adsabs/AstroCLIMB huggingface dataset:
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 6890. Black denotes XMM-Newton pn data, red denotes XMM-Newton MOS1 data, green denotes XMM-Newton MOS2 data, blue denotes data from Swift observation 00088188001, cyan denotes data from Swift observation 0008818800, and magenta and yellow denote NuSTAR FPMA and FPMB data, respectively.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 5005 NuSTAR data using a TBABS*RELXILL model and realistic reflection fraction values. Black is FPMA data, and red is FPMB data. The spin in this case is a = 0.998.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra (ObsID: 4913) and NuSTAR FPMA images of Mrk 463. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circles denote the Chandra extraction regions. Two extranuclear point sources (Source 1 and Source 2) were visible in all Chandra observations and were used in the fitting process.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra and NuSTAR FPMA images of NGC 5005. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circles denote the Chandra extraction regions. Two off-nuclear point sources (Src 1 and Src 2) are visible in the Chandra image, but were faint enough to be ignored in the spectral fitting.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: NuSTAR FPMA image of NGC 6890. The XMM-Newton data, which have lower angular resolution than Chandra, did not detect any off-nuclear point sources within the NuSTAR beam (shown in red).
Paper: Ultrawide Black Hole—Neutron Star Binaries as a Possible Source for Gravitational Waves and Short Gamma-Ray Bursts
Authors: Erez Michaely, Smadar Naoz
Figure caption: The delay time distribution (DTD) for a MW-like galaxy with a velocity dispersion of σ = 40 km s−1. Blue circles are the model calculations. Black solid line is the best power-law fit. Note that this fit is specific for the MW-like galaxy adopted here; see text for more details. The GW merger span for the entire lifetime of the galaxy, which suggests these mergers occur in early- and late-type galaxies.
Paper: Ultrawide Black Hole—Neutron Star Binaries as a Possible Source for Gravitational Waves and Short Gamma-Ray Bursts
Authors: Erez Michaely, Smadar Naoz
Figure caption: Average merger rate for a MW-like galaxy as a function of unrealistic velocity dispersion. Rate is calculated after 1010 yr from star formation accounting for binary ionization. Binaries consist of m NS = 1.5 M ⊙ and m BH = 10 M ⊙. For v enc ≲ 40 (≳150) km s−1, the closest approach b = b impulse (b = b kick) for all SMAs (gray area); see text. The white area is a mix of both regimes. The rate for an elliptical galaxy shows a similar behavior and is omitted here to avoid clutter.
Paper: Ultrawide Black Hole—Neutron Star Binaries as a Possible Source for Gravitational Waves and Short Gamma-Ray Bursts
Authors: Erez Michaely, Smadar Naoz
Figure caption: Average merger rate for a MW-like galaxy (red dots) and elliptical galaxy (blue dots). The velocity dispersion is σ = 40km s−1 for the MW-like galaxy and σ = 160km s−1 for the elliptical. Rate is calculated after 1010 yr from star formation, for binaries with m NS = 1.5 M ⊙ and varying m BH = 10 M ⊙.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Top: exact and approximate (using Equation (A4)) τ 0(θ) profiles computed between r = 0.1 and 0.4 au in a disk with a vertical temperature stratification. Vertical dashed lines indicate the location of the τ = 1 surfaces for each method. Bottom: relative τ 0 differences between both approaches.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Normalized time-dependent L 1-norms of T − T ref for different values of ﹩\hat{c}﹩ taking f dg = 10−2 (top) and 10−3 (bottom).
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Temperature distributions as a function of time for run rhdg2_c4 (left column) and the corresponding higher-resolution runs (middle and right columns for N  r  × N  θ  = 1024 × 400 and 2048 × 800, respectively).
