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Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Combined ENA flux maps for 2009–2022, as in Figure 5, but including survival probability as well as C-G corrections.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: C-G corrected IBEX ENA A maps.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: ENA A flux maps, including both survival probability and C-G corrections.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same as Figure 7, but for ENA B maps.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Average spectral index over ENA energies from ∼0.5–6 keV (FWHM) for 2009–2022, in the spacecraft reference frame. The top 14 rows show yearly fits and the bottom, a fit to all data averaged over all 14 yr.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same as Figure 14, but including survival probability corrections.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same data as Figure 12, but centered oppositely—on the downwind direction. The north/south and port/starboard lobes of the heliotail (McComas et al. 2013b) are clearly evident.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Mollweide projection of the ENA fluxes combined over 14 yr, centered on the upwind Ribbon direction (218.°33, 40.°38 in ecliptic J2000, from Dayeh et al. 2019). Lines indicate the ecliptic plane and approximate boundary of the Ribbon.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Statistically combined ram maps in the spacecraft frame for years 2009–2022.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Similar to Figure 17, but centered in the opposite direction, that is, pointing in the tailward hemisphere, in a direction 180° away from the Ribbon center.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Similar to Figure 19, but rebinned directly into equatorial J2000 coordinates. This projection is somewhat similar to the standard IBEX maps, but the north pole has been rotated to be parallel to the Earth's rotation axis and the map is centered on the vernal equinox.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Mollweide projection of the 14 yr combined ENA fluxes rebinned into Galactic coordinates. This projection shows maps from the perspective of a Sun-centered observer with the Mollweide projections centered on the Galactic center.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Similar to Figure 12, but for combined anti-ram maps.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: The computational performances of KM2 simulations using the reordered matrix with SIMD operations enabled are plotted as function of arithmetic intensity. Additionally, the plus symbol represents the computational performance of a reference model using KROME with the -useCustomCoe option. The horizontal line represents the peak performance of double-precision floating-point operations, and the diagonal lines represent the bandwidth of memory and the first-level, second-level, and third-level caches on our computing node.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Execution times of simulations with COO, CCS, CRS, and SELL formats in serial. Error bars represent the standard errors of execution times. The dashed and dotted lines represent execution times of a reference model using the KROME code with SIMD operations and the -useCustomCoe option, and a simulation using the default KROME settings, respectively.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Execution times of simulations parallelized by domain decomposition as a function of OpenMP threads. The solid, dashed, dashed–dotted, and dotted lines represent the COO, CCS, CRS, and SELL formats, respectively.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Execution times of simulations as a function of OpenMP threads, for a chemical-loop parallelization. The solid, dashed, dashed–dotted, and dotted lines represent COO, CCS, CRS, and SELL formats, respectively. Error bars represent standard errors.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Execution times of simulations parallelized by domain decomposition as a function of OpenMP threads. The solid, dashed, dashed–dotted, and dotted lines represent the COO, CCS, CRS, and SELL formats, respectively. Simulations performed on the machine Kawas were able to efficiently run 128 threads on each of its nodes.
Paper: A Nonparametric Reconstruction of the Hubble Parameter H(z) Based on Radial Basis Function Neural Networks
Authors: Jian-Chen Zhang, Yu Hu, Kang Jiao, Hong-Feng Wang, Yuan-Bo Xie, Bo Yu, Li-Li Zhao, Tong-Jie Zhang, 同杰 张
Figure caption: Reconstructed errors of the observational H(z) with linear regression. The solid red dots represent the observational error of H(z).The heuristic bounds σ + and σ − are plotted as the two solid green lines. The dashed line shows the estimated mean uncertainty σ  z .
Paper: A Nonparametric Reconstruction of the Hubble Parameter H(z) Based on Radial Basis Function Neural Networks
Authors: Jian-Chen Zhang, Yu Hu, Kang Jiao, Hong-Feng Wang, Yuan-Bo Xie, Bo Yu, Li-Li Zhao, Tong-Jie Zhang, 同杰 张
Figure caption: Structure of the RBFNN.
