denotes the epoch of that frame. For GLASS-5429, the minimum ﹩{\tilde{\chi }}^{2}﹩ = 0.8 is reached at an OE of z = 5.
Paper: Early Results from GLASS-JWST. XVII. Building the First Galaxies—Chapter 1. Star Formation Histories for 5 < z < 7 Galaxies
Authors: Alan Dressler, Benedetta Vulcani, Tommaso Treu, Marcia Rieke, Chris Burns, Antonello Calabrò, Andrea Bonchi, Marco Castellano, Adriano Fontana, Nicha Leethochawalit, Charlotte Mason, Emiliano Merlin, Takahiro Morishita, Diego Paris, Marusa Bradac, Amata Mercurio, Themiya Nanayakkara, Bianca M. Poggianti, Paola Santini, Xin Wang, Karl Misselt, Daniel P. Stark, Christopher Willmer
Figure caption: Validation of the SEDz* code through simulations. Each panel shows a different input SFH (dark blue dots) and how the code retrieves it (green squares) through SED fitting. Red dots show the integrated mass at each step, with a green dot with a red ring marking the total mass. Details of the characteristics of the different input SFHs are given in Appendix A.
Paper: The Image of the M87 Black Hole Reconstructed with PRIMO
Authors: Lia Medeiros, Dimitrios Psaltis, Tod R. Lauer, Feryal Özel
Figure caption: Comparison of the visibility-amplitude (top) and closure-phase (bottom) data to the highest-posterior image reconstruction. The theoretical errors are shown as error bars on the PRIMO reconstruction. Very little structure is seen in the residuals of both the amplitude and closure-phase plots.
Paper: The Image of the M87 Black Hole Reconstructed with PRIMO
Authors: Lia Medeiros, Dimitrios Psaltis, Tod R. Lauer, Feryal Özel
Figure caption: (Top) Comparisons of highest-posterior PRIMO images with total flux equal to 0.5, 0.6, and 0.7 Jy. (Middle) Comparisons of the highest-posterior images using only 12, 14, and 18 PCA components. The morphology of the image is robust to changes in total flux and the number of PCA components. (Bottom) Example images randomly drawn from the MCMC steps of the fiducial chains with flux of 0.6 Jy and 20 PCA components. All three example images have posteriors that are in the 50th percentile.
Paper: The Image of the M87 Black Hole Reconstructed with PRIMO
Authors: Lia Medeiros, Dimitrios Psaltis, Tod R. Lauer, Feryal Özel
Figure caption: (Left) EHT image of the black hole in the center of M87 based on 2017 data, as reported in Event Horizon Telescope Collaboration et al. (2019a). (Middle) Result of reconstructing the image by applying PRIMO to the same data set. (Right) The PRIMO image blurred to the resolution of the EHT array. The diameter of the ring of emission, the north–south brightness asymmetry, and the central brightness depression are present in all images. The PRIMO image offers a superior utilization of the resolution and dynamical range of the EHT array.
Paper: The Image of the M87 Black Hole Reconstructed with PRIMO
Authors: Lia Medeiros, Dimitrios Psaltis, Tod R. Lauer, Feryal Özel
Figure caption: Violin plot comparing the posterior (left half of the violins) of the amplitudes of PCA components 2, 6, 10, 14, and 18 to their priors (right half of the violins). The posterior distributions of the low-order components are thinner than the priors, indicating that their PCA amplitudes are well constrained by the data.
Paper: The Image of the M87 Black Hole Reconstructed with PRIMO
Authors: Lia Medeiros, Dimitrios Psaltis, Tod R. Lauer, Feryal Özel
Figure caption: Comparisons of reconstructed images based on the EHT data obtained on 2017 April 5, 6, 10, and 11. All reconstructions were performed with 20 PCA components and a compact flux of 0.6 Jy. The diameters and widths of the images are consistent across the duration of the 2017 observing campaign, which spans approximately one dynamical timescale for phenomena near the horizon of the M87 black hole.