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Cumulative mass loss of the RSG outburst models with different initial envelope structures. Solid lines track the mass expected to be ejected (with radial velocity exceeding the escape velocity); dashed lines simply tally mass leaving the outer simulation boundary regardless of velocity. Model envelopes with initial radial motions (3DCONV0.5 and 3DVRAD0.5) are susceptible to nonuniform shock propagation, resulting in considerably higher mass loss. With the initial radial velocities removed, 3DVTAN0.5 behaves qualitatively similarly to the static models 3D/1DMESA0.5.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Density slices of the 3DCONV0.5 fiducial (left) and 3DMESA0.5 (right) models at 5 t dyn (top) and 10 t dyn (bottom) after energy deposition. Aspherical distributions of the ejected mass are apparent in 3DCONV0.5. In 3DMESA0.5, the envelope reaches a maximum radius of ≈1500 R ⊙ and falls back into an inflated and turbulent state; unlike 3DCONV0.5; gas in the inner envelope cannot escape.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Radial velocity profiles of the pulse launched by energy deposition from the 3DMESA0.5 run. The curves show the evolution from 0.3 t dyn to 0.75 t dyn at intervals of 0.06 t dyn. The pulse strengthens and becomes a shock at the sonic radius of 640 R ⊙. The peaks in the speed of sound near ≈300 R ⊙ are the results of the energy deposition.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Density slices of the 3DCONV0.5 fiducial (left) and 3DMESA0.5 (right) models at 1 t dyn (top) and 2 t dyn (bottom) after energy deposition. The time stamps display the time since the beginning of the energy injection. Nonuniform shock propagation in the 3DCONV0.5 model accelerates gas above escape velocity in some lines of sight, whereas in 3DMESA0.5 the envelope expands coherently despite the RTIs.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Radial profiles of density, temperature, pressure (radiation and gas), and velocity in the 3D convective equilibrium model. The colored lines show the last 5 t dyn of evolution at intervals of 0.1 t dyn before energy deposition. The black curves in the density, temperature, and pressure panels are the 1D MESA profiles used to initialize the 3D FLASH model. In the velocity panel, the black curve denotes the convective velocity predicted by the mixing length theory in MESA. The density profiles from the 1D control run (FLASH1D) are also shown for comparison.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Histogram of pre-deposition radius of the ejected mass from the 3DCONV0.5 and 3DMESA0.5 runs. Without convective initial conditions, only mass above the sonic radius can be ejected (3DMESA0.5). In 3DCONV0.5, mass down to the energy injection radius is able to escape through low-density channels set up by the convective velocities.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Density and radial velocity slices at ϕ = π/2, taken from the last snapshot of the convective equilibrium model before energy deposition. Convective structures are evident in the RSG envelope.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Time evolution of different forms of energy during the preparation of the 3D convective equilibrium model.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Theoretically predicted SI growth timescales in a turbulent disk (colors) with superposed particle St from our models (symbols). The growth timescales are for the fastest growing SI modes, and are based on the model of Umurhan et al. (2020) and shown in shades of color in units of local orbit times. A sharp diagonal boundary in (α  t , St) phase space that cleanly separates the blue and green regions represents the ϵ = 1 line, with smaller values above the line. The values shown are specifically valid for a local Z = 0.01 just outside the snowline (i.e., T ≈ 160 K). Various growth barriers and turbulence constraints discussed in Section 4.1 are shown as lines with arrows indicating putative forbidden regions in parameter space. The plotted St symbols correspond to particle radii dominating the particle mass, from our models for four different values of α  t . Solid filled symbols represent non-porous particles while stippled symbols represent porous fractal aggregates. Two classes of particles are shown at α t = 10−3: the yellow symbols are for nominal sticky water ice, and the orange colored species denote particles whose fragmentation energies (Q f) are relatively low, representing cold water ices as discussed in Appendix B (e.g., Musiolik & Wurm 2019). The particle St predicted in our growth results generally fall within the ϵ < 1 region of parameter space wherein SI growth times are predicted to be very long, in agreement with all published numerical simulations (Umurhan et al. 2020). Only the fractal growth model (fa5g) for an extremely low α t = 10−5 falls below the ϵ = 1 line. The compact growth model (sa5g) can also satisfy this condition, but only at higher local Z (the ϵ = 1 curve shifts upwards for increasing values of the metallicity, see Umurhan et al. 2020).
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Fiducial model after 0.5 Myr (black solid curves) compared to a suite of models where we vary the disk mass M D, disk scaling parameter R 0, and fragmentation threshold Q f as listed in Table 2. (a) Gas surface densities; (b) total solids surface densities; (c) midplane temperatures; (d) disk metallicities; (e) Rosseland mean opacities; and (f) Stokes numbers of the mass-dominant aggregates, all as a function of semimajor axis. The solid blue curves that appear in panels (a)–(c) are for a standard MMSN. In each panel, the cyan region demarcates the range in location of the water snowline for these models (between ∼ 2.7 and 4 au).