Paper: A Nonparametric Reconstruction of the Hubble Parameter H(z) Based on Radial Basis Function Neural Networks
Authors: Jian-Chen Zhang, Yu Hu, Kang Jiao, Hong-Feng Wang, Yuan-Bo Xie, Bo Yu, Li-Li Zhao, Tong-Jie Zhang, 同杰 张
Figure caption: The reconstructed functions of observational H(z) (solid blue curve) and its corresponding 1σ error with RBF networks (a). Comparison between the reconstructed Ω m  values using the RBF network based on simulated OHD data and the ΛCDM (Ω m  = 0.326)(b). In panel (a), the green dots with error bars represent the simulated H(z) data and the corresponding 1σ error, while the orange curve corresponds to the fiducial flat ΛCDM model with H 0 = 67.824 km s−1 Mpc−1 and Ω m  = 0.326. In the left panel, the shaded regions illustrate the reconstruction errors associated with both the ΛCDM model and the RBFNN model when using observational H(z) data, while the right panel portrays the propagation error.
Paper: A Nonparametric Reconstruction of the Hubble Parameter H(z) Based on Radial Basis Function Neural Networks
Authors: Jian-Chen Zhang, Yu Hu, Kang Jiao, Hong-Feng Wang, Yuan-Bo Xie, Bo Yu, Li-Li Zhao, Tong-Jie Zhang, 同杰 张
Figure caption: The reconstructed functions of mock H(z) (solid blue curve) and its corresponding 1σ error with RBF networks (a). The green dots with the error bars represent the simulated H(z) data and the corresponding 1σ error, while the orange curve corresponds to the fiducial flat ΛCDM model with H 0 = 67.824 km s−1 Mpc−1 and Ω m  = 0.326. In the left panel, the shaded regions illustrate the reconstruction errors associated with both the ΛCDM model and the RBFNN model when using simulated H(z) data, while the right panel portrays the propagation error.
Paper: A Nonparametric Reconstruction of the Hubble Parameter H(z) Based on Radial Basis Function Neural Networks
Authors: Jian-Chen Zhang, Yu Hu, Kang Jiao, Hong-Feng Wang, Yuan-Bo Xie, Bo Yu, Li-Li Zhao, Tong-Jie Zhang, 同杰 张
Figure caption: Comparison of the results from reconstructing OHD data using different methods.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Ram maps in the spacecraft frame, including survival probability corrections, showing the Ribbon median separation values of GDF ENA fluxes for all five energies and 14 yr of observations.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Comparison of Ribbon lower (2), Ribbon median (3), and Ribbon upper (4) estimates in both GDF and Ribbon maps plus bounding fluxes, including uncertainties (1 and 5), for the three new years of data (2020–2022). Data are from the ∼0.7 keV energy band ram maps in the spacecraft frame and are survival probability corrected.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same as Figure 27, but anti-ram maps of the Ribbon median GDF fluxes.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Procedure for calculating Ribbon median, lower, and upper separated maps of GDF and Ribbon fluxes. Statistical estimations follow Beesley et al. (2023), but include ensembling across 84 (28 × 3) separations (see text). Lower and upper maps are the pixelwise minimum and maximum of the 84 total separations performed for each map.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Ram maps in the spacecraft frame, including survival probability corrections, showing the Ribbon median separation values of Ribbon ENA fluxes for all five energies and 14 yr of observations.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: The same as for Figure 22, but for the ∼4.3 keV ENA energy channel.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: The same as for Figure 22, but for the ∼1.7 keV ENA energy channel.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: The same as for Figure 22, but for the ∼2.7 keV ENA energy channel.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: The same as for Figure 22, but for the ∼1.1 keV ENA energy channel.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same as for Figure 33, but showing differences of each year Ribbon median separated Ribbon flux ram maps from the exposure time average of the full 14 yr of data.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Difference maps of the Ribbon median separated GDF fluxes in the spacecraft frame, including survival probability corrections, for each year compared to the prior year.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Difference maps of the Ribbon median separated Ribbon fluxes in the spacecraft frame, including survival probability corrections, for each year compared to the prior year. Color bars are the same as for the GDF in Figure 31.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Difference of each year Ribbon median separated GDF flux ram maps in the spacecraft frame, including survival probability corrections, from the exposure time, averaged maps of the full 14 yr of data for that energy bin.
