adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Distributions of the residual eccentricity at a dominant GW frequency fGW = 20 Hz (L. Wen 2003) of NSBH mergers (left) and the final BH spin–orbit misalignment (right). Red patches show NSBH mergers in triples below a threshold of e20 < 0.4. Tertiary-driven NSBH mergers with higher eccentricities could be observed as burst-like sources and are shown by yellow patches. The distribution of isolated NSBH mergers without tertiary companions is shown by blue patches. Orange, red, and teal lines show the cumulative distributions of all NSBH mergers in triples, the subset of those with e20 < 0.4, and isolated binary mergers, respectively. Dashed lines show the cumulative eccentricity distribution from our direct N-body integration (see Section 2.3). The teal shaded region in the left panel shows the detectability limit e20 ≳ 0.07 for LVK events.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Evolution of an example triple that leads to an NSBH merger with large BH spin–orbit misalignment and significant residual eccentricity. The left panel shows large-amplitude ZKL oscillations of the NSBH eccentricity e1 (black line) as a function of time since NSBH formation. Meanwhile, the direction of the NSBH orbital angular momentum oscillates while the BH spin direction remains effectively constant, which leads to large changes of the spin–orbit angle (red line). The system merges after a few cycles at around t ≈ 0.2 Myr with a spin–orbit misalignment close to 90 °. The right panel shows the eccentricity evolution as a function of the dominant GW frequency fGW. The initial parameters of the system are m1 = 11.14 M⊙, m2 = 1.50 M⊙, m3 = 0.21 M⊙, e1 = 0.97, a1 = 2.99 au, e2 = 0.19, a2 = 27.57 au, ﹩{\hat{{\bf{e}}}}_{1}={(0.36,0.93,-0.11)}^{{\rm{T}}}﹩, ﹩{\hat{{\boldsymbol{j}}}}_{1}={(-0.53,0.10,-0.84)}^{{\rm{T}}}﹩, ﹩{\hat{{e}}}_{2}={(-0.57,-0.39,0.72)}^{{\rm{T}}}﹩, ﹩{\hat{{\boldsymbol{j}}}}_{2}={(0.68,0.28,0.68)}^{{\rm{T}}}﹩, and ﹩{\hat{{\boldsymbol{S}}}}_{\mathrm{BH}}={(-0.70,0.52,-0.49)}^{{\rm{T}}}﹩.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Cartoon of hierarchical NSBH triples whose formation and evolution is studied in this work. The two inner binary stars form an NSBH with masses m1 = mBH and m2 = mNS that is orbited by a distant tertiary companion star with mass m3. The inner and outer orbits are ellipses (denoted by indices “1” and “2,” respectively) that can be characterized by eccentricity vectors e1 and e2 that point toward the orbital periapses and have magnitudes equal to the orbital eccentricities ∣e1∣ = e1 and ∣e2∣ = e2 and by dimensionless orbital angular momentum vectors j1 and j2 that are perpendicular to the orbital planes (S. Tremaine et al. 2009). The two semimajor axes of the inner and outer orbits are hierarchical in the sense that the semimajor axes satisfy a1 ≪ a2. We also consider the evolution of the BH spin vector SBH and its angle θBH with respect to j1.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Properties of surviving triples harboring an NSBH in the inner binary (red line) and of the subset leading to mergers (red patches). NSBHs that retain significant residual eccentricity (e20 > 0.1) upon merging and coalesce with large BH spin–orbit misalignment (θBH > 90 °) are highlighted by solid and dashed golden lines, respectively. All parameters are shown at the time when the NSBHs form (i.e., after the second SN). The fractions on the y-axes are defined with respect to the total number of massive triples (10 M⊙ < m1 < 100 M⊙) at the ZAMS.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Distribution of the adiabaticity parameter ﹩R={t}_{{\rm{ZKL}}}/{t}_{{{\bf{S}}}_{{\rm{BH}}}}﹩ (see Equations (10) and (17)) and jGW/jGR (Equations (18) and (19)) of NSBH triples. Colors are as in Figure 4.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Same as Figure 6 for an example system that merges before fully completing a full ZKL cycle. As a result, the inner orbital angular momentum could only slightly deviate from the BH spin direction. The initial parameters are m1 = 7.30 M⊙, m2 = 1.50 M⊙, m3 = 0.13 M⊙, e1 = 0.58, a1 = 2.22 au, e2 = 0.63, a2 = 58.22 au, ﹩{\hat{{\boldsymbol{e}}}}_{1}={(-0.92,0.17,0.35)}^{{\rm{T}}}﹩, ﹩{\hat{{\boldsymbol{j}}}}_{1}={(-0.33,0.11,-0.94)}^{{\rm{T}}}﹩, ﹩{\hat{{\boldsymbol{e}}}}_{2}={(-0.51,0.55,-0.66)}^{{\rm{T}}}﹩, ﹩{\hat{{\boldsymbol{j}}}}_{2}={(-0.19,0.68,0.71)}^{{\rm{T}}}﹩, and ﹩{\hat{{\boldsymbol{S}}}}_{\mathrm{BH}}={(-0.33,0.17,-0.93)}^{{\rm{T}}}﹩.