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Evolution of the internal density ρ int = ρ p/ψ of aggregates for models fa2g, fa3g, and fa4g shown in Figures 2, 7, and 8. Despite being relatively massive (∼105−109 g), the large aggregates outside the snowline are quite underdense, though they continue to be compacted. In the inner disk, particles were initially underdense, but begin to be compacted earlier on and more vigorously. Transitions in density due to compositional changes at EFs can be seen as vertical bands in the plots. Darker vertical bands (lower density particles) initially seen at ∼250 au are solid methane (see Paper III). This region of the disk also exhibits rapid inward particle drift where St ∼ 1 (a location that moves outward with time due to viscous spreading of the disk), which manifests as the peak in particle mass seen at 150−200 au until 105 yr. The particle size distributions for these models after 0.5 Myr can be seen in Appendix A.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Examples of the fraction of parent body masses of a particular element that are predicted to be in the convection zone of a WD as a function of time, according to the J09 model (Equation (2)). We assume an accretion disk lifetime of 105 yr and settling times of 102 yr for the DA (top) and 106 yr for the DB (bottom). Note the three phases of accretion: increasing, steady state, and decreasing. While analogous phases occur both for the DA and DB, the timescales defining the boundaries of each phase are swapped due to the longer DB settling times.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Comparison of simulations that use Gaussian (g; Section 2.4.3) and Maxwellian (m) velocity PDFs. These highlight subtle differences in the particle mass distributions, and in particular the difference in the mass of the lucky particles m L, which are the largest mass to which particles or aggregates can grow beyond the fragmentation barrier m f (dashed curves). The solid curves are the dominant mass particle m M of the distribution. Sharp variations in m M and m L especially seen in the top two panels are associated with crossing EFs. For example, the organics EF is at ∼1.5 au, and the water ice EF is located at ∼4 au, outside of which Q f increases so aggregates can begin to grow larger.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Particle size distributions for compact particle (top panels) and fractal aggregate growth models (bottom panels) plotted on roughly the same scale in solids mass volume density m 2 f(m) after 0.5 Myr for the indicated simulations. These wireframes (plotted out to 10 au) can be compared with the rightmost panels of the particle mass distributions in the main text. Several EFs are indicated by the cyan (water), orange (organics), and green (troilite) curves. Regions that appear flat at this scale correspond to particle sizes that have not reached the fragmentation barrier. Recall that in the moments method, the dust population is modeled as a power law up to the fragmentation barrier r f.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Evolution of the midplane solids-to-gas ratio ϵ = ρ solids/ρ over time, for compact particle (left panels) and fractal aggregate (right panels) growth models with α t = 10−3, 10−4, and 10−5. The location of the water ice snowline at the corresponding simulation times is indicated by the vertical dotted lines. Only the lowest turbulence model sees a very short period where ϵ > 1 at the snowline, with St ≳ 0.1. Models with α t = 10−2 are not shown because there is no significant enhancement in ϵ anywhere. Planetesimal formation by SI requires midplane ϵ > 1 (Paper I; Umurhan et al. 2020).
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Variation of the monomer size for model fa3gQ (cold H2O ice model) after 0.1 Myr. In the context of our adopted fractal growth model (Okuzumi et al. 2012), larger monomer sizes do lead to slightly more compact particles compared to the nominal model (solid curve), but porosities are still much larger than typical cometary IDPs.
