adsabs/AstroCLIMB huggingface dataset:
Paper: The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions
Authors: Ilse De Looze, Dan Milisavljevic, Tea Temim, Danielle Dickinson, Robert Fesen, Richard G. Arendt, Jeremy Chastenet, Salvatore Orlando, Jacco Vink, Michael J. Barlow, Florian Kirchschlager, Felix D. Priestley, John C. Raymond, Jeonghee Rho, Nina S. Sartorio, Tassilo Scheffler, Franziska Schmidt, William P. Blair, Ori Fox, Christopher Fryer, Hans-Thomas Janka, Bon-Chul Koo, J. Martin Laming, Mikako Matsuura, Dan Patnaude, Mónica Relaño, Armin Rest, Judy Schmidt, Nathan Smith, Niharika Sravan
Figure caption: Total integrated MIRI MRS and NIRSpec spectra for one specific ring in the GM (position P2) with line identifications, some of which remain uncertain. The colors indicate whether the line emission is mostly blueshifted (blue), near-rest-frame velocity (green), or redshifted (red). Black lines point to specific dust features. For NIRSpec, the flux was integrated in a 2.5 × 2.5 arcsec2 box centered on the ring to avoid noisy signal at the edges. In the MRS data, several lines ([Ne II], [Ne III]) originate from two distinct velocity (v = 0 and v = 5000 km s−1) components. The [Ar II], [Ar III], [Ar V], [S III], and [S IV] emission lines mostly originate from blueshifted components, whereas the [O IV] line has multiple blue- and redshifted components. The H2 lines trace the ISM along the same line of sight. In the NIRSpec data, the Brα line is the only line originating from the v = 0 km s−1 component, whereas the other lines appear to be emitted from a high-velocity (v = 5000 km s−1) component.
Paper: The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions
Authors: Ilse De Looze, Dan Milisavljevic, Tea Temim, Danielle Dickinson, Robert Fesen, Richard G. Arendt, Jeremy Chastenet, Salvatore Orlando, Jacco Vink, Michael J. Barlow, Florian Kirchschlager, Felix D. Priestley, John C. Raymond, Jeonghee Rho, Nina S. Sartorio, Tassilo Scheffler, Franziska Schmidt, William P. Blair, Ori Fox, Christopher Fryer, Hans-Thomas Janka, Bon-Chul Koo, J. Martin Laming, Mikako Matsuura, Dan Patnaude, Mónica Relaño, Armin Rest, Judy Schmidt, Nathan Smith, Niharika Sravan
Figure caption: This JWST multicolor image presents the main GM region applying the same color scheme for NIRCam and MIRI images as used in Figure 1. The most striking features are dozens of circular holes speckled across the GM, with sizes ranging between ≈1″ and 3″ (see the scale bars for some of the holes in the top). The orange arrows point to a very faint and curved ∼1 pc long ejecta filament that seems to run up against the base of a ring structure with targeted MRS observations in position P2 (see also Figure 1). We argue that the ejecta interaction with a reverse shock at this specific location is coincidental.
Paper: The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions
Authors: Ilse De Looze, Dan Milisavljevic, Tea Temim, Danielle Dickinson, Robert Fesen, Richard G. Arendt, Jeremy Chastenet, Salvatore Orlando, Jacco Vink, Michael J. Barlow, Florian Kirchschlager, Felix D. Priestley, John C. Raymond, Jeonghee Rho, Nina S. Sartorio, Tassilo Scheffler, Franziska Schmidt, William P. Blair, Ori Fox, Christopher Fryer, Hans-Thomas Janka, Bon-Chul Koo, J. Martin Laming, Mikako Matsuura, Dan Patnaude, Mónica Relaño, Armin Rest, Judy Schmidt, Nathan Smith, Niharika Sravan
Figure caption: Comparison of the observed line ratios (gray shaded regions) with the library of radiative shock models from M. G. Allen et al. (2008) for models with different preshock densities n of 10 (blue), 100 (green), and 1000 (red) cm−3 and different ionization mechanisms: shock-ionized emission (solid lines), preionization of unshocked material by the shock’s radiation (dashed–dotted lines), or both (dotted lines). The observations are consistent with low shock velocities (<200 km s−1) but are unable to exactly pinpoint the ionization and excitation mechanism and the gas density.
