adsabs/AstroCLIMB huggingface dataset:
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: The probability of model selection for each model (vertical axis) given a certain Tlast (horizontal axis), with a bin width of 4 s. The color gradients represent different models: Shen (gray to black), LS220 (light red to red), Furusawa–Togashi (light blue to blue), and Togashi (light green to green). The differences in color intensity represent variations in the baryonic mass of the PNS, with darker colors indicating higher mass.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Same as Figure 10, but showing the comparison of different PNS baryonic masses in Shen EOS. The red, green, blue, and light purple represent Mb = 1.40M⊙, Mb = 1.54M⊙, Mb = 1.70M⊙, and Mb = 1.86M⊙, respectively.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: The time difference distribution between the 500th-to-last event and 1000th-to-last event. The black, red, blue, and green lines represent Shen, LS220, Furusawa–Togashi, and Togashi EOS, respectively. The horizontal axis shows the difference between the time of the 500th-to-last event (T500) and the time of the 1000th-to-last event (T1000). The solid and grid lines in panel (b) mean a MZAMS = 15M⊙ and MZAMS = 40M⊙, respectively.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Schematic diagram of Tlast determination method. It represents supernova neutrino and background events plotted over time, with their corresponding energy values represented on the vertical axis. The green box shows supernova neutrino events whose energy is more than Eth and the black boxes indicate background events. White boxes with green outlines show supernova neutrino events that are excluded because their energy is below a Eth or their time difference from Tlast exceeds Twid.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: The Tlast distribution for each combination of Twid and Eth. Panel (a), (b), (c), and (d) correspond to Shen EOS, LS220 EOS. Furusawa–Togashi EOS, and Togashi EOS, respectively. Here, the PNS models with mass of Mb = 1.40M⊙ and MZAMS = 15M⊙ are shown.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: Average interval between signal events as a function of time after the bounce. The black, red, blue, and green represent Shen EOS, LS220 EOS. Furusawa–Togashi EOS, and Togashi EOS, respectively.
Paper: Observing Supernova Neutrino Light Curves with Super-Kamiokande. VI. A Practical Data Analysis Technique Considering Realistic Experimental Backgrounds
Authors: Fumi Nakanishi, Ken'ichiro Nakazato, Masayuki Harada, Yusuke Koshio, Ryuichiro Akaho, Yosuke Ashida, Akira Harada, Masamitsu Mori, Kohsuke Sumiyoshi, Yudai Suwa, Roger A. Wendell, Masamichi Zaizen
Figure caption: The probability of model selection (vertical axis) given a certain time difference (horizontal axis), with a bin width of 0.5 s. The color gradients are the same as Figure 13.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: (a) Temporal evolution of X-ray count rates observed by RHESSI in the energy bands 3–6 keV, 6–12 keV, 12–25 keV, and 25–50 keV during 03:30 UT–04:15 UT on 2014 January 8. The GOES SXR flux in 1–8 Å (solid black curve) and 0.5–4 Å (dashed black curve) channels are also shown for the same time interval. RHESSI fluxes are normalized by factors of ﹩\frac{1}{15}﹩, 2, 3, and 7 for 3–6, 6–12, 12–25, and 25–50 keV energy bands, respectively. RHESSI attenuator states, A0 and A1, are shown by red and blue horizontal bars, respectively. Two arrows are used to indicate two peaks in RHESSI light curve in the energy band 25–50 keV. (b) Cotemporal AIA (E)UV light curves in 94​​​​​, 131, 171, 193, 304, and 1600 Å channels that are normalized by their corresponding peak fluxes. For the clear visualization, these curves are further normalized by factor of 3.0, 1.5, 1.1, 1.5, and 2.0 for 94, 131, 304, 193, and 1600 Å, respectively. The region used for the construction of AIA light curves is shown by a red box in Figure 2(l). The gray shaded region in both the panels (a) and (b) show the fast rise phase of the coronal loop system.