adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology and Dynamics Reveal Interior Structure and Coeval Evolution in the Triply Post-main-sequence System DG Leo
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Li-Ying Zhu, Jia Zhang, Qi-Bin Sun, Fang-Bin Meng
Figure caption: The light curves from four TESS sectors and their corresponding phase-binned light curves (green circles) are overplotted with the best-fitting model (red solid curves; W-D Model 2). Residuals are shown in the bottom panel for each sector.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The local LF of Fermi FSRQs, de-evolved at z = 0. The blue points are the calculated values from the ﹩1/{V}_{{\rm{\max }}}﹩ method. The pink hatched area is the ±1σ uncertainty of the LF. The total uncertainty is shaded in gray. The total uncertainty is calculated by combining the statistical (1σ uncertainty) and systematic uncertainties (see Section 3.5). The red line depicts the best-fit line of the local LF.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The space density of Fermi FSRQs in the intermediate-luminosity range: ﹩\mathrm{log}{L}_{\gamma }﹩ (erg s−1) = 45.8–47.2. The best-fit line of our model is represented by the blue line, surrounded by the 1σ uncertainty region, shaded in the pink hatched pattern, and the total uncertainty, shaded in gray. The green dashed–dotted line shows the space density of BL Lacs obtained using the best-fit model and parameters from M. Ajello et al. (2014), within the same intermediate-luminosity range.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The space density of Fermi FSRQs in the low-luminosity range: ﹩\mathrm{log}{L}_{\gamma }﹩ (erg s−1) = 43.5–45.6. The best-fit line of our model is represented by the blue line, surrounded by the 1σ uncertainty region, shaded in the pink hatched pattern, and the total uncertainty, shaded in gray. The green dashed–dotted line shows the space density of BL Lacs obtained using the best-fit model and parameters from M. Ajello et al. (2014), within the same low-luminosity range.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The space density of Fermi FSRQs in the high-luminosity range: ﹩\mathrm{log}{L}_{\gamma }﹩ (erg s−1) = 47.2–48.4. The best-fit line of our model is represented by the blue line, surrounded by the 1σ uncertainty region, shaded in the pink hatched pattern, and the total uncertainty, shaded in gray. The green dashed–dotted line shows the space density of BL Lacs obtained using the best-fit model and parameters from M. Ajello et al. (2014), within the same high-luminosity range.
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The space density of Fermi FSRQs. The best-fit line of our model is represented by the blue line, surrounded by the 1σ uncertainty region, shaded in the pink hatched pattern, and the total uncertainty, shaded in gray. The green dashed–dotted line shows the space density of FSRQs obtained using the best-fit parameters from M. Ajello et al. (2012).
Paper: The Gamma-Ray Luminosity Function of Flat-spectrum Radio Quasars
Authors: Garima Rajguru, L. Marcotulli, M. Ajello, M. Di Mauro, M. Urry
Figure caption: The luminosity density of Fermi FSRQs. The best-fit line of our model is represented by the blue line, surrounded by the 1σ uncertainty region, shaded in the pink hatched pattern, and the total uncertainty, shaded in gray. The green dashed–dotted line shows the luminosity density of FSRQs obtained using the best-fit parameters from M. Ajello et al. (2012).
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: The total flux of 3C 286 measured with ALMA in Band 3 (top) and Bands 6 and 7 (bottom). Filled circles without error bars represent the full data set. Larger highlighted circles with error bars indicate the average flux and the standard deviation at each frequency (Table 7), displayed at the median date of the corresponding period: Period I (MJD 58200–59000), Period II (MJD 59200–59900), and Period III (MJD > 60100). Shaded regions correspond to these three periods. Dashed horizontal lines indicate the mean flux values over the entire monitoring period.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: Total flux (top), fractional polarization (middle), and EVPA (bottom) of 3C 286 obtained with IRAM at 86 and 229 GHz and SMA at 225 GHz. The horizontal dotted lines represent the average values at each frequency. Note that the y-axis scales are identical to those in Figure 1.
