adsabs/AstroCLIMB huggingface dataset:
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: High- and low-frequency wave emissions around the 5th perihelion. (a) High-frequency electric field spectrum from AC differential voltage data measured by V 12 and V 34 antennae pairs (same as Figure 2(f)). (b) Low-frequency magnetic field spectrogram from FGM data. (c) Degree of polarization, magnetic field. (d) Ellipticity of the magnetic field waves in the spacecraft frame. Ellipticity is +1 for right-hand and −1 for left-hand polarization. In panels (c) and (d) the gray area corresponds to points where either the degree of polarization is below 0.7 or the wave power is below 1 × 10−3 nT2 Hz−1. In panels (b)–(d) the black line represents the ion gyrofrequency f ci. (e) Magnetic field in RTN coordinates, same as Figure 2(c).
Paper: Parker Solar Probe Observations of Near-f Ce Harmonic Emissions in the Near-Sun Solar Wind and Their Dependence on the Magnetic Field Direction
Authors: Sabrina F. Tigik, Andris Vaivads, David M. Malaspina, Stuart D. Bale
Figure caption: Probability distribution with respect to ϕ   B   for the day around the 5th orbit perihelion. (Red) All data points, (yellow) data points with wave emission power being above (a) ﹩1.0\times {10}^{-4}\,{(\mathrm{mV}\,{{\rm{m}}}^{-1})}^{2}{\mathrm{Hz}}^{-1}﹩ and (b) ﹩2.0\times {10}^{-4}\,{(\mathrm{mV}\,{{\rm{m}}}^{-1})}^{2}{\mathrm{Hz}}^{-1}﹩, and (blue) estimated Parker spiral angle for all data. Each histogram bin corresponds to 1°, and the sum of the bar heights of each quantity in the total angle range (±90°) is ≤1.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: We show the SMHMs at z = 0 of 30 Caterpillar trees from our best model. At given M vir,peak, we show the mean M * (gray circles) and the standard deviation among the galaxies from each tree. We also plot the SMHM derived by Nadler et al. (2020) as a gray contour, where the dark gray shows the 1σ region and the light gray shows the 2σ region. The SMHM derived with the AM technique by Garrison-Kimmel et al. (2014) is plotted with a red curve until the observational completeness.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Volume filling fraction of ionized regions (top) and metal-enriched regions (bottom). We compare three different approaches to model an MW-like galaxy with and without spatial information. The gray lines and symbols are models from the literature (compare Figures 5 and 9). These literature models should only guide the eye since an MW-like volume is not representative and these simulations do not intend to reproduce these literature values. The early peak of ionizing radiation in the EPS-based model is due to a smaller effective volume and due to a higher Pop III SFRD at early times.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Cosmic SFRDs for Pop III stars (top panel) and Pop II stars (bottom panel). The blue lines show our model prediction, the dashed lines show other models from the literature (Trenti & Stiavelli 2009; Johnson et al. 2013; de Souza et al. 2014; Xu et al. 2016a; Jaacks et al. 2018; Mebane et al. 2018; Sarmento et al. 2019; Visbal et al. 2020), the dotted lines in the bottom panel show observations (Madau & Dickinson 2014; Behroozi & Silk 2015; Finkelstein 2016; Behroozi et al. 2019), and the gray dashed–dotted lines in both panels show the total SFRD (Pop II+Pop III).
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Comparison of SFRD (top) and MDF (bottom) between different MW-like simulations. The gray lines are models from the literature (compare Figures 11 and 12). We focus on the difference between our three models, and the SFRD in an MW-like volume should not reproduce the cosmologically representative SFRD. Hence, we do not focus on the comparison to literature here, but rather provide them to guide the eye. The two models that are based on Caterpillar merger trees (blue, orange) provide similar results, whereas the EPS-based model differs at high redshift and low metallicity.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: We compare the MDF produced with the calibrated model and observations of Youakim et al. (2020), Bonifacio et al. (2021), and Chiti et al. (2021). The black lines show model results for all the Caterpillar trees. Other lines show three different observations. The histogram shows the number of stars in each bin. The sum of the histograms at [Fe/H] < −2 is normalized to be 1 for both model results and observations.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: CSMFs at z = 0 extracted from our set of 30 Caterpillar trees, processed using our fiducial model parameters. The CSMFs from our Caterpillar trees are plotted in gray, and the observed CSMF for the MW is plotted in blue. The gray shaded area represents the region in which the observations are known to be incomplete. The observed CSMF in this region is plotted using a dashed line and is not used to calibrate the model.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Best A-SLOTH model (black) compared to two independent observation-based constraints. We incentivize the result to lie between these two constraints and penalize the maximum distance that our modeled cumulative SFRD is outside the green band.