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: (a)–(b) AIA 171 Å images on 2014 January 8 at 03:41 UT and 03:44 UT, respectively, to show the evolution of pre-CME arcade. White straight line in panel (a) shows the direction along which we have constructed a time-slice diagram. The apex of the pre-CME arcade is marked by the cross symbol in both the panels. (c) Time-slice diagram showing the eruption of dense coronal loop system during 03:20 UT–04:10 UT. Two phase evolution of the arcade is clearly observed. In the first phase, loop system evolves slowly with a linear speed ≈3 km s−1, and in the second phase, it accelerates to a very high speed of ≈400 km s−1. For reference, we overplot GOES SXR flux at 1–8 Å channel by green curve.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: (a)–(f) A series of few selected AIA 131 Å images showing the evolution of the hot flux rope. (g) Time-slice diagram showing kinematic evolution of the hot flux rope during 03:20 UT to 03:50 UT. Two phase evolution (i) slow rise with speed ≈10 km s−1 and (ii) fast rise with speed ≈ 300 km s−1 of the flux rope is noticed. Red straight line in panel (f) shows the slit direction along which we have constructed the time-slice diagram.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: Multiwavelength overview of the pre-CME coronal arcade in the AIA 171 Å (panel (a)), 193 Å (panel (b)), 131 Å (panel (c)), and 94 Å (panel (d)) wavelengths. Red box indicates the core region while black and green arrows mark the low-lying and high overlying coronal loops, respectively.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: (a)–(b) AIA 171 Å images at 02:00 UT and 03:20 UT, respectively, to show the evolution of coronal loops. White straight line in panel (a) shows the direction along which we have constructed a time-slice diagram. (c) Time-slice diagram showing evolution of coronal loop during 02:00 UT–03:20 UT.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: (a) AIA 171 Å image during the peak of the M3.6 flare. RHESSI contours in the energy bands 6–12 keV (red), 12–25 keV (green), and 25–50 keV (blue) are overplotted in order to show the location of the HXR sources during the peak of the flare. (b)–(e) Temporal evolution of the HXR sources in 3–6 keV (black), 6–12 keV (red), 12–25 keV (green), and 25–50 keV (blue) energy bands from the early stage to the decay phase of the flare. RHESSI images are constructed by the CLEAN algorithm. Contour levels are 50%, 60%, 70%, and 90% of the peak flux of each images.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: A series of selected AIA 171 Å images showing the eruption of the two filaments F1 and F2 from the AR. Red and blue arrows indicate the two filaments F1 and F2, respectively, and their subsequent eruption. Black arrows in panels (f)–(g) are used to show the bifurcated parts of second filament F2 while in panel (h) to mark the erupting part of F2.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: Dynamic radio spectrum observed by HiRAS in the frequency range 50–500 MHz during 03:30 UT–04:00 UT. Many discrete type III radio bursts are observed during 03:45 UT–03:46 UT. A split-band harmonic type II radio burst is noticed during 03:46 UT–03:56 UT. For reference, GOES SXR flux in 1–8 Å wavelength is overplotted by white curve.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: A series of selected AIA 304 Å images showing the evolution of the coronal loops and subsequent filament eruption. Yellow arrows in panel (a) indicate coronal loop system. White arrows are used to show the eruption of the coronal loop system. Green and blue arrows in panel (b) are used to show the two filaments F1 and F2, respectively. Black arrows in panel (e) mark the bifurcated parts of filament F2. Sky blue arrow in panel (f) marks the postflare loop arcade.
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: EM maps of the AR for three different temperature ranges: 1.0–1.5 MK (top row), 2.5–3.5 MK (middle row), and 4.5–7.5 MK (bottom row) at three selected times 03:40 UT (left column), 03:46 UT (middle column), and 03:55 UT (right column).