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: Panels (A) and (B) (top row) show the dynamic spectra of electric field power, E(f, t)2, in the radio frequency range, measured before and at the shock crossing on 2022 September 5 (S1) and 2023 March 13 (S2), respectively. The units are in solar flux units (1 sfu = 10−22 W m−2 Hz−1). The arrival of both shocks at PSP is marked by the red (S1) and blue (S2) arrows on top of the figure. The synchrotron emissions, the coherent plasma emissions (type II and type III), and the local f pe are marked. Panels (A2) and (B2) (middle row) show the degree of circular polarization normalized by total intensity (Stokes V/I; see text for details). Panels (A3) and (B3) (bottom row) show the magnetic field components and magnitude.
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: Characteristics of the synchrotron emission from S1 and the corresponding electron distribution. Panel (A) presents the time evolution of the electron intensity in units of counts s−1 observed between 16:00 UT and 18:00 UT. The arrival of the shock at PSP is marked by the vertical black line at 17:27 UT and the red arrow on top. Panel (B) shows the 10 minute averaged electron energy distribution between 17:17 and 17:27 UT in units of particles cm−2 s−1 sr−1 keV−1. The different detectors of IS⊙IS used to construct the electron spectrum are annotated with colored markers. The approximate power-law fits and the exponents are also shown in the legend. Panel (C) shows the intensity–frequency profiles at specific times leading up to the shock arrival, along with approximate power-law fits to the optically thin regime. The f c for Syn-1, Syn-2, and Syn-3 are indicated by the distinct markers introduced in Figure 1(A).
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: Characteristics of the synchrotron emission from S2 and the corresponding electron distribution. Panel (A) presents the time evolution of the electron intensity in units of counts s−1 observed between 04:00 UT and 07:30 UT. The arrival of the shock at PSP is marked by the vertical black line at 07:13 UT and the blue arrow on top. Panel (B) shows the 10 minute averaged electron energy distribution between 07:03 and 07:13 UT in units of particles cm−2 s−1 sr−1 keV−1. The different detectors of IS⊙IS used to construct the electron spectrum are annotated with colored markers. The approximate power-law fits and the exponents are also shown in the legend. Panel (C) shows the intensity–frequency profiles at distinct times leading up to the shock arrival, and approximate power-law fits to the optically thin regime are shown.
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: Schematic of the synchrotron emission from S1 and S2. The curved purple front represents the traveling shock wave, with magnetic field lines shown in blue. The shock geometry along the reference field lines is labeled as Q ⊥ (quasi-perpendicular) and Q ∥ (quasi-parallel). The finite region on the shock surface where relativistic electrons are accelerated and subsequently emit synchrotron radiation is indicated by the red square. The emitted photons are represented by yellow markers and the notation γ.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The comparison between the total percentage of foreign ejecta within 1 m depth surrounding the CE-6 landing region delivered from 10 potential key source craters without impact gardening and with the impact gardening of (a) 3.0 Gyr, (b) 2.8 Gyr, (c) 2.6 Gyr, and (d) 2.4 Gyr, for the minimum crater diameter of 20 m.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The compositional evolution (left column) that originated from depth ≤1 m (orange dashed–dotted lines) and depth >1 m (green solid lines), and the total foreign material abundance (blue dashed lines in the left column and bar plots in the right column) from five main source craters within 1 m depth surrounding the CE-6 landing region, for four surface ages (i.e., start time) of (a, b) 3.0 Ga, (c, d) 2.8 Ga, (e, f) 2.6 Ga, and (g, h) 2.4 Ga, for the minimum crater diameter of 20 m. The shaded regions show the uncertainties of 1σ.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The comparison between the total percentage of foreign ejecta within 1 m depth surrounding the CE-6 landing region delivered from five main source craters without impact gardening and with the impact gardening of (a) 3.0 Gyr, (b) 2.8 Gyr, (c) 2.6 Gyr, and (d) 2.4 Gyr, for the case in which Chaffee S formed at 2.14 Ga and the minimum crater diameter is 20 m.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The optical maturity parameter (OMAT), FeO abundance, and the Diviner RA (J. L. Bandfield et al. 2011) surrounding craters (a) Chaffee S, (b) Pythagoras (∼2.13 Ga), and (c) Vavilov (∼1.26 Ga). The Clementine-UVVIS-derived OMAT and FeO map is from P. G. Lucey et al. (2000), and the Kaguya-MI-derived OMAT and FeO map is from M. Lemelin et al. (2019).
