adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of Giant Bubbles in the Hot Gaseous Halo of the Massive Disk Galaxy NGC 6286
Authors: Lin He, Zhiyuan Li, Zongnan Li, Rubén García-Benito, Yuanqi Liu, Meicun Hou
Figure caption: Instrumental background-subtracted, exposure-corrected radial (left), and vertical (right) X-ray intensity profiles of NGC 6286 in the 0.5–2 keV band, adaptively binned to achieve an S/N greater than 2. The sky-blue and gray lines indicate the level of instrumental background and sky background, respectively. The arrow indicates the position of the companion galaxy NGC 6285. The vertical dashed lines indicate the size of the semimajor axis in the left panel and the semiminor axis in the right panel, respectively. A zoom-in view of the inner 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩4 (1.6 kpc) is shown by the inserts.
Paper: Discovery of Giant Bubbles in the Hot Gaseous Halo of the Massive Disk Galaxy NGC 6286
Authors: Lin He, Zhiyuan Li, Zongnan Li, Rubén García-Benito, Yuanqi Liu, Meicun Hou
Figure caption: Left: 0.5–8 keV counts image centered on NGC 6286. The white ellipse and boxes demarcate the disk and bubble emission, respectively, while the two green ellipses are used to outline the shells of the putative bipolar bubbles. Right: Observed X-ray spectrum of the bubbles, adaptively binned to achieve an S/N ratio of 2 per bin. The best-fit model (black solid line), TBabs × APEC, represents the shells dominating the observed soft X-ray emission. The lower panel plots the relative residual. A putative hot wind component, i.e., a second APEC with a fixed temperature of kT =  5 keV, is also plotted (blue dash line) for illustration.
Paper: Discovery of Giant Bubbles in the Hot Gaseous Halo of the Massive Disk Galaxy NGC 6286
Authors: Lin He, Zhiyuan Li, Zongnan Li, Rubén García-Benito, Yuanqi Liu, Meicun Hou
Figure caption: Observed line-of-sight velocity field of the Hα gas (left), a fitted pure rotating-disk model (middle), and the residuals (right). The black contours are the same as those in Figure 1.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Distribution of neutral hydrogen column density (NHI) for the simulated halo with 3 × 1011M⊙ at z ≈ 2 from the runs without and with CRs (top and middle panel, respectively). The dashed circles denote 0.5 Rvir, where Rvir is the virial radius of the dark matter halo (≈72 kpc). The neutral hydrogen fraction is recomputed by postprocessing each snapshot with RAMSES-RT. The bottom panel shows the azimuthally averaged NHI profile. The galaxy simulated with CR feedback clearly has a more extended H I distribution than the one without, even though the total H I mass is smaller.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Comparison of the UV magnitudes at 1500 Å (M1500) and Lyα properties of a simulated galaxy with observations. Black symbols indicate the observed samples of LAEs at various redshifts (T. Hashimoto et al. 2017; F. Leclercq et al. 2017; Y. I. Izotov et al. 2018a; J. Matthee et al. 2021), as indicated in the legend. Blue circles and red pentagons indicate simulated UV and Lyα from our simulations without and with CR feedback, respectively. Both quantities are dust-attenuated. Each data point represents a different sightline and snapshot between 2 ≤ z ≤ 4. Intergalactic medium (IGM) attenuation, which lowers the Lyα luminosities by ∼15%, is not included in this figure.
Paper: Magnetic Reconnection as a Potential Driver of X-Ray Variability in Active Galactic Nuclei
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄, Lang Cui, 朗 崔, Hanle Zhang, 晗乐 张, Jiang-Tao Li, 江涛 李, Li Ji, 丽 纪, Jin-Jun Geng, 金军 耿, Orkash Amat, 热卡西-艾麦提 吾, Fan Xu, 帆 许, Chen Du, 琛 杜, Wen-Long Zhang, 文龙 张, Ze-Cheng Zou, 泽城 邹, Xiao-Fei Dong, 小飞 董, Chen Deng, 晨 邓, Pengfei Jiang, 鹏飞 蒋, Jie Liao, 杰 廖
Figure caption: Sliding window analyses for the 13 quasars. Each dumbbell-shaped marker represents a temporal window, including 10 temporally adjacent luminosity measures (including upper limits) in the light curve. Different colors correspond to different statistical parameters in the window. The mean luminosity with ±1σ uncertainty is shown in blue. The median luminosity is shown in red. The standard deviation with ±1σ uncertainty is shown by the black dashed line. Gray lines and bands denote the global mean and standard deviation for the whole light curve.
