adsabs/AstroCLIMB huggingface dataset:
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Radial distributions of (a) the dust and gas surface densities, (b) the vertically integrated gas pressure, and (c) its radial gradient at 510 kyr. The lines show the azimuthally averaged values, and the shaded regions represent the range between the maximum and minimum values. In panel (a), the colors depict different components: dust (green) and gas (orange). The dust density is multiplied by 1000 to facilitate easier comparison. In panel (c), the red solid line depicts negative gradients, and the blue dashed line indicates positive gradients. The dashed–dotted vertical lines mark the positions of two examples of dust density peaks, at 50 au (black) and 120 au (gray), among several observed. In panel (a), the blue dotted line represents the fitting function for the gas density, given by ﹩80{\left(r/20\,{\rm{au}}\right)}^{-1.7}﹩ g cm−2, which is used in Section 4.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Disk evolution during the first 300 kyr (early phase). The top, middle, and bottom rows show the two-dimensional distributions of the surface density of gas, that of dust, and the maximum dust size at three different epochs, 20, 130, and 300 kyr after the disk formation. The dust density is the sum of grown and small dust densities. In each panel, the white contour line delineates an isosurface density of 0.3 g cm−2, indicating the approximate location of the outer edge of the disk.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Multiple dust ring formation in the late phase. Each column displays the spatial distributions of the surface densities of dust (upper) and gas (lower) at four different periods, 410, 460, 510, and 750 kyr from left to right.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Gas surface density ratio between the simulation results and the fitting function shown in Figure 5(a), given by ﹩80{\left(r/20\,{\rm{au}}\right)}^{-1.7}﹩ g cm−2. The panels represent the snapshot at the same epoch of 510 kyr in the three different simulations: (a) the fiducial, (b) high-α-viscosity, and (c) inviscid runs. In each panel, the blue regions indicate areas of relatively higher surface density compared to their surroundings, while the red regions indicate areas of relatively lower density.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Evolution of the gas mass distribution up to the end of the fiducial run. The lines represent three different components: the envelope (solid), the central star (dashed), and the disk (dotted).
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Spatial distributions of the dust and gas surface densities in the run with high turbulent viscosity of α = 10−3 at three different epochs, 410, 460, and 510 kyr, shown in the three columns on the left. In the rightmost column, the spatial distributions in the fiducial run with the viscosity of α = 10−4 are displayed.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Radial profiles of the dust surface density at 510 kyr in the fiducial (solid) and high-α-viscosity (dashed) runs.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: The same as Figure 6, but for the inviscid run.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Top: reduced GMOS spectra of EELG1002 highlighting multiple emission line detections securing the spectroscopic redshift with the fitted emission line spectrum (black dashed line). Strong [O III]5007 Å relative to [O II]3727 Å emission along with comparable [Ne III]3869 Å and [O II] emission highlight the highly energetic ISM. [O II]4363 Å detection allows for direct-Te abundance measurements confirming the low-metallicity nature. Bottom: multiwavelength photometry and best-fit SEDs for EELG1002 with Cigale (green) and Bagpipes (red). Strong [O III]+Hβ color excess is clearly observed in Subaru/HSC and S Cam i indicative of high EWs. HST F814W also shows an excess although not as sensitive given the wider wavelength coverage. Subaru intermediate and narrow bands are also affected by strong nebular emission line features. Cigale and Bagpipes are in relative agreement with slight differences. We note stellar population, IMF, and SFH modeling assumptions may be driving these minor differences.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: GMOS slit position (blue) for EELG1002 with a 10″ × 10″ HST/ACS F814W cutout (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩03 pix−1 resolution; background). Subaru/HSC i detection is shown in red contours highlighting the lower resolution of ground-based observations where we find ∼50% of EELG1002’s total flux is observed along the 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 GMOS slit. EELG1002 has GALEX/NUV (purple contours) and FUV detections, which would suggest strong Lyα emission and possible LyC escape, respectively; however, GALEX spatial resolution is quite poor. The proximity of two nearby sources along line of sight, shown with their COSMOS2020/Classic IDs and best-fit photometric redshifts, suggests the GALEX detections suffer blending issues. We therefore ignore GALEX, as well as Spitzer, photometry in this analysis due to blending issues.