adsabs/AstroCLIMB huggingface dataset:
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Comparison of I Zw 18 H2 population diagrams with Meudon PDR-7 isobaric models. As for the isochoric models, the visual extinction AV was fixed to have a maximum of unity; only the models that best approximate the observed data are shown. Further constraints are discussed in the main text (Section 3.5).
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Left panel: Comparisons of the H2 column Ntot and H2 total mass inferred from fits at different Tu, and also with and without fitting the OPR. The left-hand ordinate scale shows H2 column density, and the right H2 total mass within the apertures. Right panel: Comparison of OPR inferred from fits with different Tu. The open star shows the mean for each region. In the right panel, the horizontal dashed line indicates the maximum LTE value of OPR = 3.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Comparison of I Zw 18 H2 population diagrams with Meudon PDR-7 isochoric models. The visual extinction AV was fixed to have a maximum of unity; only the models with G0/nH ≤ 0.05 are shown since they best approximate the observed data. Further constraints are discussed in the text.
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: Schematic summary of our results. The figure illustrates the formation of oxygenated carbon chains, C3O2, C5O2, CCO, and CO2. Panel (a) represents the ideal situation in the ISM, with a low accretion rate of carbon atoms impinging the ice. Panel (b) shows the exemplification of the sequential deposition experiments at 10 K. Panel (c) shows the co-deposition experiments at 10–25 K. Pale green boxes represent molecules that are compatible with ISM dilution conditions, whereas gray boxes represent molecules that are less likely to occur in the ISM.
Paper: Formation of Unsaturated Carbon Chains through Carbon Chemisorption on Solid CO
Authors: Masashi Tsuge, Germán Molpeceres, Ryota Ichimura, Hideko Nomura, Kenji Furuya, Naoki Watanabe
Figure caption: (a) Schematic view for the simulated reaction profile for the formation of C3O2. (b) Suggested scheme for the formation of C5O2 in our experiments. ΔUR and ΔUa represent the reaction energies and activation energies, if any, of the elementary steps showcased in the diagram. All energies are shown in kcal mol−1.
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: Ejecta density (the first row), temperature (the second row), and Planck mean opacity (the third row) profiles along the representative lines. In each panel, the dashed, solid, and dotted lines correspond to H1_hd_0.1c (Σdisk = 1.7 × 105 g cm−2), H1_md_0.1c (Σdisk = 1.7 × 104 g cm−2), and H1_ld_0.1c (Σdisk = 1.7 × 103 g cm−2) at t = 12.4 minutes. 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 lines are sampled at simulation time 5.0 minutes since the star is at disk midplane. In each panel, the star data points are where τeff,P = c/v; triangle data points are where τeff,R = c/v.
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: Estimated total luminosity for the backward ejecta (upper panel) and the forward ejecta (lower panel). The blue, green, and red lines correspond to H1_hd_0.1c (Σdisk = 1.7 × 105 g cm−2), H1_md_0.1c (Σdisk = 1.7 × 104 g cm−2), and H1_ld_0.1c (Σdisk = 1.7 × 103 g cm−2). The time axis corresponds to the time since the star is at the disk midplane. For comparison, the Keplerian orbital period at the assumed collision radius is 8.6 hr. In each plot, the vertical dotted lines show the estimated diffusion timescale tdiff (Equation (3)). The dotted lines show fitting of power-law decay L ∝ t−β. In the lower panel, the gray shaded region marks the brief breakout emission. In the lower panel, the peak of the red line near t ≈ 10 minutes is due to the numerical effect of an angular discretized radiation field.
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: Estimated ejecta mass Mej from H1_hd_v0.1c (Σdisk = 1.7 × 105 g cm−2, blue), H1_md_v0.1c (Σdisk = 1.7 × 104 g cm−2, green), and H1_ld_v0.1c (Σdisk = 1.7 × 103 g cm−2, red). The time axis corresponds to the time since the star is at the disk midplane. For comparison, the Keplerian orbital period at the assumed collision radius is 8.6 hr. The solid lines show the Mej below the disk, corresponding to the forward ejecta. The dashed lines show Mej above the disk, corresponding to the backward ejecta. The dotted horizontal lines with color correspond to the estimation in Equation (1) for each simulation. The black solid line shows the power law Mej ∝ t1.7. The mass Mej is estimated from the two-dimensional simulation and is normalized by R⊙.