Paper: Water Production Rates of the Interstellar Object 3I/ATLAS
Authors: Zexi Xing, Shawn Oset, John Noonan, Dennis Bodewits
Figure caption: Compilation of reddening measurements for 3I/ATLAS. Left panel: reddening measurements of 3I/ATLAS in literature versus the central wavelength of the measurement bands. Marker shapes denote references; colors indicate heliocentric distance (colorbar at far right). Black dashed line marks the middle effective wavelength between V and UVW1 (4381.8 Å). Right panel: same measurements converted to reddening at the middle effective wavelength between V and UVW1. Y-axis shows original measurement wavelengths; x-axis shows converted reddening values at our middle wavelength. Symbols and colorbar as in the left panel.
Paper: Water Production Rates of the Interstellar Object 3I/ATLAS
Authors: Zexi Xing, Shawn Oset, John Noonan, Dennis Bodewits
Figure caption: Dependence of number of OH molecules within the 10″ aperture and water production rate on reddening. The left panel presents results from the July 31 visit, while the right panel shows results from the August 19 visit. In each panel, the blue line shows the number of OH molecules and corresponding water production rates as a function of assumed reddening between V and UVW1 effective wavelengths. Shaded regions indicate 1σ stochastic uncertainty. The black dotted line indicates the reddening measured at the same wavelength range using reflectance spectra from R. Rahatgaonkar et al. (2025; private communication). The blue dashed line denotes zero production rate.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Distribution of inner semimajor axis a1 (top panel) and semimajor axis ratio a2/a1 (bottom panel) before the second SN of systems that successfully form stable NSBH triples. Different colors refer to different natal kick models, and the distributions are normalized with respect to the total number of NSBH triples formed in each model.
Paper: Water Production Rates of the Interstellar Object 3I/ATLAS
Authors: Zexi Xing, Shawn Oset, John Noonan, Dennis Bodewits
Figure caption: Stacked images of interstellar comet 3I/ATLAS acquired with UVOT, two visits. The first were obtained on 2025 July 31 and August 1 (visit 1, top half of figure) and the second on 2025 August 19 (visit 2, bottom half of figure). Images acquired with the V filter are shown on the left, with UVW1 images shown on the right. Source apertures used are shown in red, with the background sky annulus in dotted white. The UVW1 aperture is ≈20,000 km (10″) for July 31 and ≈19,000 (10″) km for August 19. Background annulus spans 122,000–184,000 km for visit 1 and 114,000–171,000 km for visit 2. Ticks along the edges mark 20″, with 2047 and 1908 km per arcsecond for each visit, respectively. Color scales are individually optimized for viewing. Inset grids are 10″ × 10″, centered on the nucleus.