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Example of one QD step. We start at the previous value (vertical dotted line), sample four additional values (blue points), fit a quadratic function (blue line), and choose the maximum value as a new parameter (orange star).
Paper: Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Authors: Tilman Hartwig, Mattis Magg, Li-Hsin Chen, Yuta Tarumi, Volker Bromm, Simon C. O. Glover, Alexander P. Ji, Ralf S. Klessen, Muhammad A. Latif, Marta Volonteri, Naoki Yoshida
Figure caption: Metal-enriched volume fraction simulated with A-SLOTH in the 8 Mpc box (blue solid) compared to other results from the literature (Pallottini et al. 2014; Salvadori et al. 2014; Jaacks et al. 2018; Visbal et al. 2020).
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: Top: HMI/Stokes I at two different times during the evolution of the LPS. White boxes A, B, and C show the regions of analysis. Bottom: AIA 94/193/211 combination at same times, showing presence of cool plasma; blue contours are for the LPS feature from HMI/Stokes I at 75%, 85%, 95%. The RHESSI 12–18 keV intensity contours at 10%, 30%, 50%, 70%, 90% are shown in all the images in red color for two evolutionary times close to the HMI image time. The lower-left panel matches Figure 1. The orange solid line represent the SDO/HMI limb.
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: A snapshot of the multiwavelength sources observed in SOL 2017-09-10 at 16:16:41 UT, with the background image an AIA 94/193/211 composite. The blue contours show the bright HMI loops at this moment, and the RHESSI image at 12–18 keV is shown by red contours (10%, 30%, 50%, 70%, 90%).
Paper: Observations of Thomson Scattering from a Loop-prominence System
Authors: Juan Carlos Martínez Oliveros, Juan Camilo Guevara Gómez, Pascal Saint-Hilaire, Hugh Hudson, Säm Krucker
Figure caption: SDO/HMI Stokes parameters in the regions A, B, C. The top panel shows the intensity values as a function of time with GOES 1–8 Å in gray. The second panel from the top shows the Q′, U′, and V Stokes parameters. The third panel shows the ratio ﹩{\rm{\Delta }}Q^{\prime} /{\rm{\Delta }}I﹩ for the regions A and B. The bottom panel shows the spatial and temporal evolution of the LPS intensity within a 10″ slit centered at the LPS’s brightest feature, the blue line indicates the apparent motion of the LPS with an average velocity of 7.88 km s−1 whereas the green line indicates the final phase of the event with an average velocity of 1.75 km s−1.
Paper: KIC 2857323: A Double-mode High-amplitude δ Scuti Star with Amplitude Decline of the First Overtone Mode
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Xiao-Ya Sun, Rui-Xuan Tang, Ali Esamdin
Figure caption: Top panels: the amplitude variations of F0 and F1. The solid line is the mean of the 29 time bins and the dashed lines represent the ±3σ amplitude significance interval from the mean. The dashed thick blue line shows the slow linear downward trend of the amplitude of F1. Bottom panels: the phase variations of F0 and F1.
Paper: KIC 2857323: A Double-mode High-amplitude δ Scuti Star with Amplitude Decline of the First Overtone Mode
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Xiao-Ya Sun, Rui-Xuan Tang, Ali Esamdin
Figure caption: Top panel: the amplitude spectrum of the 4 yr of LC data for KIC 2857323 beyond the LC Nyquist frequency (f  N  = 24.466 day−1, the vertical dashed lines), in which the first seven strongest peaks are labeled (red circles), as well as the alias frequencies (labeled by “a”). Middle panel: the amplitude spectrum after prewhitening of seven strongest peaks, another eight significant peaks are labeled. Bottom panel: the residual spectrum after the extraction of all significant frequencies, to an amplitude limit of about 0.1 mmag. No peak is statistically significant in the residual.
Paper: KIC 2857323: A Double-mode High-amplitude δ Scuti Star with Amplitude Decline of the First Overtone Mode
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Xiao-Ya Sun, Rui-Xuan Tang, Ali Esamdin
Figure caption: Visualization of the resulting 1/χ 2 as a function of metallicity Z (top panel) and stellar mass M (bottom panel), respectively. Each circle represents one stellar model with a minimum value of χ 2 along one evolutionary track. The dashed blue lines mark the threshold value of χ 2 (=0.0034), corresponding to about five times the frequency resolution.