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: Upper panel: measured luminosity of backward ejecta (solid lines) and forward ejecta (dashed lines). We stop the luminosity curves when the ejecta expand beyond the simulation domain. The time axis is the time since the star crosses the disk midplane. Lower panel: normalized gas kinetic energy (solid lines) and radiation energy (dashed lines) for H1_md_0.15c (purple, v* = 0.15c), H1_md_0.1c (dark, v* = 0.1c), and H1_md_0.07c (orange, v* = 0.07c). The normalization factor corresponds to the estimated shocked gas kinetic energy in Equation (6). The time delay between the lower-panel radiation energy density peak and upper-panel luminosity peak is primarily due to the photon diffusion time from the shock front to the ejecta photosphere.
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: Effective diffusion timescale (Equation (7)) along the sampling line similar to Figure 6 in the forward ejecta for H1_hd_0.1c (Σdisk = 1.7 × 105 g cm−2, dashed lines), H1_md_0.1c (Σdisk = 1.7 × 104 g cm−2, solid lines), and H1_ld_0.1c (Σdisk = 1.7 × 103 g cm−2, dotted lines). The triangles label the location of ﹩{\tau }_{{\rm{tr}},{\rm{R}}}=c/v﹩; tdiff = 2.97 × 102 s, 5.78 × 103 s, and 1.4 × 103 s in H1_hd_v0.1c, H1_md_v0.1c, and H1_ld_v0.1c. The three triangles next to the left y-axis labels are the estimated diffusion time tdiff with κes (Equation (4)), from higher to lower they correspond to descending Σdisk.
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 radiation energy density snapshots from H0.3_md_v0.1c and H3_md_v0.1c. The white arrows show the normalized velocity field in the disk frame. In each snapshot, the three dashed cyan lines show the midplane of the disk and ±2Hdisk from the midplane. In the left plot (H0.3_md_v0.1c), the beamed pattern above the disk is due to the angular discretization of the radiation field in the numerical scheme in an extremely optically thin region, which is referred to as a “ray effect.”
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: Estimated timescale tff,th, which is the timescale to produce enough photons to establish a blackbody SED by free–free emission. Left is for the high surface density disk H1_hd_v0.1c, and right is for the low surface density disk H1_ld_v0.1c; the snapshot time is t = 5.0 minutes since the star is at disk midplane, corresponding to the third column in Figure 1.
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: Estimated luminosity of backward ejecta (upper panel) and forward ejecta (lower panel). The blue, black, and pink lines correspond to H0.3_md_0.1c (Hdisk = 0.3R*), H1_md_0.1c (Hdisk = R*), and H3_md_0.1c (Hdisk = 3R*). The dotted lines show power-law fittings (Equation (9)). The time axis is the time since the star is at the disk midplane.
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 snapshot from H0.3_md_v0.1c (left) and H3_md_v0.1c (right). We show the x- and y-axes in units of cm instead of normalized to Hdisk due to different disk scale heights.
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 comparison of SN 2023ixf with several SNe II observed at infrared wavelengths. All spectra have been corrected for redshift and extinction. To aid in comparison, the spectra of SN 2023ixf are continuum subtracted with blackbody functions of 850, 550, 360, and 300 K from the +252.67-, +373.52-, +600.21-, and +719.96-day data, respectively. Left: comparison of the NIR spectra, between 1.5 and 5.5 μm, of SN 1987A and SN 2023ixf. Right: comparison of the SN 2023ixf MIRI spectra with SN 1987A (D. H. Wooden et al. 1993), SN 2004dj (T. Szalai et al. 2011), SN 2004et (R. Kotak et al. 2009), and SN 2005af (R. Kotak et al. 2006). Both SN 1987A and SN 2004et were digitized from D. H. Wooden et al. (1993) and R. Kotak et al. (2009), 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: Evolution of the α (top), β (middle), and γ (bottom) transitions of the different hydrogen series located between 0.32 and 14.0 μm at +252.67 (blue), +373.52 (green), +600.21 (red), and 719.96 days (purple). Several of the isolated hydrogen emission lines, especially the α-transitions, show a triple-peaked profile consisting of a blueshifted peak (−1100 km s−1), a slightly redshifted peak (+500 km s−1), and a strongly redshifted shoulder (+2200 km s−1), shown by the vertical dashed blue, green, and red lines, respectively. Additional high-velocity components (shaded blue regions) emerge between + 252.67 and + 372.53 days, located between ±4000 and 8000 km s−1.