Paper: Water Production Rates of the Interstellar Object 3I/ATLAS
Authors: Zexi Xing, Shawn Oset, John Noonan, Dennis Bodewits
Figure caption: Radial surface brightness profiles of 3I/Atlas in the V and UVW1 images for two observation visits. The left panel corresponds to the July 31 visit and the right panel to August 19. In each panel, solid lines represent the measured profiles, while shaded regions indicate 1σ stochastic uncertainty. Dashed lines represent the instrumental PSF for each filter. All profiles are normalized to the brightness at the nucleus. The profiles for the V filter are represented in green, while the UVW1 profiles are depicted in purple.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Cumulative distribution of the residual eccentricity at fGW = 20 Hz of tertiary-driven NSBH mergers (top panel) and their spin–orbit misalignment (bottom panel). Different colors refer to our range of natal kick models, restricted to a subset of mergers with e20 < 0.4. Dashed gray lines include mergers above e20 ≥ 0.4, and solid gray lines display mergers from isolated binaries.
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: Spectrally integrated flux maps for 3I/ATLAS observed using JWST NIRSpec: (a) scattered light from coma dust at ∼1.2 μm, plotted on a logarithmic scale to highlight the coma shape, (b) CO2 at 4.3 μm, (c) H2O at 2.7 μm, and (d) CO at 4.7 μm. Image axes are aligned with the equatorial (R.A./decl.) grid. Molecular line emission has been isolated by subtracting a polynomial fit to the adjacent continuum. Spatial coordinates are with respect to the brightest pixel in the continuum dust map. For panels (b)–(d), inset plots (upper right) show the continuum-subtracted spectra, spatially averaged across all IFU pixels. Panel (a), lower left corner, shows the direction of the (sky-projected) comet–Sun (S) and nucleus velocity (v) vectors (which are too close to distinguish). For H2O and CO, the 3σ noise level is shown with a dotted contour; for the dust and CO2 maps, the 3σ noise level lies outside the IFU boundary, so it is not shown.
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: JWST spectrum of 3I/ATLAS using the NIRSpec PRISM (sky background subtracted), spatially integrated over the IFU field of view and plotted with a logarithmic flux scale. Prominent spectral features are labeled.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: 1/ρ-enhanced 1.2 μm scattered light map for 3I/ATLAS observed using JWST NIRSpec. This is panel (a) from Figure 2, multiplied by ρ (the sky-projected distance from the center of the brightest pixel—the assumed location of the nucleus). Similarly enhanced maps of the gas emission are shown in Appendix A (Figure 7). Image axes are aligned with the equatorial (R.A./decl.) grid. The white cross shows the position of the (pseudo) nucleus pixel.
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: Coma CO2/H2O mixing ratios as a function of heliocentric distance for previously observed comets, grouped by category: (1) long-period comets (LPCs), including Oort Cloud and Halley-type comets, (2) Jupiter-family comets (JFCs), (3) main-belt comets, and (4) Centaurs. Data are from the compilation of O. Harrington Pinto et al. (2022), with additional values from M. S. P. Kelley et al. (2023), O. Harrington Pinto et al. (2023), H. H. Hsieh et al. (2025), C. E. Woodward et al. (2025), and C. Snodgrass et al. (2025). Values for 67P/Churyumov–Gerasimenko at rH = 3.5, 1.2, 3.5 au (pre- to postperihelion) are included, from M. Combi et al. (2020). Upper and lower limits are shown with arrows. A log-linear curve is fitted to the combined LPC + JFC data set (dashed line), with ±1σ margins shown as dotted gray lines (where σ is the standard deviation of the data from the fit). The peculiar, hypervolatile-rich comet C/2016 R2 was excluded from the fit. 3I/ATLAS (red star) is labeled, in addition to the lower limit for the recently observed distant Oort cloud comet C/2024 E1 (C. Snodgrass et al. 2025).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: Best-fitting production rates for CO2, CO, H2O, and OCS as a function of distance from the nucleus (Q curves). Spectra were extracted and modeled within four spatial regions of the IFU, as shown in the inset diagram, consisting of a central ﹩0\mathop{.