Paper: Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-dependent Polarization Attributed to Core-shift
Authors: Minchul Kam, Hiroshi Nagai, Motoki Kino, Keiichi Asada, Rüdiger Kneissl, Iván Agudo, Sascha Trippe, Seiji Kameno, Ioannis Myserlis, Ramprasad Rao, Hojin Cho, Richard A. Perley, Bryan J. Butler, Mark Gurwell, Tomoki Matsuoka, Jongho Park, Carolina Casadio, Baltasar Vila Vilaro, Celia Verdugo, Matias Radiszcz, Kurt Plarre, Wanchaloem Khwammai, Diego Álvarez-Ortega, Juan Escudero, Clemens Thum, Garrett Keating
Figure caption: Total flux (top), fractional polarization (middle), and EVPA (bottom) of 3C 286 obtained with ALMA at 91.5, 103.5, 233.0, and 343.4 GHz. The horizontal dotted lines represent the average values at each frequency.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Example case illustrating the procedure used to develop MADCAT. Panels (a) and (b) show observations from COR2B and COR2A, respectively. On the coronagraph images we overlay the boundary of the CORSET mask (red dashed line) and the projection of a GCS reconstruction (blue dashed line). Panel (c) shows the location of the STEREO satellites relative to Earth, taken from the Solar-MACH webtool. The reference longitude indicates the CME direction. Panel (d) shows the reconstructed CME mass versus height using CORSET and four different GCS fits for both STA and STB.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: Migration of the coronal hole as seen in AIA 193 Å (top row) and AIA 171 Å (bottom row). The first column shows overview images from June 26 17:55. The coronal hole boundary from June 25 10:50, which we rigidly rotated with the solar surface to 17:55, is outlined in blue. This boundary corresponds to the initial location of the coronal dimming at the solar surface. The coronal hole boundary from June 26 17:55 is outlined in red. This boundary corresponds to the location where the coronal hole eventually stabilized. A slice in the migration direction is marked in white. The second column shows the temporal evolution of AIA intensities along the slice, describing the migration of the coronal hole.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Comparison of masses reconstructed from different viewpoints for the same CME. The top panels show scatter plots of the mass in STB versus STA for the CORSET (left) and GCS (right) events. We include black and gray dashed lines showing ratios of 1, 1.5, 2, 3, and 4 between the two different masses. The bottom panels show histograms of the probability density of the weighted mass differences along with a best-fit skew normal distribution in black. The colored distribution line shows the profile from the adjacent panel for comparison.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Diagram showing the general algorithm used within this work. The yellow box at the top shows the standard coronagraph image processing that we perform before we calculate masses using either the CORSET (light gray) or GCS (dark gray) information. Within the larger boxes, white boxes indicate numerical routines, black boxes indicate inputs, dark gray boxes indicate intermediate data products, and colored circles indicate output results.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Reconstructed CME mass versus time. The top panel shows CORSET results (CORSET A in red and B in blue) and the second panel shows GCS results (A in maroon and B in light blue). The third panel shows the masses for the full CDAW catalog (dark gray) and for a subset of larger events (CDAW*, light gray) more comparable to the events in the top two panels. The bottom panel shows the median values for each data set using the same colors as the scatter plots.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: Same as Figure 4, but derived from the wider coronal hole boundaries.
Paper: Formation of a Coronal Hole by a Quiet-Sun Filament Eruption
Authors: Stefan J. Hofmeister, Eleanna Asvestari, Karin Dissauer, Michael Hahn, Stephan G. Heinemann, Veronika Jercic, Alexandros Koukras, Kilian Krikova, Jonas Saqri, Daniel W. Savin, Manuela Temmer, Astrid Veronig
Figure caption: Additional coronal holes likely formed by filament eruptions. All panels display AIA 193 Å observations. First column: overview images showing filament channels, with the field of view for the second column marked in white. Second column: zoom-in on the filaments, indicated by blue arrows. Third column: same field of view at the next solar rotation. The filaments have now disappeared, and coronal holes (red arrows) have formed. Fourth column: overview images at the times of the coronal holes.
Paper: New Measures of STEREO CME Masses and Directions
Authors: C. Kay, A. Vourlidas, L. A. Balmaceda
Figure caption: Comparison of masses reconstructed using different methods for each viewpoint in a similar format to Figure 4. The scatter plots show the GCS mass versus the CORSET mass for STA (left) and STB (right).