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Survival probabilities for 0.7 (solid), 1.1 (dotted), and 4.3 (dashed) keV H ENAs in the polar (A) and in the in-ecliptic (B) IBEX pixels; energy-dependent total ionization rates for H ENAs in the polar directions and in the ecliptic plane at 1 au (C), and the total flux in the solar Lyα line (D). The occasional jitter in the survival probabilities between 2014 and 2017, visible in the top panel, results from specific variations of the spacecraft spin axis.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Orders in which nonzero elements are calculated in CCS, CRS, and SELL formats.
Paper: An Efficient Algorithm for Astrochemical Systems Using Stoichiometry Matrices
Authors: Kazutaka Motoyama, Ruben Krasnopolsky, Hsien Shang, Kento Aida, Eisaku Sakane
Figure caption: Distributions of nonzero elements in a stoichiometry matrix without row reordering (a) and with row reordering (b).
Paper: Fourteen Years of Energetic Neutral Atom Observations from IBEX
Authors: D. J. McComas, M. Alimaganbetov, L. J. Beesley, M. Bzowski, H. O. Funsten, P. H. Janzen, M. A. Kubiak, J. S. Rankin, D. B. Reisenfeld, N. A. Schwadron, J. R. Szalay
Figure caption: Same as Figure 29, but anti-ram maps of the Ribbon fluxes from the Ribbon median separations.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the nonrotating models. Top to bottom: Z, F, E. The x-axis represents the time prior the collapse of the Fe core, marked as t final in the plot. The blue area marks the H-rich layers, the red one the pure He zone, the cyan the C/O region, the magenta the Ne/O region, the violet the O-rich layers, the green area the Si-rich zones while the brown zone the Fe core. The yellow area marks the convective zones.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Evolution on the Hertzsprung–Russell (H-R) diagram of 15 (left panels) and 25 M ⊙ (right panels) rotating massive stars. The different colors indicate the various initial equatorial velocity. The filled symbols mark different evolutionary stages.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Ratio of surface angular velocity to critical velocity in the 15 M ⊙ (left panels) and 25 M ⊙ stars (right panels) in Set Z (first row), Set F (second row), and Set E (third row) for four characteristic central H abundances in mass fraction: initial (red), 0.3 (yellow), 10−2 (green), and 10−6 (blue).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: The total angular momentum J at the onset of the main-sequence phase in all the computed models. Diamonds represent 15 M ⊙ models; dots represent 25 M ⊙ models.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 25 M ⊙ models of [Fe/H] = −5. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 25 M ⊙ zero metallicity models. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption:  12C abundance in mass fraction at the central He depletion as a function of the initial equatorial rotation velocity in the 15 (top panel) and 25 M ⊙ cases (bottom panel).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: He core mass in the 15 (top panel) and 25 M ⊙ models (bottom panel) at central He ignition (filled dots) and exhaustion (filled diamonds).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: CO core mass at central He depletion in the 15 (top panel) and 25 M ⊙ models (bottom panel).
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 25 M ⊙ models of [Fe/H] = −4. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Kippenhahn diagrams of the rotating 15 M ⊙ zero metallicity models. The color coding is the same as in Figure 2.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Nuclide chart.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Comparison of the sum of all the yields above Ge between the models computed in this work and the ones presented in Frischknecht et al. (2016) for [Fe/H] = −4.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Comparison between the models computed in this work and the ones presented in Frischknecht et al. (2016) for [Fe/H] = −4.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Same as Figure 30 but for the 25 M ⊙ models.
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Upper panel: on the left side, the [Sr/Mg] ratio of sample of observations of stars with [Fe/H] ≤ −3.5 taken from JINAbase, and on the right side, our theoretical predictions. The horizontal dashed line shows the lowest observed [Sr/Mg] value of the sample. Lower panel: the same but for [Ba/Mg].
Paper: Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei
Authors: Lorenzo Roberti, Marco Limongi, Alessandro Chieffi
Figure caption: Left: [Sr/Ba] ratios in a sample of observations of stars with [Fe/H] ≤ −3.5 taken from JINAbase. Right: our theoretical predictions.