adsabs/AstroCLIMB huggingface dataset:
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: A snapshot of a flux rope from one of the cartesian MHD simulations with η 0 = 0.029, and ρ 0 = 1.0, showing heatmaps of various diagnostic quantities to illustrate its structure. The black lines in the magnetic field plot are the field lines projected onto the plane, and the heatmap represents the out-of-plane component of the field. All quantities except the fluid velocity are strictly positive, increasing from zero (white) to their maximum value (red) on the colormap. The vertical fluid velocity can take negative values within the rope, which are shown in blue.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Illustration of the initial condition and relaxed outflow field state of the MHD simulations. Such an outflow field is obtained in the absence of driven boundary conditions or supergranular diffusion, where the system evolves due to the effect of the solar wind alone. The colormaps show the vertical velocity, out-of-plane magnetic field (zero, in this case) and the fluid density.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: A snapshot of a flux rope in one of the cartesian MF simulations with η 0 = 0.005, and ν 0 = 1.0, showing colormaps of various diagnostic quantities to illustrate its structure. The black lines in the magnetic field plot are the field lines projected onto the plane, and the heatmap represents the out-of-plane component of the field.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Formation and eruption of a flux rope. This is a cartesian MHD simulation with coronal diffusion η 0 = 0.01. The heatmaps represent the out-of-plane current density, and the black lines are the magnetic field lines projected into the plane. The rope erupts at around t = 285 days, after which it reforms. The process would then in general repeat.
Paper: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Authors: Oliver E. K. Rice, Anthony R. Yeates
Figure caption: Photospheric shearing rates varying with latitude (measured from the north pole). The angular velocity (solid line) is then shifted into the correct reference frame and to code units (dashed line). It is then multiplied by ﹩\sin \theta ﹩ to give a linear velocity on the solar surface (dotted line).
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Closer look at the main pulse (left) and interpulse components (right) in the recovered intrinsic pulse profile across 19 frequency bands. Red arrows point to a bump caused by giant pulse emission. The vertical axis for each profile is in intensity with arbitrary units. Scaling is different between the left and right panels to help see details; the interpulse component is approximately half as bright at its peak as the main pulse component.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Comparison between the observed pulse profile (left panels) and the recovered intrinsic pulse profile (right panels) for PSR B1937+21. Top: average pulse profiles at 327 MHz (bandwidth of 3.125 MHz) for our two observations at MJD 58245 and MJD 58298. On the right, the profile for MJD 58298 is plotted with a dashed line to help visually identify both profiles. Middle: average pulse profiles for the observation on MJD 58245 across the 19 frequency bands. Bottom: pulse profiles at 327 MHz (bandwidth of 3.125 MHz) across time for the observation on MJD 58245.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Top: noise-corrected normalized correlations between giant pulse data and predicted IRFs for 0 ms ≤ τ ≤ 0.8 ms, where most of the signal lies. The correlations are corrected for contributions by noise in both the data and model but not for correlation in the noise between the two. Bottom: normalized correlations for the pure-noise regions of τ < 0 and >3 ms between the data and model. The correlation between the model and the training set confirms that they share correlated noise, while the lack of correlation with the validation set shows that there are no systematic effects shared between all pulses.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Giant pulse search. Top: squared modulus of the observed signal. The reference pulse is marked with an arrow. The inset shows the real part of the complex-valued voltages of the reference pulse, with the 0.4 ms span used in the cross-correlation to find further pulses highlighted in pink. Bottom: signal cross-correlated with the reference pulse, revealing many other impulses. The dashed horizontal line denotes the detection threshold we use. The inset is a zoom-in around the impulse marked with the arrow, with the dashed vertical line indicating the impulse’s computed location.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Best-fit τ and ﹩\dot{\tau }﹩ (with error bars) inferred from Gaussian fits to the 2.4 ms feature across three frequency bands on MJD 58245. The contours mark the 1σ widths of the Gaussians. The center and widths for a fit for the total intensity on MJD 58298 are shown for comparison.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Wavefield solutions for three specific bands (of width 3.125 MHz) for both of our observations. The color scale corresponds to ﹩{\mathrm{log}}_{10}| W(\tau ,{f}_{D}){| }^{2}﹩ in arbitrary units. One sees that most power is contained within τ ≲ 0.8 ms but that the IRF extends to larger delays, with a faint structure at ∼2.5 ms.