Paper: Magnetic Reconnection as a Potential Driver of X-Ray Variability in Active Galactic Nuclei
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄, Lang Cui, 朗 崔, Hanle Zhang, 晗乐 张, Jiang-Tao Li, 江涛 李, Li Ji, 丽 纪, Jin-Jun Geng, 金军 耿, Orkash Amat, 热卡西-艾麦提 吾, Fan Xu, 帆 许, Chen Du, 琛 杜, Wen-Long Zhang, 文龙 张, Ze-Cheng Zou, 泽城 邹, Xiao-Fei Dong, 小飞 董, Chen Deng, 晨 邓, Pengfei Jiang, 鹏飞 蒋, Jie Liao, 杰 廖
Figure caption: σ–μ relation of high-redshift AGNs. (a) The global means (﹩{\mu }_{{L}_{2-{\rm{10keV}}}}﹩) vs. the global standard deviations (﹩{\sigma }_{{L}_{2-{\rm{10keV}}}}﹩) of rest-frame 2–10 keV luminosity for the 13 quasars. The data points can be well fitted with a linear function (solid line), with the 90% confidence interval illustrated as a shaded region. The solid line has a slope of 0.42. The correlation is strong, which exhibits a Kendall’s τb coefficient of 0.85 and a P-value of 1.3 × 10−5 when tested by using the nonparametric method. (b) The σ–μ relation plotted with the X-ray photon index Γ color-coded and the optical-to-X-ray spectral slope size-scaled. (c) The σ–μ relation plotted with the redshift color-coded and the rest-frame observing span size-scaled.
Paper: Magnetic Reconnection as a Potential Driver of X-Ray Variability in Active Galactic Nuclei
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄, Lang Cui, 朗 崔, Hanle Zhang, 晗乐 张, Jiang-Tao Li, 江涛 李, Li Ji, 丽 纪, Jin-Jun Geng, 金军 耿, Orkash Amat, 热卡西-艾麦提 吾, Fan Xu, 帆 许, Chen Du, 琛 杜, Wen-Long Zhang, 文龙 张, Ze-Cheng Zou, 泽城 邹, Xiao-Fei Dong, 小飞 董, Chen Deng, 晨 邓, Pengfei Jiang, 鹏飞 蒋, Jie Liao, 杰 廖
Figure caption: X-ray light curves of the 13 bright quasars at z > 4.5. The error bars of the observational data points correspond to 1σ uncertainties, while the upper limits are shown at the 3σ confidence level. In each panel, the rectangular inset provides a zoomed-in view of the region bounded by the corresponding line style.
Paper: Magnetic Reconnection as a Potential Driver of X-Ray Variability in Active Galactic Nuclei
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄, Lang Cui, 朗 崔, Hanle Zhang, 晗乐 张, Jiang-Tao Li, 江涛 李, Li Ji, 丽 纪, Jin-Jun Geng, 金军 耿, Orkash Amat, 热卡西-艾麦提 吾, Fan Xu, 帆 许, Chen Du, 琛 杜, Wen-Long Zhang, 文龙 张, Ze-Cheng Zou, 泽城 邹, Xiao-Fei Dong, 小飞 董, Chen Deng, 晨 邓, Pengfei Jiang, 鹏飞 蒋, Jie Liao, 杰 廖
Figure caption: Periodicities of J090630+693030 and J143023+420436. (a) The upper panel shows the Lomb–Scargle periodogram of J090630+693030. The horizontal lines indicate the confidence levels. The lower panel compares the best-fit light curve with the observed data points. (b) The upper panel shows the Lomb–Scargle periodogram of J143023+420436, while the lower panel compares the best-fit light curve with the observed data points.
