adsabs/AstroCLIMB huggingface dataset:
Paper: Electrostatic Wave Decay in the Randomly Inhomogeneous Solar Wind
Authors: C. Krafft, P. Savoini
Figure caption: Homogeneous plasma with T  e /T  i  = 10. (a) Cross-bicoherence b  c  of the triplet (δ n  i , E  x , E  y ) in the plane (ω 1/ω  p , ω 2/ω  p ), in logarithmic scales; the maximum is b  c (ω 1, ω 2) = 0.5, at ω 1/ω  p  = 0.006 and ω 2/ω  p  = 1.014. (b) Cross-bicoherence b  c  of the triplet (δ n  i , E  x , E  y ) in the plane (k  x1 λ  D , k  x2 λ  D ); the maximum is b  c (k  x1, k  x2) = 0.86, at k  x1 λ  D  = 0.225 and k  x2 λ  D  = –0.096. (c) Time variations of energies of Langmuir waves ﹩{ \mathcal L }﹩ and ﹩{{ \mathcal L }}^{{\prime} }﹩ (black and blue) and ion acoustic modes ﹩{{ \mathcal S }}^{{\prime} }﹩ (red), as well as of the energy products ﹩{W}_{{ \mathcal L }}{W}_{{{ \mathcal L }}^{{\prime} }}﹩ (dotted pink, ﹩{ \mathcal L }\,* \,{{ \mathcal L }}^{{\prime} }﹩) and ﹩{W}_{{ \mathcal L }}{W}_{{{ \mathcal S }}^{{\prime} }}﹩ (dotted light blue, ﹩{ \mathcal L }\,* \,{{ \mathcal S }}^{{\prime} }﹩). (d) Time variations of energies of Langmuir waves ﹩{{ \mathcal L }}^{{\prime} }﹩ and ﹩{{ \mathcal L }}^{{\prime\prime} }﹩ (black and blue) and ion acoustic modes ﹩{{ \mathcal S }}^{{\prime\prime} }﹩ (red), as well as of the energy products ﹩{W}_{{{ \mathcal L }}^{{\prime\prime} }}{W}_{{{ \mathcal S }}^{{\prime\prime} }}﹩ (dotted green, ﹩{{ \mathcal L }}^{{\prime\prime} }\,* \,{{ \mathcal S }}^{{\prime\prime} }﹩) and ﹩{W}_{{{ \mathcal L }}^{{\prime\prime} }}{W}_{{{ \mathcal L }}^{{\prime} }}﹩ (dotted pink, ﹩{{ \mathcal L }}^{{\prime\prime} }\,* \,{{ \mathcal L }}^{{\prime} }﹩). (c)–(d) Energies, in logarithmic scales, are integrated on the 2D simulation box and normalized by the initial beam energy. All variables are dimensionless.
Paper: Electrostatic Wave Decay in the Randomly Inhomogeneous Solar Wind
Authors: C. Krafft, P. Savoini
Figure caption: (For a better representation of (h) and (i), please zoom or print.) Randomly inhomogeneous plasma with ΔN > 0 and T  e /T  i  = 10. (a), (c) Energy spectra of ion acoustic waves ﹩{{ \mathcal S }}^{{\prime} }﹩ and ﹩{{ \mathcal S }}^{{\prime\prime} }﹩ in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 2500 and 4500. (b), (d) Dispersion curves, at the same times, in the plane (ω/ω  p , k  x  λ  D ); the black dashed lines represent the theoretical dispersion law; ΔN = 0.05. (e) Variations with time of Langmuir and ion acoustic wave energies (integrated on the 2D simulation box and normalized by the initial beam energy), for ΔN = 0.05 (solid lines) and ΔN = 0.025 (dashed lines), in logarithmic scale. ﹩{ \mathcal L }﹩ : black; ﹩{{ \mathcal L }}^{{\prime} }﹩ : blue; ﹩{{ \mathcal S }}^{{\prime} }﹩, ﹩{{ \mathcal S }}^{{\prime\prime} }﹩: red. (f), (g) Ion acoustic energy spectra in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 1500 and 11,500, for ΔN = 0.025. (h) Time evolution (1300 ≲ ω  p  t ≲ 3970) of profiles along x of the parallel electric field E  x . (i) Corresponding profiles of δ n  i /n 0, in the same time interval as (h); ion acoustic waves propagate in the forward and backward directions (oblique lines with slopes c  s /v  T  and −c  s /v  T ). All variables are normalized.