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Reconstruction of the whitened deviation strain δs for GW190916_200658 residual data. The blue curve is the whitened residual strain in each detector. The black curve is the median estimate of δs using Gaussian process regression for the maximum-likelihood estimate of the GR waveform parameters θ, and the gray shaded region is the 90% credible interval on δs for this estimate. The orange shaded region is the 90% credible interval on δs marginalized over the uncertainty in θ.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Rest-frame U − V vs. V − J colors (i.e., UVJ diagram) of galaxies in the DJA photometry catalog. Red solid lines are selection criteria for quiescent galaxies adopted from R. J. Williams et al. (2009). We extend our selection in the highest redshift bin (dashed red line) to include recently quenched galaxies, following Z. Mao et al. (2022). The sample selected with this extended quiescent box is used only in Sections 4.3 and 5.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Curves of growth for the PSFs from primer-uds-south-grizli-v7.2 in each filter (blue), compared to the target PSF used for PSF matching (F444W; black dotted line). The red curves show the PSFs after convolution with the constructed kernels, demonstrating how closely they match the target PSF.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution of the Gaussian process hyperparameters for GW190916_200658 residual data. The contours are the 1σ, 2σ, and 3σ intervals. Shown in black are the posteriors for the initial maximum-likelihood estimate run for the GR waveform parameters θ, and shown in orange are the reweighted posteriors, taking into account the uncertainty in θ.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Reconstruction of the whitened deviation strain δs for GW150914 residual data. The blue curve is the whitened residual strain in each detector. The black curve is the median estimate of δs using Gaussian process regression, and the gray shaded region is the 90% credible interval on δs, which shows no signal is present in the data.
Paper: Stellar Mass Assembly History of Massive Quiescent Galaxies since z ∼ 4: Insights from Spatially Resolved Spectral Energy Distribution Fitting with JWST Data
Authors: Novan Saputra Haryana, Masayuki Akiyama, Abdurro'uf, Hesti Retno Tri Wulandari, Juan Pablo Alfonzo, Kianhong Lee, Naoki Matsumoto, Ryo Albert Sutanto, Muhammad Nur Ihsan Effendi, Itsna Khoirul Fitriana, Ibnu Nurul Huda, Anton Timur Jaelani, Sultan Hadi Kusuma, Lucky Puspitarini, Dian P. Triani
Figure caption: Stellar mass and redshift of quiescent galaxies with zphot < 4. Gray, red, and blue points show all quiescent galaxies, massive quiescent galaxies (﹩{\mathrm{log}}({M}_{* }/{M}_{\odot })\gt 11﹩), and the massive quiescent galaxies with confirmed spectroscopic redshift, respectively.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distribution of the Gaussian process hyperparameters for GW150914 residual data. The contours are the 1σ, 2σ, and 3σ intervals. The posterior on k0 does not exclude the lower bound of 10−46, indicating no signal is present in the data.
Paper: A Gaussian Process Framework for Testing General Relativity with Gravitational Waves
Authors: Lachlan Passenger, Shun Yin Cheung, Nir Guttman, Nikhil Kannachel, Paul D. Lasky, Eric Thrane
Figure caption: Comparison between the log-signal-to-noise Bayes factor ﹩{\mathrm{ln}}{ \mathcal B }﹩ distributions for 174 noise segments (blue) and the 60 GWTC-3 GW events (orange) analyzed.
Paper: Living with Neighbors. VI. Unraveling the Dual Impact of Bars on Star Formation in Paired Galaxies Using DESI
Authors: Woong-Bae G. Zee, Suk-Jin Yoon
Figure caption: Top: normalized distributions of the redshift (left), stellar mass (middle), and local density (right) for paired galaxies (purple) and initial, unmatched sample of isolated, unbarred galaxies (dashed gray). Bottom: same as the top panels, but comparing the matched sample of paired galaxies (purple) to the final control sample of isolated, unbarred galaxies (solid gray). The p-values from the K-S test confirm the statistical consistency between the matched samples, validating the effectiveness of our control selection. Black error bars on the histograms represent Poisson uncertainties for the control sample.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: The left panels show the light curves for nonvariable white dwarfs in our sample. The right panels show the corresponding Fourier transforms with the observation date labeled on top. The dashed black lines mark the 4〈A〉 detection limits, which are listed in Table 7.
Paper: Living with Neighbors. VI. Unraveling the Dual Impact of Bars on Star Formation in Paired Galaxies Using DESI
Authors: Woong-Bae G. Zee, Suk-Jin Yoon
Figure caption: Example DESI-LS multiband images of galaxy pairs in which the target galaxy hosts a stellar bar. For each system, we indicate the normalized bar length (LBar/D25) and the projected separation between the target and its companion (rNei). The target barred galaxy is marked with a white arrow in each panel.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves and Fourier transforms for J0408+2323.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves and Fourier transforms for J0657+7341.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curve and Fourier transform for J2208+2059.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curve and Fourier transform for J2026−2254.