Paper: Energy Conversion and Partition in Plasma Turbulence Driven by Magnetotail Reconnection
Authors: Xinmin Li, Rongsheng Wang, Can Huang, Quanming Lu, San Lu, J. L. Burch, Shui Wang
Figure caption: Energy conversion with current density. (a) The cumulative distribution functions (CDFs) of current density (black trace) and energy conversion rate (red trace). The CDF of current density, at ∣ J ∣, was defined by ﹩{\sum }_{\left|{\boldsymbol{J}}\right|}^{\infty }f﹩, representing the probability that current density is greater than ∣ J ∣, where f is the probability density function of current density. The CDF of  J • E , at ∣ J ∣, was defined by ﹩{\sum }_{0}^{\left|{\boldsymbol{J}}\right|}{\boldsymbol{J}}\bullet {\boldsymbol{E}}﹩, representing the sum of energy conversion rate in the region with the current density less than ∣ J ∣. The dashed curve line represents a Gaussian distribution. The major net positive energy conversion region is marked by two vertical dashed lines. (b) The averages of ﹩\left|{\boldsymbol{J}}\bullet {\boldsymbol{E}}\right|﹩ calculated based on the binned value of current density (bin size is 5 nA/m2). The black line represents a linear fitting between ﹩{\left\langle | {\boldsymbol{J}}\bullet {\boldsymbol{E}}| \right\rangle }_{{\boldsymbol{J}}}﹩ and ∣ J ∣. (c) The average of  J • E  conditioned on the local current density. Black points represent ﹩{\left\langle {\boldsymbol{J}}\bullet {\boldsymbol{E}}\right\rangle }_{{\boldsymbol{J}}}\gt 0﹩, and gray points represent ﹩{\left\langle {\boldsymbol{J}}\bullet {\boldsymbol{E}}\right\rangle }_{{\boldsymbol{J}}}﹩ < 0. The dotted line is a quadratic fit between ﹩{\left\langle {\boldsymbol{J}}\bullet {\boldsymbol{E}}\right\rangle }_{{\boldsymbol{J}}}﹩ and ∣ J ∣.
Paper: Energy Conversion and Partition in Plasma Turbulence Driven by Magnetotail Reconnection
Authors: Xinmin Li, Rongsheng Wang, Can Huang, Quanming Lu, San Lu, J. L. Burch, Shui Wang
Figure caption: Energy partition between ions and electrons related to the local current intensity and direction. (a) Cumulative distribution function (CDF) of  J • E ,  J  ∥• E  ∥,  J  ⊥• E  ⊥. (b) CDF of  J • E ,  J    e  • E ,  J    i  • E . (c) CDF of  J  ⊥• E  ⊥,  J    e ,⊥• E  ⊥, J  i,⊥• E  ⊥. (d) CDF of  J  ∥• E  ∥,  J    e ,∥• E  ∥,  J    i ,∥• E  ∥ The black traces in (a)–(d) represent the CDF of ∣  J ∣.
Paper: Energy Conversion and Partition in Plasma Turbulence Driven by Magnetotail Reconnection
Authors: Xinmin Li, Rongsheng Wang, Can Huang, Quanming Lu, San Lu, J. L. Burch, Shui Wang
Figure caption: Power spectral density (PSD) of magnetic field and electric field. (a) PSD of the magnetic field. (b) PSD of the total (black trace), parallel (magenta trace), and perpendicular (cyan trace) electric field. The vertical dashed lines represent the average ion cyclotron frequency (f  ci  ∼ 0.14 Hz), average lower hybrid frequency (f  lh  ∼ 6 Hz), and average electron cyclotron frequency (f  ce  ∼ 250 Hz). The colored dashed lines are power-law fits to specific frequency bands.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Long-term optical and near-infrared light curves of V1515 Cyg. The vertical solid black line denotes the fading event that occurred in 1980. We complemented our work with data from the literature prior to 2006 and it is summarized in Table 2.(The data used to create this figure are available.)
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Upper panels: Fourier spectra (black line) calculated from the detrended and transformed to normalized flux units 2019 (Sectors 14 and 15) and 2021 (Sector 41) TESS light curves. The stochastic nature (a  f  ∼ f −1) of these oscillations is indicated by the two parallel green dashed lines. The amplitude errors are represented by blue dots. Middle panels: respective Morlet wavelet spectra for TESS. Bottom panels: Morlet wavelet spectra showing the 13.1–13.9 d QPO observed in 1987 and 2003. The original Johnson V data are shown below. In all wavelet spectra, the major edge effects lie outside of the white dashed lines. The secondary effects caused by interruptions in TESS data acquisition are marked by white solid lines.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Time evolution of some characteristic lines in the optical spectra of V1515 Cyg. To show each line profile clearly, we smoothed them with a 30 pixel moving window. The Li I 6707 Å line observed on 2015 December 26 is affected by an artifact, which is indicated with a dashed line in the third panel. The artifacts on the other lines are also presented with dashed lines.