Paper: Blowout Expansion of Overlying Coronal Loops and Subsequent Filament Eruption: AIA and RHESSI Observations
Authors: Hema Kharayat, Bhuwan Joshi, Binal D. Patel, Ramesh Chandra
Figure caption: Total EM (left column) and temperature (right column) maps of AR at 03:43 UT and 03:46 UT. Note that, to derive total EM, the DEM is integrated over the temperature range of log T = 5.7 to log T = 7.3.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: Light curves of all GRBs in the corresponding time bins.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: The evolution of ΔDIC over time. The gray shading is the light curve, and the red dotted line indicates ΔDIC =10. Exceeding the red dashed line indicates compelling evidence of a thermal component.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: The top panels show the distribution of α, while the bottom panels show the distribution of Ep. The left and right panels correspond to the first and second pulses of the sample, respectively. The blue solid line represents α = −0.67.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: The spectral parameter α fitted with the best model is shown as a function of time. The green and purple regions represent the best-fitting model without a BB component (“best model”) and with a BB component (“best model + BB”), respectively. The red dashed line indicates α = −0.67.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: Ep evolution over time. The green part and the purple part represent the best model without BB component (best model) and the best model with BB component (best model+BB), respectively.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: Norris function fitting results of all GRB pulses.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: Direct comparison of the raw spectra for the two pulses of each GRB. The four red dashed lines from left to right correspond to 10, 50, 100, and 300 KeV, respectively. Here P2/P1 denotes the ratio of the photon counts in the second pulse to those in the first pulse, computed in each energy band, providing a direct measure of the relative spectral consistency between the two pulses.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Time-series plots for equal-mass impacts for fixed impact speeds and varying distances with the -R impact geometry. Each plot shows the ratio of the largest remnant to the target mass as a function of time (in hours) for a specific impact speed, indicated on the top of each subfigure. The color scale indicates the distance to the central body in normalized units. Plotting Mlr normalized to the target mass, rather than the total mass, makes it easier to distinguish the threshold between an erosive and accretionary collision, which is indicated by the dotted black line.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: The two impact geometries considered in this study, shown in a radial–tangential–normal (RTN) coordinate frame. The ﹩\hat{R}﹩ direction points directly away from the central body, ﹩\hat{T}﹩ points along the target’s orbital velocity vector, and ﹩\hat{N}﹩ completes the right-handed triad, pointing along the orbit normal. For a “-R” collision, the impactor comes from the ﹩-\hat{R}﹩ direction with a relative velocity in the ﹩+\hat{R}﹩ direction. Similarly, “+T” collisions have the impactor coming from the ﹩+\hat{T}﹩ direction with its relative velocity in the ﹩-\hat{T}﹩ direction.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Snapshots of equal-mass ratio collisions with an impact speed of 1vesc and a radial (-R) impact geometry for δ = 2 and δ = 3. When the bodies are close-in, the tides from the primary prevent them from fully merging, and instead, they temporarily form a contact binary which is then stripped, resulting in a hit-and-run. Animations of these two simulations can be found in the accompanying Zenodo repository at doi:10.5281/zenodo.15790522.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Snapshots of collisions with Mproj/Mtarg = 0.01 at different distances with an impact speed of 30vesc and the radial (-R) impact geometry. All three collisions have the same specific energy of QR ≈ 352 J kg−1. Animations of these three simulations can be found in the accompanying Zenodo repository at doi:10.5281/zenodo.15790522.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Snapshots of equal-mass ratio collisions for different distances with an impact speed of 2vesc and a radial (-R) impact geometry. All three collisions have the same specific energy of QR ≈ 38.7 J kg−10 yet result in entirely different outcomes as a result of the impact triggering a tidal disruption for close-in targets.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: The same as Figure 2, but for Mproj/Mtarg = 0.01 impacts with the -R impact geometry.
Paper: A Reidentification of Six Candidate Gravitationally Lensed Gamma-Ray Bursts
Authors: Yu Zhao, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li
Figure caption: Amati relation. In the figure, maroon circles represent Type I GRBs, and blue circles represent Type II GRBs. The first pulses of the sample GRBs are shown as pentagrams, while the second pulses are shown as diamonds. GRBs with the same color correspond to the same event.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: (a) Plots of ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ for collisions for all three mass ratio collisions and radial (-R) impacts. (b) The same plot as (a), with the scaling from Equation (12) to account for tides. Note: this scaling is not fit to the data, but rather the value of ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ at δ = 10 is taken as a notional value for the value of ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ at an infinite distance. This simple scaling does a remarkable job of predicting the effective ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ at close orbital distances, despite its simplicity. The black vertical dashed line indicates the approximate Roche limit for a cohesionless, spherical satellite with a 35∘ friction angle and demonstrates that tides play an important role in collisional disruptions well outside the Roche limit.