Paper: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Authors: Hiroshi Kimura, ヒロシ キムラ, Takaya Okamoto, Takayuki Hirai, Fumi Yoshida, Peng K. Hong, Koji Wada, Tomoko Arai, Eiichiro Kokubo, Yuki Yoshida, Toshihiko Kadono, Sota Arakawa, Hiroki Senshu, Masanori Kobayashi, Ko Ishibashi, Manabu Yamada, Hiroshi Akitaya, Osamu Okudaira, Takafumi Matsui
Figure caption: The constant of proportionality, σr0/γ, for the van der Waals (vdW) interaction (dotted line) and σ in Equation (19) normalized to γ/r0 (solid line) as a function of volume-filling factor ϕ.
Paper: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Authors: Hiroshi Kimura, ヒロシ キムラ, Takaya Okamoto, Takayuki Hirai, Fumi Yoshida, Peng K. Hong, Koji Wada, Tomoko Arai, Eiichiro Kokubo, Yuki Yoshida, Toshihiko Kadono, Sota Arakawa, Hiroki Senshu, Masanori Kobayashi, Ko Ishibashi, Manabu Yamada, Hiroshi Akitaya, Osamu Okudaira, Takafumi Matsui
Figure caption: The elastic modulus E* for aggregate particles consisting of silica spheres as a function of the volume-filling factor ϕ at r0 = 0.025 μm (left) and the monomer radius r0 at ϕ = 0.55 (right). Open circles: experimental results of K. Kendall et al. (1987a); solid curves: Equation (6) with m = 8.
Paper: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Authors: Hiroshi Kimura, ヒロシ キムラ, Takaya Okamoto, Takayuki Hirai, Fumi Yoshida, Peng K. Hong, Koji Wada, Tomoko Arai, Eiichiro Kokubo, Yuki Yoshida, Toshihiko Kadono, Sota Arakawa, Hiroki Senshu, Masanori Kobayashi, Ko Ishibashi, Manabu Yamada, Hiroshi Akitaya, Osamu Okudaira, Takafumi Matsui
Figure caption: The ratio of ﹩{\sigma }_{\max }﹩ to ﹩\sqrt{E\gamma /{d}_{0}}﹩ for ideal crystals with the Lennard–Jones 12-6 potential as a function of volume-filling factor ϕ.
Paper: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Authors: Hiroshi Kimura, ヒロシ キムラ, Takaya Okamoto, Takayuki Hirai, Fumi Yoshida, Peng K. Hong, Koji Wada, Tomoko Arai, Eiichiro Kokubo, Yuki Yoshida, Toshihiko Kadono, Sota Arakawa, Hiroki Senshu, Masanori Kobayashi, Ko Ishibashi, Manabu Yamada, Hiroshi Akitaya, Osamu Okudaira, Takafumi Matsui
Figure caption: The elastic modulus E* (left) and the fracture energy R* (right) normalized to ﹩{[{E}^{2}{(1-{\nu }^{2})}^{-2}\gamma {r}_{0}^{-1}]}^{1/3}﹩ and ﹩{[{E}^{-2}{(1-{\nu }^{2})}^{2}{\gamma }^{5}{r}_{0}^{-2}]}^{1/3}﹩, respectively, as a function of the volume-filling factor ϕ. Open squares: analytical model for aggregate particles of spheres in regular packings by K. Kendall et al. (1986, 1987a) and K. Kendall (1987); open circles: analytical models for aggregate particles of spheres in regular packings by C. Thornton (1993) on the left and by K. Kendall et al. (1986) times (3/13)1/3 on the right; solid curves: Kendal’s approximation of ϕ4 dependences (K. Kendall et al. 1986; K. Kendall 1987, 1988, 2001); dashed curves: Equations (6) and (7).
Paper: Mechanical Properties of Dust, Pebbles, and Planetesimals Based on Johnson–Kendall–Roberts, Griffith, and Weibull Theories
Authors: Hiroshi Kimura, ヒロシ キムラ, Takaya Okamoto, Takayuki Hirai, Fumi Yoshida, Peng K. Hong, Koji Wada, Tomoko Arai, Eiichiro Kokubo, Yuki Yoshida, Toshihiko Kadono, Sota Arakawa, Hiroki Senshu, Masanori Kobayashi, Ko Ishibashi, Manabu Yamada, Hiroshi Akitaya, Osamu Okudaira, Takafumi Matsui
Figure caption: The elastic modulus E* experimentally (open circles) and numerically (crosses) determined for amorphous silica (left) and water ice (right) as a function of the volume-filling factor ϕ in comparison to our formula (solid curves) given in Equation (6). The right axis of each panel denotes the bulk sound velocity C0, which corresponds to the elastic modulus E* on the left axis, in relation to ﹩{C}_{0}\equiv \sqrt{{E}^{* }(1-{\nu }^{2})/[3(1-2\nu )\rho \phi ]}﹩.