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The percentage of the foreign materials for 1 and 10 simulation runs, within different sampling depths, at different model start times, for the minimum crater diameter of 20 m. The final abundances of foreign distal ejecta over 10 simulations within the sampling depths of 1.0 and 2.0 m are shown by the blue diamonds and green circles, and the corresponding distal ejecta from one simulation run are depicted by orange (1.0 m) and red (2.0 m) pentagons, respectively. The four groups correspond to the duration of impact gardening after 3.0, 2.8, 2.6, and 2.4 Gyr. The solid vertical lines display the uncertainties of 1σ.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: An example illustrating the elevation evolution within a 1 × 1 km grid at three points in time. (a) No elevation variations at the initial time of the model; (b) elevation after the formation of several on-grid primary craters; and (c) elevation after the delivery of distal ejecta and simultaneous formation of on-grid secondary craters from an off-grid primary crater. Please note that the time steps shown in these illustrations do not correspond to those used in the actual simulation, and the thickness of the distal ejecta has been exaggerated for improved visual clarity.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The compositional evolution of local materials that originated from depth ≤60 m (yellow solid lines) and depth >60 m (red dashed–dotted lines), and the total foreign material abundance (blue dashed lines) within 1 m depth surrounding the CE-6 landing region, for four surface ages (i.e., start time) of (a) 3.0 Ga, (b) 2.8 Ga, (c) 2.6 Ga, and (d) 2.4 Ga, for the minimum crater diameter of 10 m. The shaded regions show the uncertainties of 1σ.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: Crater measurements (D ≥ 10 m) within a circle of 1 km in diameter across the CE-6 landing site (the red star) by an LROC NAC image (M1305784636R; 1.88 m pixel−1 resolution, 78.°94 incidence angle). Mollweide projection.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The comparison between the total percentage of foreign ejecta within 1 m depth and a 0.8 × 0.8 km region centered on the CE-6 landing site, delivered from five main source craters, without impact gardening and with the impact gardening of (a) 3.0 Gyr, (b) 2.8 Gyr, (c) 2.6 Gyr, and (d) 2.4 Gyr, for the minimum crater diameter of 10 m.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The geometry of the improved Maxwell Z-model for the case of Z = 2.7. Within a transient crater with an apparent radius of ﹩{R}_{{\rm{a}}{\rm{t}}},﹩ the ejected materials (within the blue region) move along the excavation flows sourced from the effective center of Z-model flow (EDOZ), represented by the purple filled star, located at a depth of ﹩{d}_{{\rm{E}}{\rm{D}}{\rm{O}}{\rm{Z}}}﹩ beneath the impact site. Each ejected particle tracer (the red filled circles) is originally located at a radial distance ﹩{r}_{0}﹩ from EDOZ and an angular coordinate ﹩{\theta }_{0}﹩ from the nadir. The particle is ejected at a radial distance of ﹩{r}_{e}﹩ and with radial and angular velocities of ﹩{u}_{r}﹩ and ﹩{u}_{\theta },﹩ respectively, following a trajectory depicted by the red dashed line before being redeposited on the pre-impact surface. Particles that are not ejected (the cyan filled circles within the orange region) are assumed to be randomly distributed at varying depths between the final and transient craters for simplification in the model.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The compositional evolution (left column) that originated from depth ≤2 m (orange dashed–dotted lines) and depth >2 m (green solid lines), and the total foreign material abundance (blue dashed lines in the left column and bar plots in the right column) within 2 m depth surrounding the CE-6 landing region, for four surface ages (i.e., start time) of (a, b) 3.0 Ga, (c, d) 2.8 Ga, (e, f) 2.6 Ga, and (g, h) 2.4 Ga, for the minimum crater diameter of 10 m. The shaded regions show the uncertainties of 1σ.
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: (a) Dynamic spectrum averaged to around 8 MHz frequency resolution for the main pulse of pulsar B1929+10. We choose an integration time of approximately 10 s (45 rotation periods) for each spectrum to minimize the impact of system noise. The flux density has been scaled with the peak radio emission of the averaged pulse. (b) To better reveal variations over the frequencies and the arrival time, we plot the observed flux densities (black dots) for the main pulse as a function of the observation time for nine narrow bands with a bandwidth of 50 MHz. Their corresponding centered frequencies are included in the lower left corner of each subpanel, while the cyan dots denote the flux density of the interpulse. The ﹩{{I}_{A}}_{\mathrm{peak}}﹩ represents the peak radio emission of the average pulse for the main pulse, corresponding to the peak radio emission of the interpulse of the averaged pulse. The integration time of each dot is the same as that of each spectrum.
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: Variations over the entire 110 minute observation. We plot the measured DM (a), the measured RM (b), the detection of α (c), and the measured κ DM (d) as a function of the observation time. Each dot corresponds to an integration of 2 minutes. To better exhibit the event, we use the vertical gray shadow to mark the region of the event.