Paper: Electrostatic Wave Decay in the Randomly Inhomogeneous Solar Wind
Authors: C. Krafft, P. Savoini
Figure caption: Homogeneous plasma with T  e /T  i  = 10. (a) Time variations of energies (integrated on the 2D simulation box and normalized by the beam initial energy) of Langmuir waves ﹩{ \mathcal L }﹩, ﹩{{ \mathcal L }}^{{\prime} }﹩, and ﹩{{ \mathcal L }}^{{\prime\prime} }﹩, and ion acoustic waves ﹩{{ \mathcal S }}^{{\prime} }﹩ and ﹩{{ \mathcal S }}^{{\prime\prime} }﹩, in logarithmic scale. (b) Langmuir wave energy spectrum in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 4500, in logarithmic scale. (c) Space distribution of δ n  i /n 0, at ω  p  t = 4500, in the plane (x/λ  D , y/λ  D ). (d) Spatiotemporal variation of the cross-distribution along x (at fixed y) of δ n  i /n 0, with descending and ascending lines exhibiting the propagation of waves ﹩{{ \mathcal S }}^{{\prime} }﹩ and ﹩{{ \mathcal S }}^{{\prime\prime} }﹩, with group velocities −c  s /v  T  and c  s /v  T . All variables are normalized.
Paper: Electrostatic Wave Decay in the Randomly Inhomogeneous Solar Wind
Authors: C. Krafft, P. Savoini
Figure caption: (a) Space distribution of δ n  i /n 0, at ω  p  t = 4500, for a homogeneous plasma with T  e /T  i  = 1. (b)–(c) Ion acoustic quasi-modes’ ﹩{{ \mathcal S }}_{{qm}}^{{\prime} }﹩ and ﹩{{ \mathcal S }}_{{qm}}^{{\prime\prime} }﹩ energy spectra in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 2500 and 4500, for ΔN = 0 and T  e /T  i  = 1, in logarithmic scales. (d)–(e) Dispersion curves corresponding to (b)–(c). (f) Time variations of energies (integrated on the 2D simulation box and normalized by the initial beam energy) of Langmuir waves ﹩{ \mathcal L }﹩, ﹩{{ \mathcal L }}^{{\prime} }﹩, and ﹩{{ \mathcal L }}^{{\prime\prime} }﹩ (black) and ion acoustic quasi-modes ﹩{{ \mathcal S }}_{{qm}}^{{\prime} }﹩ and ﹩{{ \mathcal S }}_{{qm}}^{{\prime\prime} }﹩ (solid red), in logarithmic scale, for ΔN = 0 and T  e /T  i  = 1; for comparison, the dashed red line is the energy variation of the ﹩{{ \mathcal S }}^{{\prime} }﹩ mode for ΔN = 0 and T  e /T  i  = 10. (g)–(i) Ion acoustic quasi-modes’ energy spectra in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 1500, 2500, and 4500, for ΔN = 0.05 and T  e /T  i  = 1. All variables are normalized.