Paper: Using Giant Pulses to Measure the Impulse Response of the Interstellar Medium
Authors: Nikhil Mahajan, Marten H. van Kerkwijk
Figure caption: Comparison between the predicted impulse response and an observed giant pulse at 327 MHz. As can be seen from the zoom-in, as well as from the flat residuals, there is good correspondence between the data and the model.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Time evolution of critical radii for the fiducial model. By assuming a fixed binary cavity size, the inner edge of the gas disk obeys R in = 2 a bin at all times. Inside the trapping radius R trap, photons are advected inwards with the accretion flow faster than they can escape via outwards diffusion (Equation (11)) (olive curve), while within R adv,1/2 (red curve) the rate of advective cooling exceeds half of the total cooling rate. The stagnation radius R stag is defined as the smallest radius where v  r  = 0, thus separating gas flowing in toward the binary and that spreading viscously outwards. The radii R m,1/2 and R j,1/2 are those within which half of the disk mass and angular momentum are contained, respectively. The radius R irr,1/2 is the location beyond which the irradiation heating rate exceeds half the total heating rate (i.e., the inner edge of the irradiation-dominated region), while R pe is where the rate of photoevaporation wind mass loss ﹩2\pi {r}^{2}{\dot{{\rm{\Sigma }}}}_{\mathrm{pe}}﹩ peaks. For comparison, we show the thermal time (Equation (13); vertical dashed line) and an approximate range of nuclear times (gray shaded region) of the stripped He core.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Top panel: partition of the initial disk mass and angular momentum among the CBD, binary (through accretion, green curve), and the photoevaporation wind as a function of time, for the fiducial model. Bottom panel: rates of various mass-loss processes from the CBD, including ﹩{\dot{M}}_{\mathrm{in}}﹩, accretion rate onto the binary at R in; ﹩{\dot{M}}_{\bullet }﹩, accretion rate reaching the central BH/NS at R isco accounting for super-Eddington wind mass loss (Equation (58)); ﹩{\dot{M}}_{\mathrm{pe}}﹩, total mass-loss rate to photoevaporation-driven winds (Equation (30)). For comparison, we show the Eddington accretion rate ﹩{\dot{M}}_{\mathrm{edd}}\equiv {L}_{\mathrm{Edd},\bullet }/(0.1{c}^{2})﹩ of the BH/NS and the local Eddington accretion rate ﹩{\dot{M}}_{\mathrm{edd},\mathrm{in}}\equiv ({L}_{\mathrm{Edd}}/{c}^{2})({R}_{\mathrm{in}}/{R}_{{\rm{G}}})﹩ at R in. We also show the thermal time (Equation (13); vertical dashed line) and an approximate range of nuclear times (gray shaded region) of the stripped He core.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Physical properties of post-CE CBD in the space of local mass M d ≡ 2π r 2Σ and radius, calculated from vertical hydrostatic and thermal balance (Section 3). We adopt a density profile ﹩{\rm{\Sigma }}={{\rm{\Sigma }}}_{0}{\left(r/{R}_{{\rm{d}},0}\right)}^{-2}﹩, for an assumed R d,0 = 200R ⊙ motivated by Equation (4) and normalization Σ0 ≡ Σ(R d,0) related to the total disk mass M d,0 according to Equation (5). We otherwise adopt the parameters of the fiducial model: binary mass M bin = 20M ⊙, luminosity L bin = L Edd, viscosity α = 0.01, advective cooling parameter ξ = 1 (Table 1). We mark the characteristic initial disk radius R d,0 and the radius R g (Equation (29)) external to which photoevaporation mass loss becomes important as ticks along the bottom axis.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Similar to Figure 3 but shown for the fiducial model snapshot radial profiles of the ratio of gas pressure to total pressure (P gas/P;  top panel), the fraction of the disk heating due to irradiation from the binary (﹩{F}_{\mathrm{irrad}}/{F}_{\mathrm{total}}^{+}﹩, ﹩{F}_{\mathrm{total}}^{+}\equiv {F}_{\mathrm{irrad}}+{F}_{\mathrm{visc}};﹩ middle panel), and the ratio of the radiative cooling rate to the total cooling rate, i.e., the radiative efficiency (﹩{F}_{\mathrm{rad}}/{F}_{\mathrm{tot}}^{-}﹩, ﹩{F}_{\mathrm{total}}^{-}\equiv {F}_{\mathrm{rad}}+{F}_{\mathrm{adv}};﹩ bottom panel). The half-mass radius R m,1/2 is marked with a dot on each profile. The expanding disk evolves from a radiation-dominated, viscously heated, advectively cooled state at early times to an irradiation-supported, radiatively cooled, gas-pressure-supported state at late times.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Snapshots of the radial profiles of various properties of the CBD for the fiducial model (see Table 1). The location of the half-mass radius R m,1/2 is marked with a dot on each profile. The expansion of the disk can also be tracked in the plot of the mass accretion rate (lower left). Note that the inner boundary of the disk is dynamical: R in(t = 0) = 60 R ⊙ and R in(t ≈ 105 yr) ≈ 30 R ⊙.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Evolution of the binary total mass M bin, orbital angular momentum J bin, and semimajor axis a bin for the fiducial model. Note that we assume a circular, equal-mass binary at all times, as described in Section 3.2. We therefore neglect any mass or angular momentum loss due to winds from the accretion flow onto the NS/BH, though we explore the implications of such mass loss on the growth and accretion power of the compact object in Section 5.5. For comparison, we show the thermal time (Equation (13); vertical dashed line) and an approximate range of nuclear times (gray shaded region) of the stripped He core.