Paper: Magnetic Reconnection as a Potential Driver of X-Ray Variability in Active Galactic Nuclei
Authors: Chen-Ran Hu, 宸然 胡, Yong-Feng Huang, 永锋 黄, Lang Cui, 朗 崔, Hanle Zhang, 晗乐 张, Jiang-Tao Li, 江涛 李, Li Ji, 丽 纪, Jin-Jun Geng, 金军 耿, Orkash Amat, 热卡西-艾麦提 吾, Fan Xu, 帆 许, Chen Du, 琛 杜, Wen-Long Zhang, 文龙 张, Ze-Cheng Zou, 泽城 邹, Xiao-Fei Dong, 小飞 董, Chen Deng, 晨 邓, Pengfei Jiang, 鹏飞 蒋, Jie Liao, 杰 廖
Figure caption: CDF of rest-frame 2–10 keV luminosity for the 13 quasars in our sample. The luminosity CDF is calculated by using the Kaplan–Meier estimator method, which takes into account the upper-limit data points.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Comparison of the blue-to-red flux ratio of Lyα (B/R) and the location of the red peak (vred) in velocity space in simulations with (CRMHD) and without CRs (MHD). The upper panels show the angle-averaged quantities before (a) and after (b) LyC postprocessing with RAMSES-RT. The filled and empty symbols represent measurements after and without applying the simple IGM attenuation model of A. K. Inoue et al. (2014), respectively. Lyα properties estimated from 1D mock spectra within a 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 aperture are compared in (c). The black symbols correspond to observational data from D. K. Erb et al. (2014), H. Yang et al. (2016), A. Verhamme et al. (2017), I. Orlitová et al. (2018), J. Matthee et al. (2021), A. Runnholm et al. (2021). Panel (d) shows the simulated ratio between the flux in the valley of the two peaks and the maximum of the peaks (fvalley, filled circles). The black diamonds indicate the LASD values obtained using the systematic redshift. For comparison, we also include fvalley values, calculated using Lyα collected within the entire virial sphere (empty circles).
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Upper panel: fractions of collisional radiation to the total emergent, PSF-convolved Lyα SB profiles. Solid and dashed lines show results for different redshift ranges (2 < z < 2.5 and 3 < z < 3.5, respectively). Lower panel: median-stacked SB profiles of galaxies simulated without (MHD, cyan) and with (CRMHD, orange) CR feedback. The median-stacked SB profile of LAEs at z ∼ 3.5, obtained with the MUSE instrument, is included for comparison (thick gray line with shaded regions, L. Wisotzki et al. 2018). We also include the PSF-smoothed intrinsic SB profiles as dotted lines. To correct for the redshift dimming effect, the SB profiles are scaled by a factor of (1 + z)4/(1 + 3)4.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: LyC luminosity-weighted distribution of NHI measured from each star particle over 2 ≤ z ≤ 4. Different color-codes correspond to different simulations, as shown in the legend. Simulations postprocessed with RAMSES-RT are shown as dotted–dashed lines, while those without postprocessing are shown as solid lines.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Predicted Lyα profiles formed by ISM region (r < 0.1 Rvir, green symbols) or by CGM (r > 0.1 Rvir, orange symbols). Note that the source positions are limited to r < 0.1 Rvir for vred,ISM or vred,CGM for easier interpretation. The vred,tot values are the same as the vred values in Figure 5 (left panel) and thus are obtained from all the photons generated within the virial sphere. The location of the red peak from the galaxy (vred) is compared before (squares) and after (triangles) LyC postprocessing with RAMSES-RT.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) Best-fit model-predicted dust impact count rates on PSP for solar encounter 4, for α-meteoroids (green), β-meteoroids (purple), and total impact rate (black). PSP impact rate data are plotted in gray. (b) Model-predicted dust impact direction on the PSP spacecraft, for α-meteoroids (green) and β-meteoroids (purple). (c) Cross-sectional area values for α-meteoroids (green) and β-meteoroids (purple). Spacecraft body values are shown with solid lines, heat shield values are shown with dashed lines. (d) Predicted fraction of impacts that strike the spacecraft body. All quantities are plotted as a function of days from solar encounter 4 perihelion.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Stacked, angle-averaged Lyα profiles from the MHD and CRMHD runs (upper and lower panels, respectively). Profiles are normalized to the maximum flux of the emergent spectrum in the CRMHD run. Intrinsic fluxes are reduced by a factor of two for clarity. The dotted and dashed lines represent the intrinsic Lyα spectrum and results of MCRT calculations on the simulation outputs without LyC postprocessing, respectively. The solid lines indicate the MCRT calculations performed on the postprocessed simulations, which also include the contribution from collisional radiation. Attenuation by the IGM is not included.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Correlation between separation of double peaks in Lyα (vsep) and escape fraction at 900 Å (f900). The black star symbols represent the observed properties of LAE galaxies from A. Verhamme et al. (2017), while the colored points denote the results from simulations (empty: 1D, filled: 3D). The black solid line is the empirical relation from Y. I. Izotov et al. (2018c). For comparison, we include the analytic correlation between vsep and f900 for dust-free uniform media with turbulence velocities of 0 and 100 km s−1 (dotted lines). No clear correlation is found between f900 and vsep at f900  ≲  0.1.