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: Evolution of the Hα profile from a blueshifted P Cygni−like feature at +72 days to an asymmetric multipeak feature at +761.97 days, with high-velocity components that emerge around +258.30 days. Earlier spectra are presented in Paper I. All spectra have been corrected for redshift and extinction and have been continuum subtracted. The blue, green, and red vertical lines denote the three shifted peaks located at ∼−1100, ∼600, and ∼2200 km s−1, respectively. The blue shaded regions highlight the emerging high-velocity hydrogen features.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Tracing the full ancestry of six leaves through several plots presented in this work. In panels (b)–(h), the six leaves are shown with ⋆ symbols, while their ancestors are traced with a colored line. In some cases, the full hierarchy is obscured by ancestries merging to a common progenitor. (a) Ancestries highlighted on the full dendrogram as in Figure 2. (b) Highlighted on the αvir−R relation as in Figure 4. (c)–(e) Highlighted on the relations of αvir against physical properties (mass, surface density, and velocity dispersion) as in Figure 5. (f)–(h) Highlighted on the relations of αvir against hierarchical properties (height, level, number of leaf descendants) as in Figure 6.
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 evolution of the SED covering 0.32−14.0 μm of SN 2023ixf from +252.67 to +719.96 days post-explosion. Photometry is shown by the colored symbols, at +301.72, +600.21, and +719.96 days. The data have been corrected for extinction and are presented in the rest frame. The SEDs are dominated by a large number of emission lines that decline in strength as SN 2023ixf evolves. CO molecule and dust features are highlighted. In addition, there is a strong IR excess that grows in strength relative to the SN flux at late times.
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: A stacked three-color image of the host galaxy spiral arm using the F770W, F1000W, and F1500W MIRI filters from epoch 301.72 days. The location of SN 2023ixf is highlighted by the light-blue circle.
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: Lines identified within the GB optical and NIR (top row), JWST NIRSpec G235M/F170LP (second row), G395/F290LP (third row), and MIRI (fourth row) spectra of SN 2023ixf at ∼250 days (blue), ∼373 days (green), ∼600 days (red), and ∼720 days (purple) post-explosion. The spectra have been vertically shifted for clarity. The CO first-overtone and fundamental bands are shown by the shaded blue regions. The full list of identified lines is given in Tables 3 and 4.
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 evolution of the Hα, Paα, and Brα emission features. All features have been continuum subtracted and normalized to the flux at 0 km s−1. No wavelength-dependent attenuation of the redshifted flux is observed at a given epoch, although a temporal-dependent attenuation is visible.
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 diamond between laboratory experiments (symbols) and Equation (1) with m = 6 (solid line) for nonporous (ϕ = 1.0) diamond (r = 77 pm, γ = 9.30 J m−2). Upper left: monocrystalline diamond (m-DIA) under uniform bending test (square) by A. Banerjee et al. (2018) and A. Nie et al. (2019), and uniaxial tensile test (circle) by C. Dang et al. (2021); upper right: polycrystalline diamond (p-DIA) produced with CVD methods and applied a tensile stress to the coarse-grained side of transparent (open circles) and dark (open diamonds) samples and the fine-grained side of transparent (open triangles) and dark (open squares) samples by T. E. Steyer et al. (1995), A. Hirata et al. (1997), K. L. Jackson et al. (1997), S. Takeuchi et al. (2001), C. S. J. Pickles (2002), A. R. Davies & J. E. Field (2004), A. R. Davies et al. (2005), V. G. Ralchenko et al. (2012), and M. A. Lodes et al. (2015); bottom: polycrystalline diamond films under uniform bending tests by M. Mohr et al. (2014).
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Logarithmic snapshots of the disk surface density Σ/Σ0 across a range of binary semimajor axes (columns) and viscosities (rows). The left-most panels illustrate the disk structure following the viscous relaxation period of 1000 binary orbits—preceding the onset of a gravitational wave inspiral. As the inspiral progresses, the semimajor axis of the binary decreases (right) and the disk reacts, primarily through a shrinking central cavity. Decoupling happens earlier for less viscous disks (top) while the intrabinary bridge is more stable for larger viscosities (bottom).