adsabs/AstroCLIMB huggingface dataset:
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The radial profiles of region S1. The red data points are the profile of the 2019–2020 observations. The cyan line is the profile of the 2006 observations without a shift. The blue line is the 2006 profile shifted by the measured expansion. The lower panel shows the residuals of the 2020 profile and the shifted 2006 profile.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The spectrum of region S2 from the Epoch B data fit with a vpshock model and the background model. The black points and line are the spectral data and model. The red line is the background model. The vpshock model parameters are listed in Table 8.
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: Multiwavelength observations of the M8.7 flare, which occurred on 2024 July 29. (a1)–(a3) AIA 131 Å raw and running difference images taken at times corresponding approximately to those shown in panels (a1)–(a3) of Figure 5. (b) LASCO C2 running difference image at 14:12 UT, with a cyan arrow indicating the CME associated with this filament eruption event. (c1)–(c2) AIA 171 Å running difference images taken at times corresponding approximately to those shown in panels (a2)–(a3) of Figure 5. (d) Irradiance variations of O V 629.7 Å. The vertical dashed lines mark the Hα (black) and GOES (blue) peak times. (e) Evolution of pre-event-subtracted O V spectra during this event. (f) Double Gaussian fitting result of the O V line profile near its peak time, showing distinct central and blueshifted emission components.
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: Multiwavelength observations of the C6.7 flare that occurred on 2024 June 16. (a1)–(a3) AIA 131 Å images taken at times corresponding approximately to those shown in panels (a1)–(a3) of Figure 1. (b) LASCO C2 running difference image at 16:36 UT, retrieved from https://cdaw.gsfc.nasa.gov/. (c1)–(c2) AIA 171 Å images taken at times corresponding approximately to those shown in panels (a2)–(a3) of Figure 1. The cyan and magenta arrows in panel (c1) indicate the filament and flare ribbons, respectively.
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: Multiwavelength observations of the quiescent filament eruption that occurred on 2024 April 11. (a1)–(a3) AIA 131 Å raw and running difference images taken at times corresponding approximately to those shown in panels (a1)–(a3) of Figure 3. (b) LASCO C2 running difference image at 07:00 UT, with a cyan arrow indicating the CME associated with this filament eruption event. (c1)–(c2) AIA 171 Å running difference images taken at times corresponding approximately to those shown in panels (a2)–(a3) of Figure 3. The cyan arrows in panels (a2) and (c1) indicate the direction of filament eruption.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Spectral lag evolution and its correlation with luminosity during the ME and EE phases of GRB 240619A. Panel (a) shows the spectral lags between different energy bands, represented as energy-dependent spectral lags between the lowest energy band and any higher energy band. Black filled circles and red diamonds correspond to the ME and EE phases, respectively. Panel (b) presents the relationship between spectral lag and luminosity. Black squares and black circles represent the SGRB and LGRB samples, respectively. The blue shaded region denotes the 2σ confidence interval of the fitted relation for the LGRB sample. The yellow and green pentagrams correspond to the ME and EE phases of GRB 240619A, respectively.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Correlations of hardness ratio (HR) and peak energy (Ep) with T90. Panel (a) presents the relationship between HR and T90, including a comparison with other Fermi GRB samples reported by J.-M. Chen et al. (2025). Panel (b) shows a similar analysis for the correlation between Ep and T90. The color bar on the right indicates the probability of each GRB being classified as a short GRB. The yellow and green pentagrams represent the ME and EE phases of GRB 240619A, respectively.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: The Amati and Yonetoku relations. In panel (a), the gray and reddish-orange symbols represent the SGRB and LGRB samples, respectively. In panel (b), black symbols denote the SGRB sample. The yellow and green pentagrams correspond to the ME and EE phases of GRB 240619A, respectively, while the yellow and green diamonds represent the ME and EE phases of GRB 211211A. The shaded regions indicate the 2σ confidence intervals.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: Composite light curve analysis for GRB 240619A. (a) Shows the light curve from NaI detectors within the 8–900 keV energy range. (b) Presents the cumulative photon count curve, with the red lines indicating the range of values between the 5th and 95th percentiles of cumulative photon counts.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: The relationship between the amplitude parameter (f(feff)) and T90. Gray, blue, and red symbols represent the LGRB, SGRB, and SGRB-EE samples, respectively. The yellow pentagram denotes GRB 240619A.