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: The rest-frame [O III]+Hβ EW–stellar mass anticorrelation. EELG1002 is shown as a star with dark blue using Bagpipes and light blue for Cigale for the continuum flux density in measuring [O III]+Hβ EW. We find EELG1002 is a uniquely “extreme” ELG with [O III]+Hβ EW ∼32–36× higher compared to the typical [O III]+Hβ EW at z ∼ 0.8 (blue line; A. A. Khostovan et al. 2016) and somewhat higher than the typical EW at z ∼ 3–9 (A. A. Khostovan et al. 2016; J. Matthee et al. 2023; K. Boyett et al. 2024). EELG1002 also has EW higher than Blueberries (H. Yang et al. 2017b), Green Peas (C. Cardamone et al. 2009), the z ∼ 2.5 intense starburst BOSS-EUVLG1 (R. Marques-Chaves et al. 2020), and the z ∼ 3.2 LyC emitter Ion2 (S. de Barros et al. 2016). EELG1002 is consistent with local LyC leakers (Y. I. Izotov et al. 2016, 2018, 2021b), and we do discuss the potential of LyC escape further in this study. Overall, EELG1002 is a uniquely rare and “extreme” ELG with EWs somewhat more extreme than Epoch of Reionization (EoR)-era galaxies.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Mass–metallicity relation (MZR) with measured relations at z ∼ 0 (B. H. Andrews & P. Martini 2013), z ∼ 0.5–1 (C. Ly et al. 2016), z ∼ 2.2–3.3 (R. L. Sanders et al. 2021), and z ∼ 8 (D. Langeroodi et al. 2023). EELG1002 is found to have ﹩12+{\mathrm{log}}_{10}﹩ (O/H) below z < 1 EELGs (R. Amorín et al. 2015), Blueberries (H. Yang et al. 2017b), and Green Peas (H. Yang et al. 2017c) at fixed stellar mass. Both Cigale and Bagpipes stellar mass measurement places EELG1002 highly consistent with z ∼ 5–9 galaxies at similar stellar mass (D. Langeroodi et al. 2023; J. Matthee et al. 2023; K. Boyett et al. 2024). Similar to EELG1002, local LyC leakers (Y. I. Izotov et al. 2016, 2018), Ion2 (S. de Barros et al. 2016), and BOSS-EUVLG1 (R. Marques-Chaves et al. 2020) are consistent with high-z MZRs but with higher stellar mass and ﹩12+{\mathrm{log}}_{10}﹩ (O/H) suggesting past star formation and chemical enrichment periods. EELG1002 is found to have both low mass and low metallicity consistent with high-z MZR suggesting a chemically unevolved system that could be undergoing a first bursty phase of star formation activity as expected of high-z galaxies (e.g., J. H. Cohn et al. 2018).
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Ionization and excitation properties. EELG1002 is found to have O32 and R23 well above SDSS (D. Thomas et al. 2013), EELGs (R. Amorín et al. 2015), Green Peas (H. Yang et al. 2017c), and z ∼ 2 star-forming galaxies (MOSDEF; M. Kriek et al. 2015). We find EELG1002 has line ratios most consistent with few EMPGs (M. Nishigaki et al. 2023), Blueberries (H. Yang et al. 2017b), and high-z stacks from CEERS (R. L. Sanders et al. 2023; M. Tang et al. 2023) and JADES (A. J. Cameron et al. 2023). This highlights how EELG1002 has ionization and excitation conditions consistent with EoR-era galaxies making EELG1002 a unique analog in this regard.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Conditions for planetesimal formation via the streaming instability. Red dots represent the Stokes number and dust-to-gas surface density ratio for each grid cell, which spans from 30 to 300 au, sampled every 2 kyr from 510 kyr to the end of the simulation at 750 kyr. The solid and dashed lines indicate thresholds for strong clumping due to the streaming instability, based on criteria from J. Lim et al. (2025) and J. Lim et al. (2024), respectively, with the latter corresponding to the turbulent α = 10−4. Regions above either of the thresholds would undergo strong clumping conducive to planetesimal formation.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Mass-excitation (MEx) diagram for SFG/AGN classification where EELG1002 is found to have [O III]/Hβ ratios and stellar mass consistent with star-forming galaxies. Bagpipes-derived stellar mass is near the boundary; however, this can also be due to the different IMF assumed. [O III]/Hβ ratios in conjunction with its low direct Te measured metallicity is consistent with star-forming galaxies with low [N II]/Hα in the BPT diagram (M. Pettini & B. E. J. Pagel 2004; R. A. Marino et al. 2013). EELG1002 also has [O III]/Hβ ratios consistent with Blueberries (H. Yang et al. 2017b) and Green Peas (H. Yang et al. 2017c). Based on this diagnostic, EELG1002 shows no evidence of an AGN component.
Paper: Simulations of Multiple Dust Ring Formation in a Subsolar-metallicity Protoplanetary Disk
Authors: Ryoki Matsukoba, Eduard I. Vorobyov, Takashi Hosokawa
Figure caption: Radial gas surface density distributions in the test models with different inner boundary conditions, as indicated in the legend.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Illustris Analogs of EELG1002 with their respective star formation (top), stellar and gas mass (middle), and chemical enrichment (bottom) histories. Both analogs show a rapid increase in star formation activity occurring at z ∼ 0.8 signifying a first starburst phase where both are chemically unevolved and supported by high gas masses. Rapid chemical enrichment and stellar mass buildup occur within 100–250 Myr. Subsequent histories past z < 0.7 are different between both analogs owing to various mergers; however, both eventually become 1010–11 M⊙ galaxies with solar-level metallicities. Therefore, EELG1002-like sources may potentially merge with more massive systems to become large structures in the local Universe. However, if EELG1002 remains isolated, then it could be the progenitor of a massive, compact quiescent galaxy (e.g., G. Barro et al. 2013; A. Zolotov et al. 2015).