Paper: Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients
Authors: Semih Tuna, Brian D. Metzger
Figure caption: Schematic diagram of the post-CE system, showing the circumbinary disk surrounding the inner binary comprised of the stripped He core and BH/NS companion of separation a bin. The surface layers of the disk (shown in yellow, labeled HII) are irradiated and photoionized by the UV luminosity of the He core and the BH/NS disk, driving a wind from radii ≳0.1R g ≳ 1014 cm. During the late stages of evolution, the rate of wind mass loss becomes sufficiently high for the dense outflow to form dust (gray, crescent “clouds”), which efficiently absorbs the binary UV luminosity, reprocessing it to near-infrared wavelengths (Section 5.4). CBD-fed super-Eddington accretion onto the BH/NS drives a (trans)relativistic outflow/jet, powering a parsec-scale bipolar synchrotron radio nebula (Section 5.5).
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Differences between ﹩{t}_{\mathrm{expl}}^{\mathrm{peak}}﹩ and the first detection epoch for SNe 1998bw (γ-ray detection), 2006aj and 2008D (X-ray detection), and 2016gkg (shock-breakout detection). Error bars are ﹩1{\sigma }_{{t}_{\mathrm{expl}}^{\mathrm{peak}}}﹩ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Δm 15(V) as a function of Δm 15(x) for SNe IIb (blue circles), Ib (green squares), and Ic (red diamonds). Solid lines are linear fits to the data, and dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits around the fits. Error bars indicate ±1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Histograms of Δm 15(V) and ﹩{t}_{V}^{\mathrm{peak}}-{t}_{\mathrm{expl}}﹩. Dashed lines indicate mean values.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: B-band light curve of SN 1996cb, where the blue line is the ALR fit. Bottom panel: fit residuals, where dashed and dotted lines are the ±1σ and ±3σ limits, respectively. Error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:                          ﹩{t}_{V}^{\mathrm{peak}}-{t}_{\mathrm{expl}}﹩ vs. Δm 15(V). Solid lines are the best fits to the data, while dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits. Error bars are 68% errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Cumulative distributions for the ﹩{t}_{x}^{\mathrm{peak}}-{t}_{V}^{\mathrm{peak}}﹩ values. Dashed lines indicate mean values.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top row: peak time–luminosity relations for SE SNe. Solid lines correspond to the Khatami & Kasen (2019) relation (Equation (12)) fitted to observations (filled symbols), and dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits. Dotted lines correspond to Arnett’s rule. Second, third, and fourth rows: residuals against decline rate, ejecta mass, and kinetic energy, respectively, where the Pearson correlation coefficient is indicated in each panel. Error bars are 1σ errors, and arrows indicate lower/upper limits. We also show the models of Dessart et al. (2016) and Woosley et al. (2021) with empty symbols.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:                       ﹩\mathrm{log}{M}_{\mathrm{Ni}}﹩ estimates for SN 2009jf vs. the time since explosion, before (top panel) and after (bottom panel) correcting for the γ-ray deposition function. The solid horizontal line corresponds to the ﹩\mathrm{log}{M}_{\mathrm{Ni}}﹩ value that maximizes the posterior probability, while dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits. Error bars are 1σ errors due to uncertainties on photometry, while the red vertical bar depicts the 1σ error due to the uncertainty on μ, reddening, explosion epoch, and BC.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Empirical peak time–luminosity relation corrected for decline rate (solid black line) along with its ﹩\pm 1\,\hat{\sigma }﹩ region (gray region). The red dotted (blue dashed) line shows the effect on the empirical relation of decreasing E(B − V) by 0.15 mag (t expl by 5.8 days). Models of Dessart et al. (2016) and Woosley et al. (2021) are shown with empty symbols.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Empirical β values for SE SNe against peak time (left panel) and decline rate (right panel).