}\limits{^{\prime\prime} }625﹩ radius circle, followed by three successive partial annular sectors, each with a ﹩0\mathop{.}\limits{^{\prime\prime} }625﹩ radial extent. Due to its higher SNR, CO2 was also modeled within successive ﹩0\mathop{.}\limits{^{\prime\prime} }1﹩ annuli surrounding the nucleus. OCS values have been scaled up by a factor of 10 for display. Vertical error bars indicate 1σ statistical uncertainties, while the horizontal error bars indicate the radial extent of each spatial region.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: Observed NIRSpec molecular spectra of 3I/ATLAS extracted within a ﹩0\mathop{.}\limits{^{\prime\prime} }625﹩ radius circular aperture centered on the (pseudo)nucleus, along with best-fitting gas and continuum models. The left ordinate axes apply to the model gas component fluxes (lower traces), whereas the right ordinates are for the observed spectrum, total model, and continuum model components (upper traces). The weak 13CO2 band at 4.4 μm is shown in the inset panel next to the main CO2 band, with 3σ upper limit spectral model overlaid.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Scaling Law for the Orbital Architecture of Planetary Systems Formed by Gravitational Scattering and Collisions
Authors: Eiichiro Kokubo, Haruka Hoshino, Yuji Matsumoto, Re'em Sari
Figure caption: Panel (a) Examples of the final planetary system on the semimajor-axis a-eccentricity e plane, where a is scaled by the inner edge radius rin for protoplanet systems at different locations (models S0 and R1–3), together with the initial protoplanet system (top panel). The sizes of the circles are proportional to the physical sizes of the planets. Panel (b) Maximum ﹩\langle {M}_{{\rm{\max }}}\rangle ﹩ (filled circles) and average 〈Mave〉 (open circles) masses of planets (top panel) and the orbital separation between adjacent pairs ﹩\langle {\tilde{b}}_{{\rm{H}}}\rangle ﹩ (filled circles) and eccentricity ﹩\langle {\tilde{e}}_{{\rm{H}}}\rangle ﹩ (open circles) normalized by the Hill radius rH (bottom panel) against the system semimajor axis 〈aM〉 for (rin, rout) = (0.05, 0.15), (0.1, 0.3), (0.2, 0.6), and (0.5, 1.5) (the unit is au; models S0 and R1–3).
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: 1/ρ-enhanced flux maps for 3I/ATLAS observed using JWST NIRSpec. These are the images from Figure 2, multiplied by ρ (the sky-projected distance from the center of the brightest pixel), for (a) scattered light at 1.2 μm, (b) CO2 at 4.3 μm, (c) H2O at 2.7 μm, and (d) CO at 4.7 μm. Image axes are aligned with the equatorial (R.A./decl.) grid. Panel (a), lower left corner, shows the direction of the (sky-projected) comet–Sun (S) and nucleus velocity (v) vectors (which are too close to distinguish). The white cross shows the position of the nucleus pixel.
Paper: JWST Detection of a Carbon-dioxide-dominated Gas Coma Surrounding Interstellar Object 3I/ATLAS
Authors: Martin A. Cordiner, Nathan X. Roth, Michael S. P. Kelley, Dennis Bodewits, Steven B. Charnley, Maria N. Drozdovskaya, Davide Farnocchia, Marco Micheli, Stefanie N. Milam, Cyrielle Opitom, Megan E. Schwamb, Cristina A. Thomas, Stefano Bagnulo
Figure caption: Best-fitting rotational temperatures for CO2, CO, and H2O as a function of sky-projected distance from the nucleus.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Scaling Law for the Orbital Architecture of Planetary Systems Formed by Gravitational Scattering and Collisions
Authors: Eiichiro Kokubo, Haruka Hoshino, Yuji Matsumoto, Re'em Sari
Figure caption: Time evolution of the number 〈N〉 (top panel) and the normalized orbital separation between adjacent pairs ﹩\langle {\tilde{b}}_{{\rm{H}}}\rangle ﹩ (filled circles), eccentricity ﹩\langle {\tilde{e}}_{{\rm{H}}}\rangle ﹩ (open circles), and inclination ﹩\langle {\tilde{i}}_{{\rm{H}}}\rangle ﹩ (open squares; bottom panel) of the standard protoplanet systems (model S0). The values and error bars indicate the median and median absolute deviation in 20 runs, respectively.