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Left: ionizing photon production efficiency, ξion, in terms of [O III]+Hβ EW. EELG1002 is found to have ξion higher than z ∼ 1.3–2.4 EELGs (M. Tang et al. 2019), 5 < z < 7 EIGER (J. Matthee et al. 2023), and z ∼ 6.2 JWST/ERS (F. Sun et al. 2023). We find EELG1002 has ξion mostly consistent with the highest EW emitters identified at 3 < z < 9 (D. P. Stark et al. 2017; M. Onodera et al. 2020; R. Endsley et al. 2021a; M. Tang et al. 2023; Z. Chen et al. 2024). Right: ξion in terms of sSFR. EELG1002 is found to be consistent with the highest sSFR and ξion sources identified in CEERS (L. Whitler et al. 2024) and MIDIS (P. Rinaldi et al. 2023) while also being higher than 2 < z < 5 galaxies in VANDELS (M. Castellano et al. 2023) and EIGER. This highlights how EELG1002 has ionization properties consistent with some of the most “extreme,” bursty, and ionizing sources currently identified at z > 5 and provides a unique case study of low-z analogs of high-z galaxies.
Paper: EELG1002: A Record-breaking [O III]+Hβ EW ∼ 3700 Å Galaxy at z ∼ 0.8—Analog of Early Galaxies?
Authors: Ali Ahmad Khostovan, Jeyhan S. Kartaltepe, Malte Brinch, Caitlin Casey, Andreas Faisst, Santosh Harish, Ghassem Gozaliasl, Masato Onodera, Kiyoto Yabe
Figure caption: Comparison of Ne3O2 and O32 line ratios as a tracer of harder ionizing radiation spectrum. We find EELG1002 has O32 and Ne3O2 ratios significantly higher than the typical ratios measured by SDSS (D. Thomas et al. 2013), HALO7D (J. Pharo et al. 2023), CLEAR (C. Papovich et al. 2023), MOSDEF (M.-S. Jeong et al. 2020), and KBSS (A. L. Strom et al. 2017). EELG1002 is comparable to known LyC leakers (Y. I. Izotov et al. 2016, 2018), Ion2 (E. Vanzella et al. 2020), and z > 6 galaxies (A. J. Cameron et al. 2023; M. Tang et al. 2023). Compared to our Cloudy+BPASS model (green), we find EELG1002 has 0.15 dex higher Ne3O2 at fixed O32, which would suggest a harder ionizing radiation field (e.g., more energetic EUV photons).
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Three snapshots (left to right) from our fiducial simulation (at a polar magnetic field B0 = 4 × 1015 G for a nonrotating PNS) showing 2D maps of radial velocity vr (left half of each panel) and entropy (right half of each panel). We show the structure of the magnetic field during magnetic reconnection and subsequent plasmoid eruption. The outer boundary shown here is at a radius of 100 km (though the full simulation domain extends to 104 km). The white lines are the magnetic field lines, and the central white circle is the PNS with a radius of 12 km. We show the T = 0.5 MeV surface (dotted cyan lines) because this is the temperature around which the α-process occurs to burn the α particles into heavier seed nuclei for the subsequent r-process, and the properties of the wind around this temperature are critical for nucleosynthesis. See the figures in T. Prasanna et al. (2024) for the effects of various values of magnetic field and neutrino luminosity on the structure of the magnetosphere.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Radial location (top panel), polar angle (middle panel), and entropy (bottom panel) of a few tracers from the wind simulation of a nonrotating PNS at a polar magnetic field strength B0 = 4 × 1015 G. Based on the polar angle of the initial tracer release, various physical and thermodynamic tracer paths are possible, as shown. Tracers released close to the PNS equator are trapped for a significant amount of time before being released into the expanding wind. The trajectory closest to the PNS equator in the plot is shown with a dashed line.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Radial location (top panel), polar angle (middle panel), and entropy (bottom panel) of a few tracers from the wind simulation of a nonrotating and nonmagnetic (NRNM) PNS. We obtain a spherically symmetric steady-state wind in this case. The radial coordinate and entropy profiles of the tracers as a function of time are the same for all tracers released at the same instant of time from various polar angles. The trajectory closest to the PNS equator in the plot is shown with a dashed line.