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: Narrowband pulsar timing of nine narrow frequencies with a bandwidth of 50 MHz as a function of the observation time for pulsar B1929+10; their corresponding frequencies are included in the upper left corner of each panel, as labeled. In each panel, the black dot represents the arrival time of a pulse profile in a short duration of 2 minutes.
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: The scatter plots of the timing residuals between pairs of frequencies. The frequencies are labeled and in units of MHz. The dots correspond to the arrival times of pulse profiles in a short duration of 2 minutes and are in units of microseconds.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: Geological contexts surrounding the CE-6 landings site. (a, b) Locations of 10 potential main foreign source craters in this study (see Table 2). The yellow and green hollow circles indicate the Copernican and Eratosthenian craters, respectively. The landing sites of previous lunar sample-return missions are labeled by A (Apollo), L (Luna), and CE (Chang’e). Lunar Reconnaissance Orbiter (LRO) Wide-Angle Camera (WAC) image (100 m pixel−1 resolution). (c) The boundary of the CE-6 mare unit (white solid curve; X. Zeng et al. 2023) and rays of Chaffee S crater (orange dashed lines; C. Orgel et al. 2024). Chang'e-2 (CE-2) Digital Orthophoto Map (DOM; 7 m pixel−1). (d) TiO2 abundance map surrounding the CE-6 landing region, with the CE-6 mare unit outlined by the black curve. Kaguya Multiband Imager (MI) TiO2 Map (∼60 m pixel−1; C. Yang et al. 2023). (e) The study region (1 km × 1 km in size, with the center at the CE-6 landing site) in our model. LROC NAC image (ID: M166854798R and M166854798L; ∼0.5 m pixel−1). The red stars label the location of the CE-6 landing site. Panel (a) is displayed by simple cylindrical projection, and panels (b)–(e) are displayed by Mercator projection.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: Schematic showing the grid and the on-grid craters. (a) The establishment of the grid, with a size of 1 km × 1 km × 100 m (w = 1 km). The surface of the grid was divided into 500 × 500 pixels. The blue and yellow cubes on the right show the uncompressed tracers representing distal foreign ejecta and local materials, respectively. (b) Schematic of the generated on-grid and off-grid primary craters (pink filled circles without and with diagonal stripes, respectively). (c) Schematic of the on-grid and off-grid secondary craters (cyan circles without and with diagonal stripes, respectively) generated by an off-grid primary crater and located in a narrow annulus, whose inner and outer radii (defined by the two black dashed curves) are the distances from the grid center (open star) to the primary crater center (﹩r﹩) and the maximum secondary center (﹩{\rm{\Delta }}r﹩) at extreme situations (see Appendix B).
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: (a) Sketch for the outflow from the pulsar. To better unravel the local environment near the pulsar, the bow shock structure and the proper motion are also included. (b) Fitting of optical depths under nine frequency bands using bremsstrahlung absorption. The optical depths are estimated from Figure 1 through ﹩\tau =\mathrm{ln}(I/{I}_{\min })﹩ and are shown as blue dots with error bars in the plot. The errors are estimated from the fluctuation in flux density in the “pulse-off” regions. The green curve of ﹩{\tau }_{\mathrm{em},\nu }^{{ff}}﹩ is derived from the least-squares fitting. The derived ν p and n  e  are also marked on the plot.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The percentage evolution of local materials that originated at depth ≤1 m (orange dashed–dotted lines) and depth >1 m (green solid lines), and the total foreign ejecta (blue dashed lines) within the uppermost 1 m depth at the CE-6 landing site. The black triangles indicate the occurrence of key important impact events (i.e., the formation of Chaffee S (CS), Pythagoras (P), and Vavilov (V)). Four panels show the scenario with different start times of (a) 3.0 Ga, (b) 2.8 Ga, (c) 2.6 Ga, and (d) 2.4 Ga, respectively. The shaded regions show the 1σ uncertainties, representing the pixel-to-pixel variation across the model grid from one simulation run. This applies to the subsequent figures, including those in Appendix C.
Paper: An Extreme Radio Fluctuation of Pulsar B1929+10
Authors: Zhengli Wang, Shunshun Cao, Jiguang Lu, Yulan Liu, Xun Shi, Jinchen Jiang, Enwei Liang, Weiyang Wang, Heng Xu, Renxin Xu
Figure caption: The parameters are used to detect the behaviors of the profile defined in Equations (3), (4), (5), and (6) as a function of the observation time. The black dots represent the results of the observing frequency 1250 MHz with a bandwidth of 450 MHz, while the blue dots correspond to that of the frequencies that are lower than 1200 MHz. The dots correspond to the results in a 2 minute integration. The vertical gray shadow corresponds to the region of the event.