Paper: Electrostatic Wave Decay in the Randomly Inhomogeneous Solar Wind
Authors: C. Krafft, P. Savoini
Figure caption: Homogeneous plasma with T  e /T  i  = 10. (Left column) Ion acoustic energy spectra in the plane (k  x  λ  D , k  y  λ  D ), at ω  p  t = 1500, 2500, and 4500, in logarithmic scale. (Right column) Ion acoustic dispersion curves, at the same times, in the plane (ω/ω  p , k  x  λ  D ); the black dashed lines represent the theoretical dispersion law. All variables are normalized. Labels indicate the ion acoustic waves ﹩{{ \mathcal S }}^{{\prime} }﹩ and ﹩{{ \mathcal S }}^{{\prime\prime} }﹩.
Paper: Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum
Authors: Zheyi Ding, Gang Li, Nicolas Wijsen, Stefaan Poedts, Shuo Yao
Figure caption: The normalized time-integrated ion spectra for an observer at 1 au. The left and right panels represent the case without and with perpendicular diffusion , respectively. In the left main panel β = − 5/3, and in the inset β = −2; in the right main panel ϵ ⊥ = 1/9, and in the inset ϵ ⊥ = 0. The dash lines show the fitted spectra. See the text for details.
Paper: Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum
Authors: Zheyi Ding, Gang Li, Nicolas Wijsen, Stefaan Poedts, Shuo Yao
Figure caption: The left and right panels show from top to bottom: solar wind speed, solar wind number density, the spectrogram of normalized energetic ion flux intensities vs. energy and time (proton, helium, oxygen, iron) for an observer at 1 au. Left (right) panels are for the case without (with) perpendicular diffusion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Relations between 56Ni (in M ⊙) and explosion energy (in bethe), with the range in the former indicated for some models that have yet to completely asymptote. The triangles are for the exploding black hole formers, yet they still follow the nearly monotonic curve. The right panel includes the data of Rodríguez et al. (2023) and suggests by the overlap of the two a reasonable concordance. Similar observational correlations are found in Müller et al. (2017) and Pejcha (2020).
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Ejecta morphology of the 9(a), 9(b), 9.25, 9.5, 11, 15.01, 16, 17, and 18 M ⊙ models. For most models, the snapshot is taken at the end of the simulation. The 10% 56Ni isosurface is shown, colored by the Mach number of the radial velocity. Red means positive Mach number (outflow), while blue means negative Mach number (inflow). The light-blue envelope shows the shock position. The shock is rendered as a bluish bounding veil. Unbound 16O is distributed between the nickel isosurface and the shock. The only difference between models 9(a) and 9(b) is the imposition of slight velocity perturbations upon infall in the former (Wang & Burrows 2023).
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Left: relation between the final-state neutron star gravitational mass and both the compactness parameter (filled symbol) and the initial central density (open symbol). Right: relation between the final-state neutron star gravitational mass and the Si/O interface mass. The approximately monotonic behavior of the neutron star mass with all three of these quantities is a robust prediction of the theory. We note that Nakamura et al. (2015) derived a similar correlation between neutron star mass and compactness but calculated in 2D, used the all-too-approximate “IDSA” neutrino scheme, and did not calculate beyond ∼1 s after bounce. A related set of correlations was anticipated by Ertl et al. (2016).
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Ejecta Y  e  distributions for our exploding models. Most of the ejecta are at Y  e  = 0.5 or higher, in the proton-rich regime. However, a few of the models, in particular the 9(a) M ⊙ model that boasted imposed initial perturbations in the progenitor, have an interesting neutron-rich tail. Such a tail can give rise to the first peak on the r-process (see Wang & Burrows 2023, 2024).