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Mass flux of elements with mass number A > 190 as a function of polar magnetic field (left panel), PNS spin period (middle panel), and neutrino luminosity (right panel). P⋆ is the PNS spin period in milliseconds, B0 is the PNS magnetic field in units of 1015 G, ﹩{L}_{{\bar{\nu }}_{{\rm{e}}}}﹩ is the neutrino luminosity in units of 1051 erg s−1, and Ye is the electron fraction of the initial composition in the SkyNet nucleosynthesis calculation. The solid lines labeled with Hall represent nucleosynthesis calculations that consider total entropy, while the dashed lines labeled with Hν are the calculations that consider entropy from neutrino heating only (see Tables 1 and 2). The EOS used in the MHD simulation is the HEOS, and the resolution is 256 × 128 for all the calculations shown in this plot.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Normalized abundance pattern for different values of PNS polar magnetic field B0 (in 1015 G), spin period P⋆ (in millisecond; Ω⋆ = 2π/P⋆ = 0 indicates a nonrotating PNS), neutrino luminosity ﹩{L}_{{\bar{\nu }}_{{\rm{e}}}}﹩ (in 1051 erg s−1), electron fraction Ye used to the set the initial composition in the nucleosynthesis calculations, and external heating function input to SkyNet ﹩{\dot{q}}_{{\rm{ext}}}﹩ (Hall indicates calculations which use the total entropy while Hν indicates calculations which consider heating from neutrinos alone; see Tables 1 and 2 and Section 4). The EOS used in the MHD simulation is the HEOS, and the resolution is 256 × 128 for all the calculations shown in this plot.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Mass flux of elements with mass number A > 190 as a function of electron fraction Ye of the initial composition in the SkyNet nucleosynthesis calculations. The dotted lines are the MHD simulations that use the QW equation of state (Y. Z. Qian & S. E. Woosley 1996), while all the other lines are the MHD simulations that use the Helmholtz equation of state (see Tables 1 and 2). The dashed lines are the nucleosynthesis calculations which consider entropy gain of the wind material (in the MHD simulations) from neutrino heating only (mode Hν, see Tables 1 and 2), while all the other lines consider entropy gain from all sources (mode Hall, see Tables 1 and 2). The line labels in order are the PNS magnetic field B0 (in units of 1015 G), spin period P⋆ (in millisecond; Ω⋆ = 2π/P⋆ = 0 indicates a nonrotating PNS), neutrino luminosity ﹩{L}_{{\bar{\nu }}_{{\rm{e}}}}﹩ (in units of 1051 erg s−1), resolution (indicated as LR, MR, or HR; see Tables 1 and 2), and external heating input to the nucleosynthesis calculations.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: The left panel shows average abundance per baryon for a nonrotating, nonmagnetic (NRNM) PNS, while the middle panel shows average abundance per baryon for a nonrotating PNS at a polar magnetic field B0 = 4 × 1015 G. The abundance distributions shown are averages of those obtained by all the tracers. The right panel compares the abundance patterns (normalized to the first r-process peak) in these two cases with the solar r-process abundance pattern (M. Arnould et al. 2007). Note the difference in the y-axis range of the right panel compared to the left and the middle panels. The value of electron fraction used to set the initial composition in the SkyNet nucleosynthesis calculations is Ye ∼ 0.47 (see Tables 1 and 2). The EOS used in the MHD simulation is the HEOS, and the resolution is 256 × 128 for all the calculations shown in this plot.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Production factor (Equation (16)) of various isotopes of Molybdenum (Mo) normalized to the maximum production factor of the isotopes of Mo. The line labels are PNS polar magnetic field B0 in units of 1015 G and neutrino luminosity ﹩{L}_{{\bar{\nu }}_{{\rm{e}}}}﹩ in units of 1051 erg s−1. All the calculations shown here have the electron fraction Ye of the initial composition in SkyNet nucleosynthesis calculations set to 0.485 (R. D. Hoffman et al. 1996; J. Pruet et al. 2006). The EOS used in the MHD simulation is the HEOS, and the resolution is 256 × 128 for all the calculations shown in this plot.
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Entropy along the tracer path for different resolutions (indicated as Nr × Nθ at the top right of each panel) at a PNS polar magnetic field B0 = 4 × 1015 G for a nonrotating PNS. Entropy shown here is from neutrino heating only (mode Hν in Tables 1 and 2).
Paper: Heavy Element Nucleosynthesis in Rotating Protomagnetar Winds
Authors: Tejas Prasanna, Matthew S. B. Coleman, Todd A. Thompson, Brian D. Metzger, Anirudh Patel, Bradley S. Meyer
Figure caption: Mass flux (estimated using the hydrodynamic quantities) through the T = 0.5 MeV surface that satisfies the Hoffman criterion (Equation (15)) for production of the third r-process peak (R. D. Hoffman et al. 1997) as a function of resolution (indicated as Nr × Nθ in the top-right corner of each panel).