Paper: GRB 240619A: Evidence for a Compact Star Merger Origin
Authors: Jia-Ming Chen, Ke-Rui Zhu, Xue-Zhao Chang, Zhao-Yang Peng, Li Zhang
Figure caption: The relation between the minimum variability timescale (MVT) and T90, where the yellow and green pentagrams represent the ME and EE phases of GRB 240619A, respectively. The purple, orange, and green ellipses indicate the 1σ, 2σ, and 3σ confidence regions, respectively.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Evolution of ejecta density (the first row), velocity (the second row), and temperature (the third row) profiles along a representative sampling line. The first plot is for the backward ejecta; the sampling line originates from 2R* above the disk midplane with angle 20° from x = 0 (the thick brown line in Figure 1). The second plot is for the forward ejecta; the sampling line originates from 2R* below the disk midplane with angle 15° from x = 0 (the thick blue line in Figure 1). The blue, green, yellow, and red lines in the plots correspond to times of 5.0 minutes, 7.5 minutes, 9.7 minutes, and 12.2 minutes, respectively, measured since the star crosses the disk midplane. The black dashed lines in the first row of forward ejecta show two power-law fits ρ ∝ r−0.9 and ρ ∝ r−7.1. The dots in the first and second rows show the location where projected velocity equals the star incident velocity ∣vej∣ = 0.1c. In the upper panel, the blue dot corresponds to ρ = 1.0 × 10−14  g cm−3 and does not appear in the plot.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Gas density snapshots from H1_hd_v0.1c (the first row), H1_md_v0.1c (the second row), and H1_ld_v0.1c (the third row). The labeled time is the time since the star is at the disk midplane. The colored lines in the second column of H1_md_v0.1c correspond to lines where we sample ejecta 1D profiles.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: The bow shock formed between the star and disk in H1_hd_v0.07c at t = 2.5 minutes since the star enters the disk, corresponding to the time when the star is at the midplane of the disk. From left to right, we show gas density, temperature, Mach number, and radiation energy density. The two black circles in the first two panels label the stellar radius R* = R⊙ and the empirical standoff distance 1.143R*. In the rightmost plot, the white arrows show the velocity vectors in the disk frame.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: One-dimensional profiles of forward ejecta (light- and dark-blue lines) and backward ejecta (light- and dark-brown lines) in H1_md_v0.1c at t = 5.0 minutes since the star is at the disk midplane. The lines of sampled profiles are also shown in Figure 1. The thick line with dark color is the representative line in each ejecta. From the first to the third row, we show density, velocity projected on the line, and gas temperature profiles. The low-density and high-temperature feature in the brown lines are related to the small amount of gas with floor density, similar to a contact discontinuity. The high-temperature feature in the blue lines is the “Zel’dovich spike.”
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Locations of randomly sampled ejecta points that are extrapolated to 0.07 days (left), 0.12 days (middle), and 0.5 days (right) in the black hole centered frame. The red points are estimated to be with positive orbital energy (approximately unbound to the black hole); blue points are estimated to be with negative orbital energy (approximately bound to the black hole). The disk rotation is assumed to be clockwise (from positive z to negative z). The black hole location is at (0,0,0), marked by the black star. The three circles correspond to R = 50rs (where the star–disk collision occurs), R = 100rs, and R = 200rs.
Paper: Multiband Emission from Star–Disk Collisions and Implications for Quasiperiodic Eruptions
Authors: Xiaoshan Huang, 小珊 黄, Itai Linial, Yan-Fei Jiang, 燕飞 姜
Figure caption: Evolution of sampled points' distance to the black hole extrapolated up to 4 days. The red lines and blue lines represent points with positive orbital energy (approximately unbound) and negative orbital energy (approximately bound), randomly sampled from the ejecta. In the lower panel, the black lines are randomly sampled points from disk gas that is shocked and shows enhanced radiation temperature. The black dashed lines in both panels are the assumed initial collision position at 100 rg.