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Correlation matrix of the bolometric light-curve properties and explosion parameters. The Pearson correlation coefficient and the number of SNe (in parenthesis) are reported for SNe IIb (top values), Ib (middle values), and Ic (bottom values). Correlations with ∣r P∣ ≥ 0.5 are indicated with bold colored numbers.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Ejecta mass against decline rate (top panels) and 56Ni mass measured from the radioactive-tail luminosity against ejecta mass (bottom panels). Solid lines correspond to linear fits, while dashed lines are the ﹩\pm 1\,\hat{\sigma }﹩ limits. Arrows indicate lower/upper limits, and error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Change in ﹩\mathrm{log}{M}_{\mathrm{Ni}}﹩ against change in explosion time. Negative (positive) Δt expl values are quantities computed using ﹩{t}_{\mathrm{nondet}}﹩ (t detect) as explosion time. The solid line is a straight line fit and dashed lines are ﹩\pm 1\hat{\sigma }﹩ limits.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Peak time–luminosity relation for SE SNe, corrected (top panel) and uncorrected for decline rate (bottom panel). Solid and dotted lines are the best fits given by Equations (59) and (60), respectively, while dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits around the fits.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Histograms of the bolometric light-curve properties (left panels) and the explosion parameters (right panels). Dashed lines indicate mean values.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: IC 348 members and proper motion outliers. Top left: Gaia EDR3 proper motions of cataloged IC 348 members with a Gaia EDR3 parallax between 1.8 and 4.3 mas (gray points; see Section 2 for details) and proper motion outliers (colored symbols; filled symbols are members and open symbols are field stars or unclear). One additional proper motion outlier, J0340+3154 (short name; see the name description in Table 1.), is located at (62.2, −16.0) mas yr−1 and is out of the range of the panel. The yellow area covers three times the standard deviation of IC 348 members. The red circle shows 3.2 mas yr−1 deviation from IC 348, which corresponds to 5 km s−1 at 325 pc. Stars beyond the red circle are marked as proper motion outliers, except for a subgroup at pmRA ∼ 6.9 mas yr−1, pmDEC ∼ −9.4 mas yr−1. Top right: the current spatial location of IC 348 optical members (filled gray points; same as the left panel), cataloged IC 348 members without a Gaia EDR3 parallax measurement (unfilled gray points), and proper motion outliers (colored symbols). The proper motion outlier, J0340+3154, is located at (55.°0, 31.°9) and is out of the range of the panel. The magenta circle is the region containing half of the IC 348 members (Cantat-Gaudin & Anders 2020). Bottom: histogram of parallaxes for high-confidence members collected from Luhman et al. (2016) with a proper motion cut (gray histogram), compared with the parallaxes of proper motion outliers (colored symbols with no physical meaning of their position on the y-axis).
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Youth indicators to compare the proper motion outliers with YSOs and main-sequence stars. Top left: spectral type vs. X-ray luminosity of high-confidence IC 348 members (gray triangle) and proper motion outliers (colored symbols; filled symbols are members and open symbols are field stars or unclear). Upper limits are not included. The green line and shadow show the mean and standard deviation of Pleiades stars collected from Stelzer & Neuhäuser (2001); blue represents Hyades stars from Stelzer & Neuhäuser (2001), and orange represents main-sequence stars from Schmitt & Liefke (2004). The mean and standard deviation are calculated from stars within two subtypes. Vertical dotted line represents where the detection limit starts to dominate for Hyades stars under the spectral type roughly inspected from Freund et al. (2020). Top right: the distribution of apparent G-band magnitudes of high-confidence IC 348 members with X-ray detections (orange) and nondetections (blue). The black line shows the detection limit, where the nondetection of stars brighter than the limit leads to their classification as field stars. Bottom left: temperature vs. EW(Hα) of high-confidence IC 348 members (gray points); Sco–Cen members collected from Pecaut & Mamajek (2016; cyan points); Pleiades, Praesepe, and Hyades members collected from Fang et al. (2020; black points for Pleiades and green points for others); and IC 348 proper motion outliers (other colored symbols). Negative values are absorption lines, opposite of the usual convention. A proper motion outlier, LRL 70, has EW(Hα) = 159 Å, and hence is out of the range of this panel. Bottom right: temperature vs. surface gravity of Orion members and field stars collected from Kounkel et al. (2018; blue and orange points, separately), and IC 348 proper motion outliers (other colored symbols) with T eff and ﹩\mathrm{log}(g)﹩ from Kounkel et al. (2019). The red box region shows the area containing a high concentration of Orion members.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Temperature–luminosity diagram of high-confidence members of IC 348 (gray triangles), proper motion outliers (colored symbols), 2 Myr, 10 Myr, and 50 Myr PARSEC isochrone (v1.2S; dashed, dashed–dotted, and dotted black line, respectively), and 10 Myr Feiden (2016) nonmagnetic isochrone (orange line).