Paper: KIC 2857323: A Double-mode High-amplitude δ Scuti Star with Amplitude Decline of the First Overtone Mode
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Xiao-Ya Sun, Rui-Xuan Tang, Ali Esamdin
Figure caption: Evolutionary tracks of 18 candidate models, together with the constraints from effective temperature and luminosity (marked with a red square and error box). Dashed red lines marked the evolutionary tracks of the four models within the above constraints. The blue diamonds denoted the seismic models that can best reproduce the frequencies of the two dominant modes F0 and F1. The δ Sct instability strip (dashed blue lines) is from Murphy et al. (2019).
Paper: KIC 2857323: A Double-mode High-amplitude δ Scuti Star with Amplitude Decline of the First Overtone Mode
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Xiao-Ya Sun, Rui-Xuan Tang, Ali Esamdin
Figure caption: Phase diagram of KIC 2857323 from Kepler data, folded by the frequency, f 1 = 13.1270167 day−1. The red line shows the average value of light curve in a bin of 0.01 phase. The obvious light variation of rapid climb and slow descent is typical for a HADS star.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Integrated emission map of the H30α recombination line shown in color scale and black contours, overlaid with the continuum emission (gray contours), for ALMA source 2 (i.e., core B). Both line and continuum images are from the C9 configuration data. the H30α emission is integrated into the range of −5 km s−1 < V lsr < 70 km s−1. The H30α contours (black) start at 3σ and have intervals of 1.5σ, with 1σ = 0.045 Jy beam−1 km s−1 (5.5 × 102 K). The continuum contours (gray) in both panels have levels of 5σ × 2 n  (n = 0, 1, …), with 1σ = 0.061 mJy beam−1 (1.4 K). (b) Same as panel (b), but for ALMA source 3, and the H30α contours start at 5σ and have intervals of 5σ. (c) H30α spectrum at the continuum peak position of ALMA source 2 (black curve), with a Gaussian fit shown by the red curve. The central velocity (shown by the vertical dashed line) and FWHM of the Gaussian fit are labeled. (d) Same as panel (c), but at the continuum peak position of ALMA source 3. (e) Integrated blueshifted and redshifted H30α emission maps (blue and red contours) overlaid on the 1.3 mm continuum emission (grayscale and white contours) of source 2. The blueshifted and redshifted emission is integrated into the velocity ranges of −5 km s−1 < V lsr < + 30 km s−1 and + 30 km s−1 < V lsr < + 65 km s−1, respectively. The blue and red contours have the lowest contour levels of 5σ and intervals of 2.5σ, where 1σ = 270 K km s−1. The stars mark the continuum peak position. (f) Same as panel (a), but for source 3, and the blue and red contour intervals are 5σ.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Lower-resolution ALMA 1.3 mm (Band 6) continuum image of the G35.2 star-forming region, obtained by combining data from the C3 and C6 configurations. The contour levels are 5σ × 2 n  (n = 0, 1, …), with 1σ = 0.17 K (0.48 mJy beam−1) the synthesized beam is 0.″254 × 0.″250 (P. A. = −36.°3). The crosses mark the position of the compact sources identified from a high-resolution 1.3 mm continuum image and the names of the three main sources are labeled (see Figure 2 and Table 2). (b) The 0.85 mm continuum image was reimaged using the data published by Sánchez-Monge et al. (2014). The synthesized beam is 0.″47 × 0.″42 (P. A. = 51.°4) and contour levels of 5σ × 2 n  (n = 0, 1, …) with 1σ = 0.039 K (0.74 mJy beam−1). The cores A−F identified from the 0.85 mm image by Sánchez-Monge et al. (2014) are labeled. The crosses are the same as in panel (a). (c) Comparison of the ALMA 1.3 mm continuum image (color scale and gray contours) and the 0.85 mm continuum image (cyan contours). (d) Spectral index map between 1.3 and 0.85 mm shown in color scale, overlaid with the 1.3 mm continuum image with the same contour levels as in panel (a). The spectral index is defined as ﹩{\alpha }_{\nu }=\mathrm{log}({I}_{{\nu }_{1}}/{I}_{{\nu }_{2}})/\mathrm{log}({\nu }_{1}/{\nu }_{2})﹩, where ν 1 = 234 GHz and ν 2 = 343 GHz. Only the regions with >10σ continuum emissions and spectral index errors <0.5 are shown in the figure. The origin of the R.A. and decl. offsets in panels (c) and (d) are set to be core B (α ICRS = 18h58m13s.037, ﹩{\delta }_{\mathrm{ICRS}}=+1^\circ 40^{\prime} 35\buildrel{\prime\prime}\over{.} 931﹩).