Paper: JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion
Authors: K. Medler, C. Ashall, P. Hoeflich, E. Baron, J. M. DerKacy, M. Shahbandeh, T. Mera, C. M. Pfeffer, W. B. Hoogendam, D. O. Jones, S. Shiber, E. Fereidouni, O. D. Fox, J. Jencson, L. Galbany, J. T. Hinkle, M. A. Tucker, B. J. Shappee, M. E. Huber, K. Auchettl, C. R. Angus, D. D. Desai, A. Do, A. V. Payne, J. Shi, M. Y. Kong, S. Romagnoli, A. Syncatto, C. R. Burns, G. Clayton, M. Dulude, M. Engesser, A. V. Filippenko, S. Gomez, E. Y. Hsiao, T. de Jaeger, J. Johansson, K. Krisciunas, S. Kumar, J. Lu, M. Matsuura, P. A. Mazzali, D. Milisavljevic, N. Morrell, R. O'Steen, S. Park, M. M. Phillips, A. P. Ravi, A. Rest, J. Rho, N. B. Suntzeff, A. Sarangi, N. Smith, M. D. Stritzinger, L. Strolger, T. Szalai, T. Temim, S. Tinyanont, S. D. Van Dyk, L. Wang, Q. Wang, R. Wesson, Y. Yang, S. Zsíros
Figure caption: Velocity evolution of [Ni II] 6.636 μm, [Ar II] 6.985 μm, [Co II] 10.521 μm, and [Ne II] 12.813 μm. While the neon, argon, and cobalt lines are centered around 0 km s−1, the nickel emission feature is blueshifted by ∼1000 ± 500 km s−1 at all epochs. All emission features have been corrected by removing a linear continuum across the bottom of the features to remove the influence of the IR excess, especially at late times, when the lines are weaker. The FWHM and peak velocity determined by Gaussian fits are shown in the middle and bottom rows, respectively.
Paper: JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion
Authors: K. Medler, C. Ashall, P. Hoeflich, E. Baron, J. M. DerKacy, M. Shahbandeh, T. Mera, C. M. Pfeffer, W. B. Hoogendam, D. O. Jones, S. Shiber, E. Fereidouni, O. D. Fox, J. Jencson, L. Galbany, J. T. Hinkle, M. A. Tucker, B. J. Shappee, M. E. Huber, K. Auchettl, C. R. Angus, D. D. Desai, A. Do, A. V. Payne, J. Shi, M. Y. Kong, S. Romagnoli, A. Syncatto, C. R. Burns, G. Clayton, M. Dulude, M. Engesser, A. V. Filippenko, S. Gomez, E. Y. Hsiao, T. de Jaeger, J. Johansson, K. Krisciunas, S. Kumar, J. Lu, M. Matsuura, P. A. Mazzali, D. Milisavljevic, N. Morrell, R. O'Steen, S. Park, M. M. Phillips, A. P. Ravi, A. Rest, J. Rho, N. B. Suntzeff, A. Sarangi, N. Smith, M. D. Stritzinger, L. Strolger, T. Szalai, T. Temim, S. Tinyanont, S. D. Van Dyk, L. Wang, Q. Wang, R. Wesson, Y. Yang, S. Zsíros
Figure caption: Spectral evolution of the [O I] 0.6300, 0.6363 μm doublet and [Ca II] 0.7292, 0.7324 μm doublet. The features are plotted in velocity space relative to the rest-frame wavelengths of the [O I] 0.6300 μm and [Ca II] 0.7292 μm lines, respectively. The [O I] 0.6300,  0.6363 μm features show a significant blueshift of ∼1300 ± 500 km s−1, similar to the blue peak observed in the split H emission peak, while the [Ca II] 0.7292 0.7324 μm doublet remains centered at the rest wavelength. The difference in the location of the peaks suggests that the O and Ca are located in drastically different regions of the SN ejecta.