Paper: A Scaling Law for the Orbital Architecture of Planetary Systems Formed by Gravitational Scattering and Collisions
Authors: Eiichiro Kokubo, Haruka Hoshino, Yuji Matsumoto, Re'em Sari
Figure caption: Maximum ﹩\langle {M}_{{\rm{\max }}}\rangle ﹩ (filled circles) and average 〈Mave〉 (open circles) masses of planets normalized by the system total mass Mtot (top panel) and the normalized orbital separation between adjacent pairs ﹩\langle {\tilde{b}}_{{\rm{H}}}\rangle ﹩ (filled circles) and eccentricity ﹩\langle {\tilde{e}}_{{\rm{H}}}\rangle ﹩ (open circles; bottom panel) against the total mass of protoplanet systems with the reference surface density Σ1 = 5, 10, 20, and 50 (models S0 and M1–3).
Paper: A Scaling Law for the Orbital Architecture of Planetary Systems Formed by Gravitational Scattering and Collisions
Authors: Eiichiro Kokubo, Haruka Hoshino, Yuji Matsumoto, Re'em Sari
Figure caption: Orbital separation between adjacent pairs ﹩\langle {\tilde{b}}_{{\rm{K}}}\rangle ﹩ (filled circles) and eccentricity ﹩\langle {\tilde{e}}_{{\rm{K}}}\rangle ﹩ (open circles) normalized by the eccentric distance rK against the system semimajor axis 〈aM〉 for (rin, rout) = (0.05, 0.15), (0.1, 0.3), (0.2, 0.6), and (0.5, 1.5) (the unit is au; models S0 and R1–3).
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: A 3D rendering showing the surface of the BD in R1 when it is 2 weeks old. The color scale displays the radial magnetic field strength on the surface. The green streamlines display closed magnetic loops, meaning field lines that loop from magnetic north to magnetic south on the surface. The red arrow displays the angular momentum axis of the BD. The left and bottom image panels are cross-sectional slices of the interior of the BD, displaying the magnitude of current density (left) and specific gas entropy (bottom). The image panel on the right displays the maximum magnetic field strength along the line of sight (y-axis). The mass and radius of the BD are displayed in the top-left corner.
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: Circumstellar disk formed in run R2, visualized at our final simulation snapshot. Left: density slice across the center of the BD, visualized in a top-down view. The lime-colored contour displays the BD surface, defined as all gas having dissociated over 95% of its H2. Right: 2D histogram displaying the distribution of azimuthal velocity normalized by ﹩\sqrt{{g}_{{\rm{r}}}r}﹩ as a function of radius, binned across all cells in the computational domain. The colormap indicates the colatitude θ scaled by π, with θ/π = 0.5 representing the equator, while θ/π = 1 and 0 correspond to the south and north poles, respectively. A dashed line marks the threshold ﹩{v}_{\phi }/\sqrt{{g}_{{\rm{r}}}r}=1﹩.
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: Mass (a), radius (b), and specific angular momentum of the BD in each of our runs, displayed as a function of time since BD birth.
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: Evolution of the density (first row, (a)–(e)), temperature (second row, (f)–(j)), and specific entropy (third row, (k)–(o)), averaged in radial bins and displayed as a function of radius at different times, where t = 0 marks the birth of the BD. Each column corresponds to a different run.
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: Bipolar low-velocity outflows at first core scales. Shown here are radial velocity slices for each run.
Paper: Brown Dwarf Formation through Gravitational Collapse: Insights from 3D Numerical Simulations
Authors: Adnan Ali Ahmad, Benoît Commerçon, Gilles Chabrier, Antonin Borderies
Figure caption: BD radius as a function of mass for run R1 at different maximum refinement level. The lower-resolution runs are restarts at different snapshots of their higher-resolution counterparts.