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Relation between explosion energy and (1) the ejecta mass dipole (left) and (2) explosion energy dipole (right) for the exploding models in this compilation. The mass and energy dipoles are the amplitudes of the l = 1 spherical harmonic components of their angular distributions. The roughly monotonic behavior of these indices of asymmetry with explosion energy is a prediction of the neutrino-driven model of CCSNe.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The explosion energy vs. the cold, catalyzed neutron star gravitational mass. The range for some models reflects the remaining uncertainty of the final-state energies. The monotonic, roughly linear relationship emerges as one of the most interesting predictions of the neutrino-driven core-collapse model of SN explosions. See Section 5.2 for a discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The relation between explosion energy and binding energy exterior to 2.0 M ⊙ (left) and to the compactness (right). The connection between binding energy and explosion energy is physically one of the most important findings from the theoretical perspective. The only major outlier is the 19.56 M ⊙ exploding black hole former. See text in Section 5.2 for a discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Same as Figure 8, but for the 18.5, 19, 19.56, 20, 23, 24, 25, 40, and 60 M ⊙ models.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The relationship between the ejected 56Ni mass and (1) the log10 of the ZAMS mass (left) and (2) the compactness parameter (right). See text in Section 5.3 for a discussion.
Paper: The Geochemical Potential for Metabolic Processes on the Sub-Neptune Exoplanet K2-18b
Authors: Christopher R. Glein
Figure caption: Amount of Gibbs energy that could be harnessed by synthesizing CH4 from CO2 and H2 at the surface of an ocean on exoplanet K2-18b. The unknown atmospheric pressure is a key driver on hycean worlds. Solid vs. dashed curves show how changing the temperature from 25°C to 120°C also affects energy availability. Dashed curves start at 3 bars to make sure the system is on the liquid side of the saturation curve of water. A nominal case with 1% mixing ratios of CO2 and CH4 is indicated by the black curve. Colored curves represent cases where the abundances of CO2 and CH4 are at their 1σ limits in ways that maximize (high CO2/low CH4) or minimize (low CO2/high CH4) the affinity. Equilibrium corresponds to zero affinity. The estimated affinity range for Enceladus’s subsurface ocean (Waite et al. 2017) and a canonical value for the minimum affinity needed to support methanogenic life on Earth (Hoehler 2004) are shown for comparison.
Paper: The Geochemical Potential for Metabolic Processes on the Sub-Neptune Exoplanet K2-18b
Authors: Christopher R. Glein
Figure caption: Amount of Gibbs energy it costs (negative affinities) or can pay (positive affinities) to synthesize the amino acids (a) glycine and (b) alanine from CO2, NH3, and H2 at the surface of an ocean on exoplanet K2-18b. The unknown atmospheric pressure is a key driver on hycean worlds. Solid vs. dashed curves show how changing the temperature from 25°C to 120°C also affects the energetic state of these reactions. Dashed curves start at 3 bars to make sure the system is on the liquid side of the saturation curve of water. Colored curves represent cases with the indicated dry mixing ratio of NH3. Equilibrium corresponds to zero affinity. Affinities in terrestrial seawater and mixed fluids at the Lost City Hydrothermal Field are shown for comparison. Note that the ordinate axis has a break in both plots.
Paper: The Geochemical Potential for Metabolic Processes on the Sub-Neptune Exoplanet K2-18b
Authors: Christopher R. Glein
Figure caption: How chemical affinities of two amino acid synthesis reactions (see Equations (10) and (11)) evolve as a Lost City hydrothermal endmember fluid (116°C) mixes with surrounding seawater (8°C). Equilibrium corresponds to zero affinity. The reaction path calculations predict that brucite and aragonite should precipitate above ∼81°C, whereas the fluid mixture is saturated in only aragonite at lower temperatures.
Paper: Effects of Type Ia Supernovae Absolute Magnitude Priors on the Hubble Constant Value
Authors: Yun Chen, Suresh Kumar, Bharat Ratra, Tengpeng Xu
Figure caption: The observational constraints on Ωm0 and H 0. Panel (a) displays the mean values of Ωm0 and H 0, and panels (b)–(f) show the mean parameter values and 68% confidence level errors obtained for each of the five different priors of M. H 0 has units of km s−1 Mpc−1.