Paper: JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion
Authors: K. Medler, C. Ashall, P. Hoeflich, E. Baron, J. M. DerKacy, M. Shahbandeh, T. Mera, C. M. Pfeffer, W. B. Hoogendam, D. O. Jones, S. Shiber, E. Fereidouni, O. D. Fox, J. Jencson, L. Galbany, J. T. Hinkle, M. A. Tucker, B. J. Shappee, M. E. Huber, K. Auchettl, C. R. Angus, D. D. Desai, A. Do, A. V. Payne, J. Shi, M. Y. Kong, S. Romagnoli, A. Syncatto, C. R. Burns, G. Clayton, M. Dulude, M. Engesser, A. V. Filippenko, S. Gomez, E. Y. Hsiao, T. de Jaeger, J. Johansson, K. Krisciunas, S. Kumar, J. Lu, M. Matsuura, P. A. Mazzali, D. Milisavljevic, N. Morrell, R. O'Steen, S. Park, M. M. Phillips, A. P. Ravi, A. Rest, J. Rho, N. B. Suntzeff, A. Sarangi, N. Smith, M. D. Stritzinger, L. Strolger, T. Szalai, T. Temim, S. Tinyanont, S. D. Van Dyk, L. Wang, Q. Wang, R. Wesson, Y. Yang, S. Zsíros
Figure caption: Structure of SN 2023ixf and its surrounding CSM. Black circles indicate clumps within the dense CSM, as well as H- and O-rich ejecta. The elemental distribution explains the observed line features in H, O, Ne, Ar, Co, and Ni. Variations in the hydrogen velocities and spectral bumps arise from interactions of H-rich ejecta with both low-density and clumpy CSM. The blueshifted O peaks are best explained by asymmetric O-rich ejecta or a massive O-rich clump along the line of sight. A jet, oriented perpendicular to the observer’s view (eye symbol, right), could also naturally account for the asymmetric distribution; however, more detailed modeling is required to establish its presence.
Paper: JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion
Authors: K. Medler, C. Ashall, P. Hoeflich, E. Baron, J. M. DerKacy, M. Shahbandeh, T. Mera, C. M. Pfeffer, W. B. Hoogendam, D. O. Jones, S. Shiber, E. Fereidouni, O. D. Fox, J. Jencson, L. Galbany, J. T. Hinkle, M. A. Tucker, B. J. Shappee, M. E. Huber, K. Auchettl, C. R. Angus, D. D. Desai, A. Do, A. V. Payne, J. Shi, M. Y. Kong, S. Romagnoli, A. Syncatto, C. R. Burns, G. Clayton, M. Dulude, M. Engesser, A. V. Filippenko, S. Gomez, E. Y. Hsiao, T. de Jaeger, J. Johansson, K. Krisciunas, S. Kumar, J. Lu, M. Matsuura, P. A. Mazzali, D. Milisavljevic, N. Morrell, R. O'Steen, S. Park, M. M. Phillips, A. P. Ravi, A. Rest, J. Rho, N. B. Suntzeff, A. Sarangi, N. Smith, M. D. Stritzinger, L. Strolger, T. Szalai, T. Temim, S. Tinyanont, S. D. Van Dyk, L. Wang, Q. Wang, R. Wesson, Y. Yang, S. Zsíros
Figure caption: IRTF/SpeX and Keck/NIRES spectra of SN 2023ixf between 250 and 725 days. The telluric regions are highlighted by the gray regions. As SN 2023ixf evolved, the CO first-overtone feature, 2.2−2.5 μm, declined in strength, and a strong IR excess developed in the NIR continuum above ∼1.2 μm, corresponding to hot dust.
Paper: JWST Observations of SN 2023ixf. II. The Panchromatic Evolution between 250 and 720 Days after the Explosion
Authors: K. Medler, C. Ashall, P. Hoeflich, E. Baron, J. M. DerKacy, M. Shahbandeh, T. Mera, C. M. Pfeffer, W. B. Hoogendam, D. O. Jones, S. Shiber, E. Fereidouni, O. D. Fox, J. Jencson, L. Galbany, J. T. Hinkle, M. A. Tucker, B. J. Shappee, M. E. Huber, K. Auchettl, C. R. Angus, D. D. Desai, A. Do, A. V. Payne, J. Shi, M. Y. Kong, S. Romagnoli, A. Syncatto, C. R. Burns, G. Clayton, M. Dulude, M. Engesser, A. V. Filippenko, S. Gomez, E. Y. Hsiao, T. de Jaeger, J. Johansson, K. Krisciunas, S. Kumar, J. Lu, M. Matsuura, P. A. Mazzali, D. Milisavljevic, N. Morrell, R. O'Steen, S. Park, M. M. Phillips, A. P. Ravi, A. Rest, J. Rho, N. B. Suntzeff, A. Sarangi, N. Smith, M. D. Stritzinger, L. Strolger, T. Szalai, T. Temim, S. Tinyanont, S. D. Van Dyk, L. Wang, Q. Wang, R. Wesson, Y. Yang, S. Zsíros
Figure caption: The optical spectral time series of SN 2023ixf used in this work. All spectra have been corrected for redshift and extinction. The phase relative to the explosion date is given for each spectrum on the right. The emission regions of the Hα, Hβ, and Hγ lines are highlighted by the blue regions.