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) The continuum SED of source 2 for the VLA bands and ALMA 1.3 mm continuum (data points). The red dashed line shows the free–free emission of the best-fit model. ALMA 1.3 mm continuum (shown in gray) is not used in the fitting. The inset panel shows the H30α flux integrated over velocity and area (red data point) and the model fit (red dashed line). The model fits the continuum and H30α fluxes simultaneously. (b)−(d) χ 2 distribution with model parameters: electron temperature T  e  (panel (b)), the emission measure EM0 at the radius of 10 au (panel (c)), and the power-law index of the emission measure distribution ρ EM (panel (d)). (e) χ 2 distribution with the ionizing photon rate ﹩{\dot{N}}_{{\rm{i}}}﹩ calculated from T  e , EM0, and ρ EM.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: SEDs (symbols and error bars) comprising VLA and ALMA 1.3 mm continuum flux densities, for the 1.3 mm compact sources with VLA detections, i.e., ALMA sources 1−4. The ALMA 1.3 mm flux densities are measured from the C9 configuration image and are listed in Table 2. The VLA flux densities are taken from Beltrán et al. (2016). An additional 7% of uncertainties due to absolute flux calibration are added to the ALMA 1.3 mm flux densities. The power-law fit to the VLA fluxes, and between VLA 7 mm and ALMA 1.3 mm, are shown by the solid lines. In source 4 (panel (d)), the dashed line shows the power-law fit to the VLA fluxes excluding the 6 cm flux.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: High-resolution ALMA 1.3 mm continuum images from different configurations. (a) Combined image from the C3, C6, and C9 configurations. (b) Combined image from C6 and C9 configurations. (c) Image from C9 configuration alone. (d) Same as panel (c), but zoomed in to the central region. The synthesized beam size of each image is listed in Table 1. The color scale (same for all the panels) is adjusted to emphasize the compact continuum sources. In panels (a) and (b), only the regions with a primary beam response of >0.5 are shown. In panel (c), all the regions with a primary beam response of >0.1 are shown. The identified compact continuum sources are marked with circles and labeled with numbers in panels (c) and (d).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) Distribution of the H30α emission centroids (triangles with error bars) in source 3. Only channels with peak intensities >10σ (1σ = 1.8 mJy beam−1) are included. The position offsets are relative to the continuum peak. The line-of-sight velocities are shown by the color scale. (b) The best-fit disk model for the H30α centroid distribution in source 3 (see the text for more details).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: ALMA 1.3 mm continuum images (color scale) overlaid with VLA 1.3 cm (left column) and 7 mm (right column) continuum images (cyan contours). The wavelengths and configurations of the images are labeled in each panel. Panels (c) and (d) show zoom-in views of the central region (the white squares in panels (a) and (b)). The synthesized beams of the images are listed in Table 1. The contours start from 5σ and have intervals of 10σ. The 1σ rms noise levels of each image are listed in Table 1. The compact continuum sources identified in ALMA 1.3 mm images with corresponding VLA emissions are labeled in panel (d).
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: ALMA long-baseline 1.3 mm continuum images of all the compact sources identified (see Table 2). The contour levels are 4, 8, 12, 16, 20, 40, 80, 160, and 320 times the rms noise 1σ = 0.0608 mJy beam−1 (1.37 K). The synthesized beam is shown in the bottom-left corner of each panel.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The registered energies of a typical simulated flare. During this flare, 61,834 magnetic reconnections occurred (within 884 frames), leading to a total energy release of 5.74 × 104. The left panel shows the amount of energy released at each magnetic reconnection. The right panel illustrates the detected energies in successive frames.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The evolution of the lattice energy in a magnetic vector potential lattice (with 216 grids) during 200,000 driving steps. The initial lattice is constructed using uniformly distributed random numbers. After nearly 5 million evolution steps (dashed line) the system reaches an approximately stationary state. During the following steps, the driving mechanism injects energy into the system, whereas the avalanches emit energy.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The HXR emissions of the solar flare of Figure 3 vs. the selected ARIMA models and relevant residuals in the four spectral bands L, M1, M2, and H.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The ACFs and PACFs of the HXR emissions of the solar flare displayed in Figure 3.