Paper: Information Horizon of Solar Active Regions
Authors: Jay R. Johnson, Simon Wing, Carson O'ffill, Bishwa Neupane
Figure caption: (a) The image entropy of normalized Carrington map image (blue) and the sunspot number (red) as a function of Carrington number and Gregorian year. (b) The autocorrelation of the image entropy as a function of the lag time in Carrington rotation. The autocorrelation peaks at about 1, 2, and 3 solar cycle timescale. (c) Hilbert–Huang transform showing the frequencies of the dominant intrinsic mode functions as a function of Gregorian year and time since 1974. Note the strong mode at the frequency of the solar cycle, f/f  s  = 1 (f  s  = 140 Carrington rotations) and a weaker mode at half the frequency, f/f  s  = 0.5 (or 2 solar cycles).
Paper: Information Horizon of Solar Active Regions
Authors: Jay R. Johnson, Simon Wing, Carson O'ffill, Bishwa Neupane
Figure caption: An entropy filter is applied to original Carrington map image (a) to identify active region structures, which show up as regions with high entropies (b). Image (d) is obtained by multiplying the image mask (c), constructed from thresholding image (b), with the original image (a). This procedure effectively identifies and partitions the active regions in image (a). The partitions are bounded by the red rectangles in image (d).
Paper: Information Horizon of Solar Active Regions
Authors: Jay R. Johnson, Simon Wing, Carson O'ffill, Bishwa Neupane
Figure caption: Ensemble average of the mutual information of a sequence of images: MI(c(t), c(t + τ)) where c(t) is the Carrington image at time t and τ is the lag time. The MI peaks at τ ∼140 × n where n = integer. In other words, MI peaks at every integer multiplication of a solar cycle period.
Paper: Information Horizon of Solar Active Regions
Authors: Jay R. Johnson, Simon Wing, Carson O'ffill, Bishwa Neupane
Figure caption: Mutual information as a function of neighborhood averaging filter size and τ. The maximum mutual information is found for filter with 32–64 square pixels (118 × 103–236 × 103 Mm2), suggesting approximately the average scale of the active region structures.
Paper: Information Horizon of Solar Active Regions
Authors: Jay R. Johnson, Simon Wing, Carson O'ffill, Bishwa Neupane
Figure caption: Conditional mutual information between Carrington maps at look ahead τ and look behind Δ. Enhancement in the CMI are at τ = Δ = 140, where the dashed gray lines intersect, suggests a long-term memory of two solar cycles in duration.
Paper: The Game of Life on a Magnetar Crust: From Gamma-Ray Flares to FRBs
Authors: S. K. Lander
Figure caption: Number of bursts N(E burst) with energy E burst over a 1000 yr simulation, in ﹩\mathrm{log}({E}_{\mathrm{burst}})=0.5﹩ bins, compared with a power-law relation of Γ = 1.6 (the line shown). Fixing a temperature T amb,9 = 0.5, we explore the effect of cell size. Results for resolutions 14 × 56 (fiducial), 10 × 40, 20 × 80, and 44 × 176 are indicated with the circle, square, triangle, and cross points, respectively.
Paper: The Game of Life on a Magnetar Crust: From Gamma-Ray Flares to FRBs
Authors: S. K. Lander
Figure caption: First 1000 yr of evolution, for T amb,9 = 0.1. E corona is the total twist energy of all coronal loops.
Paper: The Game of Life on a Magnetar Crust: From Gamma-Ray Flares to FRBs
Authors: S. K. Lander
Figure caption: Snapshots of τ/τ el (colorscale) across the northern hemisphere, just before (top) and after (middle) the first “giant flare,” of 2 × 1045 erg, shown in the previous figure. τ/τ el at 1000 yr (bottom) is also shown.
Paper: The Game of Life on a Magnetar Crust: From Gamma-Ray Flares to FRBs
Authors: S. K. Lander
Figure caption: The magnetar crust as an array of cells. The left-hand bunch of coronal field lines are untwisted, embedded in a static cell in its elastic phase. The right-hand bunch are braided by a plastic flow  v  pl circulating around a cell whose elastic yield stress has been exceeded.
Paper: The Game of Life on a Magnetar Crust: From Gamma-Ray Flares to FRBs
Authors: S. K. Lander
Figure caption: Number N of quiescent periods of duration t  q  for two typical 1000 yr evolutions, at T amb,9 = 0.05 (solid bars) and T amb,9 = 0.5 (dashed bars).