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for crystalline water ice between laboratory experiments (symbols) and Equation (1) with m = 5 (solid lines) or m = 6 (dotted lines) for ice Ih (r0 = 138 pm, γ = 0.208 J m−2). Upper left: nonporous (ϕ ≈ 1.0) ice under uniaxial tensile tests (circle) by H. H. G. Jellinek (1957), I. Hawkes & M. Mellor (1972), E. M. Schulson et al. (1984), A. M. A. Mohamed & M. Farzaneh (2011), and S. Huang et al. (2023), three-point bending tests (square) by M. Kermani et al. (2008), and the Brazilian disk test (diamond) by M. Mellor & I. Hawkes (1971), K. L. Litwin et al. (2012), and X. Lou & Y. Wu (2021); upper right: porous (ϕ ∼ 0.9) ice under the Brazilian disk test (square) by K. Hiraoka et al. (2008) and K. L. Litwin et al. (2012); middle left: porous (ϕ = 0.60) ice measured by Y. Shimaki et al. (2011) with the Brazilian disk test; middle right: highly porous (ϕ = 0.30–0.59) ice under uniaxial tensile tests by Y. Shimaki & M. Arakawa (2021); lower left: porous ice under the Brazilian disk test (square) by K. L. Litwin et al. (2012); lower right: freshwater ice using flat jack tests (triangle) by J. P. Dempsey et al. (1999), Brazilian disk tests (square) by J. Zhang et al. (2022), cantilever tests (inverted triangle) by G. E. Frankenstein (1959), A. J. Gow et al. (1978), G. W. Timco & R. M. W. Frederking (1982), R. M. W. Frederking & G. W. Timco (1983), and M. Karulina et al. (2019), three-point bending tests (diamond) by G. E. Frankenstein (1959), A. J. Gow (1977),G. W. Timco & R. M. W. Frederking (1982), S. Tozawa & Y. Taguchi (1986), and B. L. Parsons et al. (1992), and four-point bending tests (circle) by G. W. Timco & R. M. W. Frederking (1982), J. P. Dempsey et al. (1988), A. Murdza et al. (2020, 2022), and D. Edington et al. (2025).
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for nonporous silica glass between MD simulations (symbols) and Equation (1) with m = 8 (solid lines) for amorphous silica (r = 81 pm, γ = 0.243 J m−2). Upper left: the BMHB potential by T. F. Soules (1985), R. Ochoa & J. H. Simmons (1985), R. Ochoa et al. (1991), T. P. Swiler et al. (1995), S. Ito et al. (2012), and Z. Zhang et al. (2020b) and Equation (1) with γ = 0.67 J m−2 (dotted line); upper right: the (m-)BKS potentials by E. C. C. M. Silva et al. (2006), K. Muralidharan et al. (2007), F. Yuan & L. Huang (2012, 2014), C. Tang & L. P. Dávila (2014, 2015), J. Luo et al. (2016), W. Gonçalves et al. (2018), Z. Zhang et al. (2020b), and Z.-Q. Hu et al. (2021) and Equation (1) with γ = 0.74 J m−2 (dotted line); middle left: the PMMCS potential by A. Pedone et al. (2008, 2015), Q. Liu et al. (2014), and Equation (1) with γ = 0.383 J m−2 (dotted line); middle right: the VKRE potential by J. S. Rivas Murillo et al. (2008, 2010), J. Luo et al. (2016), F. Ebrahem & B. Markert (2017), F. Ebrahem et al. (2018), J. Zhang (2018), and Q. Wu & Z. Wang (2025); lower left: the ReaxFF potential by C. Zhang et al. (2015), S. C. Chowdhury et al. (2016, 2019), T. Hao & Z. M. Hossain (2019), T. Vo et al. (2020), J. Park & K. Kirane (2021), C. Zhang et al. (2023), and E. Bryski & K. Kirane (2025) and Equation (1) with γ = 0.641 J m−2 (dotted line); lower right: the Tersoff potential by J. Wang et al. (2015), K. Sun et al. (2020a), and Equation (1) with γ = 1.43 J m−2 (dotted line).