Paper: Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum
Authors: Zheyi Ding, Gang Li, Nicolas Wijsen, Stefaan Poedts, Shuo Yao
Figure caption: The solar wind radial speed and the assumed parallel and perpendicular mean free paths for 50 keV protons in the solar equatorial plane. Panel (a) shows the radial solar wind speed. White dashed lines are magnetic field lines from the simulation. Panel (b) shows the divergence of the solar wind velocity. The compression waves can be recognized as the colorful spiral-shaped structures. Panels (c) and (d) show, respectively, the parallel and perpendicular mean free paths for 50 keV protons. The simulation domain is from r = 0.1 au to r = 5 au.
Paper: Modeling Ion Acceleration and Transport in Corotating Interaction Regions: The Mass-to-charge Ratio Dependence of the Particle Spectrum
Authors: Zheyi Ding, Gang Li, Nicolas Wijsen, Stefaan Poedts, Shuo Yao
Figure caption: The divergence of the solar wind velocity ∇ ·  V  sw and the shock obliquity θ BN as a function of radial distance along the CIR reverse shock.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Relations between the neutron star kick speed and the ejecta energy dipole (left) and the quantity ﹩{\left(\tfrac{{E}_{\exp }}{{M}_{\mathrm{bar}}}\right)}^{1/2}﹩ (right), where E exp is the explosion energy and M bar is the baryon mass of the neutron star. See Burrows et al. (2023b) for a more thorough discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Relations between the freezeout ejecta mass and the compactness parameter (top left), ejecta mass dipole (top right), and explosion energy (bottom). The reasonably robust correlations between the freezeout mass and both the explosion energy and the ejecta mass dipole are predictions of the theory that can be tested. See the text in Section 5.3 for a discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The temporal evolution of averaged shock radius (top left), PNS baryon mass (top right), the minimum explosion energy (bottom left, in bethe ≡ 1051 erg), and kick speed (bottom right). Before shock revival, we set the “explosion energy” arbitrarily to zero. Upon shock revival, the matter behind the shock is still bound, and early on most of the deposited neutrino energy goes into overcoming this negative gravitational binding energy and the (negative) contribution of the overburden exterior to the simulation grid (which is included in the accounting). This is why the explosion energy starts negative and only gradually grows to become positive over time. See text in Section 3.1 for a discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Relation between the explosion time and compactness parameter for the set of 20 models in this study. Note the roughly monotonic behavior, with lower ZAMS mass and lower-compactness models exploding more quickly, though with some scatter. See the text in Section 3.1 for a discussion.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Progenitor mass density profiles as a function of interior mass coordinate for the 20 models we employ for this 3D SN explosion investigation from the Sukhbold et al. (2016, 2018) collection of unstable massive star cores. The colors correlate with ZAMS mass, and the dashed curves are for models we see leave black holes, either explosively (the 19.56 and 40 M ⊙ models) or quiescently.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: Total stellar mass (left) that remains at collapse and the corresponding C/O and He core masses (right) as a function of the log10 of the ZAMS mass. In the right panel, the filled symbols are the C/O core masses (left label), while the open symbols are the He core masses (right label). The 60 M ⊙ progenitor has the same C/O and He core mass because it has ejected its outer envelope exterior to the C/O core in strong winds. The black circles in both panels are all the models in the Sukhbold et al. (2016, 2018) solar-metallicity set. The triangles are the black hole formers.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The behavior of the explosion energy and final-state neutron star mass with explosion time. For some models that have not quite asymptoted, a range of explosion energies is given, from minimum to projected (likely). Note the roughly monotonic behavior of both the energy and neutron star mass with explosion time. See the discussion in Section 3.1.
Paper: Physical Correlations and Predictions Emerging from Modern Core-collapse Supernova Theory
Authors: Adam Burrows, Tianshu Wang, David Vartanyan
Figure caption: The dependence of the compactness on the log10 of the ZAMS mass (left) and the Si/O interface interior mass (right). The black circles identify the full Sukhbold et al. (2016, 2018) collection of solar-metallicity models, while the colored symbols indicate the models in this study. The colored triangles identify the models that we see form black holes.