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: Cluster mass vs. redshift distribution of the PSZ2 clusters. The subsample of PSZ2 in LoTSS-DR2 (A. Botteon et al. 2022a) is reported in black. Circles denote clusters with halos having LLS > 2 Mpc and are color-coded as follows: in cyan are the megahalos (V. Cuciti et al. 2022), in red are the clusters analyzed in this work, and in magenta are other clusters reported in the literature. The solid lines represent the boundaries above which megahalos are assumed to be detected with LOFAR observations assuming that their surface brightness is ﹩\propto \,{M}_{500}^{\beta }{(1+z)}^{-4}﹩, for three possibilities for β.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Best-fit values of ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩ for simulations with Mproj/Mtarg = 0.1 as a function of normalized distance. A control case with no tides (but with rotation) is indicated with green dots, while the tangential (+T) and radial (-R) impact geometries are, respectively, indicated with black and blue triangles. The second x-axis indicates the target’s rotation rate. The error bars show the 1σ standard deviations resulting from nonlinear least squares to give a rough indication of the quality of the fit. The fits get progressively worse with decreasing orbital distance, as a result of the “universal law” breaking down due to the influence of tides. Overall, tangential collisions tend to be slightly more destructive (i.e., a lower ﹩{Q}_{\,\rm{RD}\,}^{\star }﹩).
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: PLCK G287.0+32.9 field (square-root scale) full band continuum images from MeerKAT observations using S band (1.9–2.8 GHz), L band (0.9–1.7 GHz), and UHF bands (0.5–1.0 GHz) and uGMRT Band 3 (300–500 MHz). All images have a common resolution of 20″. The radio beam size is indicated in the bottom-left corner of each image. The images show large scale diffuse radio emission, including two symmetrically located relics and a 3.5 Mpc radio halo. The contour levels are drawn at [1, 2, 4, 8. . . ] × 3σrms. Dashed contours depict the −3σrms contours. For image properties, see Table 4 (IM1, IM2, IM3, and IM4).
Paper: Radial Profiles of Radio Halos in Massive Galaxy Clusters: Diffuse Giants Over 2 Mpc
Authors: K. Rajpurohit, A. Botteon, E. O'Sullivan, W. Forman, M. Balboni, L. Bruno, R. J. van Weeren, M. Hoeft, G. Brunetti, C. Jones, A. S. Rajpurohit, S. P. Sikhosana
Figure caption: PLCK G287.0+32.9 field (square-root scale) full band continuum images from MeerKAT observations using S band (1.9–2.8 GHz), L band (0.9–1.7 GHz), and UHF bands (0.5–1.0 GHz) and uGMRT Band 3 (300–500 MHz). All images have a common resolution of 50″. The radio beam size is indicated in the bottom-left corner of each image. The images are used to extract radial surface brightness profiles of the halo as a function of frequency. The contour levels are drawn at [1, 2, 4, 8. . . ] × 3σrms. Dashed contours depict the −3σrms contours. For image properties, see Table 4 (IM5, IM6, IM7, and IM8).
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: Snapshots of simulations with Mproj/Mtarg = 0.1, an impact speed of vimp = 10vesc, at an orbital distance of δ = 3 for the control case with no tidal potential, and the two impact geometries: radial (-R) and tangential (+T). For the case with no tides, the target still has the same pre-impact spin rate as if it were in synchronous rotation on an orbit at δ = 3. Animations of these three simulations can be found in the accompanying Zenodo repository at doi:10.5281/zenodo.15790522.
Paper: The Influence of Central Body Tides on Catastrophic Disruptions of Close-in Planetary Satellites
Authors: Harrison Agrusa, Patrick Michel
Figure caption: The same plot from Figure 10, with the normalized distance δ for each natural satellite with a measured bulk density around Mars, Jupiter, Saturn, Uranus, and Neptune. Many of the small moonlets around the outer planets orbit in a regime where their catastrophic disruption threshold should be significantly smaller than that derived from scaling laws or numerical models that do not account for tides. The names and orbital distances are listed in Table 3 in Appendix B.