Paper: Impact of Cosmic Ray-driven Outflows on Lyα Emission in Cosmological Simulations
Authors: Taysun Kimm, Julien Devriendt, Francisco Rodríguez Montero, Adrianne Slyz, Jérémy Blaizot, Harley Katz, Beomchan Koh, Hyunmi Song
Figure caption: Example of NHI map before (left) and after (right) the LyC postprocessing.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) Rdata, the ratio of observed dust impacts on the spacecraft body to all detected impacts, as a function of days from perihelion 4. (b) Spacecraft floating potential as a function of days from perihelion 4. For (a) and (b), the black dashed line indicates perihelion. The gray dashed lines indicate specific structures in the spacecraft floating potential that are reflected in Rdata. (c) Scatter plot of Rdata as a function of spacecraft floating potential, with a linear best-fit line included.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) The ratio of observed dust impacts on the spacecraft body to all detected impacts, for observations (Rdata,corr, black) and for the two-component model Rmodel (blue), as a function of days from perihelion 4. (b) Same as (a), focusing on the pre-perihelion enhancement (green shading). The black dashed line indicates the time of perihelion.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) Schematic of geometry used to calculate Dmin. (b) Orbits of PSP and the asteroid 2008 FF5 in three dimensions. Features of the orbits and pre-perihelion body-hit enhancement are indicated. (c) Dmin for 2008 FF5 as a function of time from perihelion 4. The perihelion time is indicated (black dashed line), as well as the time of peak of the pre-perihelion body-hit enhancement (red dashed line). The pre-perihelion enhancement is shaded green, as in Figure 4.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) PSP model used for dust detection cross-sectional area estimates. (b) Silhouette of the PSP model for θimpact = 30° and θflap = 0°. (c) Partitioning of PSP silhouette into spacecraft body (orange) and heat shield (blue) cross-sectional areas. (d) Total cross-sectional area. (e) Heat shield cross-sectional area (f) Spacecraft body cross-sectional area. All areas in (d, e, f) are plotted as a function of θimpact for several values of θflap.