Paper: What Powered the Kilonova-like Emission after GRB 230307A in the Framework of a Neutron Star–White Dwarf Merger?
Authors: Xiangyu Ivy Wang, 翔煜 王, Yun-Wei Yu, 云伟 俞, Jia Ren, 佳 任, Jun Yang, 俊 杨, Ze-Cheng Zou, 泽城 邹, Jin-Ping Zhu, 锦平 朱
Figure caption: The multiwavelength light curves. The solid line is the afterglow plus kilonova-like emission, while the dashed line is the afterglow-only emission. Both lines are plotted with the median parameters in our fitting. The data are collected from Yang et al. (2024).
Paper: What Powered the Kilonova-like Emission after GRB 230307A in the Framework of a Neutron Star–White Dwarf Merger?
Authors: Xiangyu Ivy Wang, 翔煜 王, Yun-Wei Yu, 云伟 俞, Jia Ren, 佳 任, Jun Yang, 俊 杨, Ze-Cheng Zou, 泽城 邹, Jin-Ping Zhu, 锦平 朱
Figure caption: The bolometric light curves. The dashed and dotted lines represent the absorbed spin-down energy of the ejecta and the radioactive heating power from 56Ni, respectively. The solid line is the total energy of the two energy sources.
Paper: What Powered the Kilonova-like Emission after GRB 230307A in the Framework of a Neutron Star–White Dwarf Merger?
Authors: Xiangyu Ivy Wang, 翔煜 王, Yun-Wei Yu, 云伟 俞, Jia Ren, 佳 任, Jun Yang, 俊 杨, Ze-Cheng Zou, 泽城 邹, Jin-Ping Zhu, 锦平 朱
Figure caption: The corner plot of the posterior probability distributions of 14 parameters listed in Table 1 for the fitting of the multiwavelength light curves.
Paper: What Powered the Kilonova-like Emission after GRB 230307A in the Framework of a Neutron Star–White Dwarf Merger?
Authors: Xiangyu Ivy Wang, 翔煜 王, Yun-Wei Yu, 云伟 俞, Jia Ren, 佳 任, Jun Yang, 俊 杨, Ze-Cheng Zou, 泽城 邹, Jin-Ping Zhu, 锦平 朱
Figure caption: SEDs. The black points are the unabsorbed spectra at different epochs from Yang et al. (2024). The solid and dashed lines are the afterglow plus kilonova-like emission and afterglow-only emission, respectively.
Paper: Analytic Model and Magnetohydrodynamic Simulations of Three-dimensional Magnetic Switchbacks
Authors: Chen Shi, 辰 时, Marco Velli, Gabor Toth, Kun Zhang, 琨 张, Anna Tenerani, Zesen Huang, 泽森 黄, Nikos Sioulas, Bart van der Holst
Figure caption: Panels (a1)–(c2): snapshots of the x − z plane across the central axis (y = 0) color-coded with ρ 1 for Runs 0 ((a), top), 5 ((b), middle), and 8 ((c), bottom), where ﹩{\rho }_{1}=\rho -\left\langle \rho \right\rangle ﹩ is the density fluctuation. Black curves are magnetic field lines projected on the 2D plane. Panels (d)–(f): linear growth rate (solid) and frequency (dashed) of the PDI for a monochromatic, circularly polarized Alfvén wave with amplitude (d) A = 0.1, (e) A = 1.0, and (f) A = 2.0. In each panel, different curves correspond to different values of ﹩\tilde{\beta }={C}_{s}^{2}/{V}_{A}^{2}﹩, where C  s  and V  A  are the sound speed and Alfvén speed of the background field. ω 0 and k 0 are the frequency and wavenumber of the mother Alfvén wave. A = δ B/B 0 is the amplitude of the mother wave normalized to the background magnetic field.