Paper: A Search for Meteoroid Streams and Their Sources in the Near-Sun Zodiacal Dust Cloud
Authors: David M. Malaspina, Jamey R. Szalay, Avery Mazurkiewicz, Delaney Lee-Bellows, Margaret E. Landis
Figure caption: (a) Schematic of geometry used to calculate θβ1 and θimp1. (b) θβ1 as a function of distance to the Sun (Robj) for comet 342P/SOHO. Blue symbols indicate where θimp1 > 45°.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Comparison of the simulations with Te/Ti ≈ 3 and varying values of ωpe/Ωce. Panels (a) to (d) show profiles of the density, magnetic field, normal component of the electric field, and the NIF shock potential, respectively, for the cases with ωpe/Ωce = 8, 16, 32 at tΩci ≈ 3.5.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Energy exchange terms in the simulation with Te/Ti = 3 and ωpe/Ωce = 32: (a) electron density; (b) magnetic field; (c) NIF shock potential; (d) and (e) energy exchange term ﹩{ \mathcal R }={\int }_{{x}_{0}}^{x}({\boldsymbol{E}}\cdot {\boldsymbol{j}})\,dx﹩ for electrons and ions, respectively; (f) and (g) the term ﹩{\rm{\Pi }}={\int }_{{x}_{0}}^{x}({\boldsymbol{p}}\cdot {\rm{\nabla }}{\boldsymbol{U}})\,dx﹩ for for electrons and ions, respectively. For each quantity ﹩A=\{{{ \mathcal R }}_{e},{{ \mathcal R }}_{i},{{\rm{\Pi }}}_{e},{{\rm{\Pi }}}_{i}\}﹩ in panels (c) through (g), the thin color lines show the difference ﹩\delta A=A-\hat{A}﹩, where ﹩\hat{A}﹩ is computed with spatially smoothed quantities, the solid black lines show time average of A, and the dashed lines show the time average of ﹩\hat{A}﹩. Color corresponds to the simulation time as indicated by the color bar. See the text for more details.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: (a) The time-varying longitude-resolved fluctuation spectra (LRFS) estimated on the single-pulse sequence of PSR B1642-03, showing the broad periodic amplitude modulation feature in frequency range 0.05–0.1 cycles P-1. (b) The 0/1 time series FFT is estimated for different cutoff levels, and the signal-to-noise ratio (SNR) of the periodic feature is shown in the top panel. The maximum SNR corresponds to 1.2 times the standard deviation above the median level (dashed red vertical line). The bottom panel shows the average FFT of the 0/1 sequence with the maximum SNR of the periodic feature.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: (a) A short single-pulse sequence of PSR B1642-03 with periodic amplitude modulation. (b) The lower panel shows the average intensity of each pulse estimated within the longitude range specified by the two vertical dashed lines in the left panel. A statistical cutoff level for the two emission states is shown as the red horizontal dashed line, and the upper panel shows the 0/1 time sequence obtained using this cutoff.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: An example of ion phase-space hole in the foot region of the shock: profiles of electron and ion densities (a), electric field (b), potential (c) normalized to Φ0 = Ti/e, as well as ion (d) and electron (e) phase space. The spatial coordinates are normalized to the reference value of the Debye length λe and shifted such that Ex ≈ 0 at x = 0.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Histograms of the electric field fluctuations Ex in the simulations with Te/Ti ≈ 3 (see Figure 1) during the time interval tΩci = (2−3) in the range ﹩{x}^{{\prime} }/{d}_{p}=(3-10)﹩, where ﹩{x}^{{\prime} }﹩ is the coordinate comoving with the shock ﹩{x}^{{\prime} }=x-(t-{t}_{0}){V}_{\mathrm{sh}}﹩ and t0 = 2Ωci. The insert shows time-averaged histograms for each case on the log–log scale.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Variations of the electron density (a), parallel (b), (d), and perpendicular (c), (e) electron kinetic temperatures for electrons and ions for the same simulations and time instance as in Figure 1.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Comparison between two otherwise identical simulations with Te/Ti ≈ 3 and Te/Ti ≈ 1/3. The figure format is the same as in panels (a)–(d) of Figure 1. Slightly different times were used for comparison, since the shock speed differs between the two cases.
Paper: Magnitude of Short-wavelength Electric Field Fluctuations in Simulations of Collisionless Plasma Shocks
Authors: Vadim Roytershteyn, Lynn B. Wilson, Li-Jen Chen, Michael Gedalin, Nikolai Pogorelov
Figure caption: Ion (panel (a)) and electron (panel (b)) phase-space structure, together with the associated profile of the electric field (panel (c)). The black line in panel (b) shows variation of the (scaled) electron density across the transition region.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: Single-pulse sequence showing the nature of the periodic amplitude modulation in each pulsar. The dashed lines show the longitude window within which the average intensities are estimated for the state separation studies.
Paper: Characterizing the Nature of Periodic Amplitude Modulation in Pulsars
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The average profiles of the brighter (black) and weaker (dotted red) intensity states of periodic amplitude modulation. In some cases, scaled-up versions of weaker state profiles are also shown to better highlight the emission features.