adsabs/AstroCLIMB huggingface dataset:
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Simulation setup for the numerical model. (a) Initial magnetic field configuration, showing the radial component of the magnetic field (grayscale), four flux systems (green, cyan, blue, orange) and the boundaries between them (red field lines, which meet at the null point). (b) Shearing profile (dBϕ/dt, green-brown shading) along the northernmost polarity inversion line (PIL).
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: The sky distribution ﹩{\dot{n}}_{511}(\phi ,i)﹩ for the C WD model (placed at 100 pc). The center of the “eye” in (a) is the inferior conjunction of the MSP (the MSP between the observer and the companion). Panel (b) shows the same fluxes as panel (a), projected onto the surface of a sphere, where a brighter spot means there is more 511 keV emission in that direction. The relative difference in flux of the center of the “eye” and bright ring correlates with the atomic number, Z, of the companion. Thus observations could constrain the companion’s composition. This effect is discussed in more detail in Section 3.2.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: Schematic of an MSP irradiating its companion with high-energy γ rays and charged particles. These primary particles bombard the surface of the companion, which are reprocessed into low-energy backsplash γ rays, low-energy e−e+ pairs, and 511 keV line emission that escape from the system. In the rightmost panel, x = 0 corresponds to the incident γ ray’s path, and z = 0 corresponds to the surface of the companion along that path.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: Primary incident (blue) and secondary emission for an irradiated He WD (orange) and Fe planet (green). The MSP spectrum is defined by Equation (1) with x = E/E0, E0 = 2 GeV, Γ = 1, d = 0.6, b = 0.9, and E is the incident γ-ray energy. This system is assumed to be 100 pc from Earth, and the pulsar luminosity is LMSP = 1034 erg s−1. The normalization for this spectrum is averaged over all emission directions, and the instantaneous spectrum can vary by viewing angle.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: The backsplash spectrum and radial Doppler shifts (for zero systemic/peculiar velocity), for an He WD–MSP binary 100 pc from Earth viewed edge on over the course of an orbit. Orbital phase = 0 corresponds to the inferior conjunction of the MSP (the MSP between the observer and the companion). The 511 keV line shifts by ∼1 keV, which could substantially increase the sensitivity of coherent searches for the line emission if the Doppler shift can be resolved.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: This figure charts the genealogy and evolution of 10,000 initial photons that result in escaping 511 keV photons for the C planet system. Each row is a generation and each branch represents a different path. The black vertex is the initial photon (“INIT”), green vertices are photons producing Compton scattered electrons (“COMP”), yellow vertices are electrons or positrons producing Bremsstrahlung photons (“BREM”), orange vertices are electron–positron annihilation to produce photons (“ANNI”), red vertices are photons producing electron–positron pairs (“PAIR”), and gray vertices are escaping 511 keV photons.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: ϵ is shown as a function of ﹩\frac{{\dot{n}}_{511}(0,\frac{\pi }{2})}{{\rm{\max }}({\dot{n}}_{511}(\phi ,\frac{\pi }{2}))}﹩ for each planetary model. All five models have the same density and radius with the only difference being the composition of the companion.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: Histogram of the dominant pathways for the escaped 511 keV photons for a representative C WD. These represent multiple generations of e−e+ pair production and γ-ray production through bremsstrahlung that concludes with e−e+ annihilation, creating an escaping 511 keV γ ray.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: Density profiles of the BD and MS stars calculated with MESA.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: The normalized 511 keV flux as a function of orbit for the five planet models at i = 90∘.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Global sensitivity analysis performed on a set of 4096 simulations with varying initial conditions (y-axis) and age of evolution (x-axis). Each panel quantifies the sensitivity an output parameter (final Prot, Porb, e) in terms of the amount of variance each input parameter contributes to the distribution of final parameters.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Global sensitivity analysis performed on a set of 4096 simulations with varying initial conditions (y-axis) and age (x-axis). Each panel quantifies the sensitivity of an output parameter (final Prot, Porb, e) in terms of the amount of variance each input parameter contributes to the distribution of final parameters.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Simulations of equilibrium tide (CTL) coupled with stellar evolution. Panels show the evolution of orbital period (left), rotational period (center), and eccentricity (right) for tidal τ strengths in the range ﹩-4.0\lt {\mathrm{log}}\,(\tau )\lt 1.6﹩. Tidal τ influences the timescale of synchronization and circularization, where higher tidal τ results in more rapid evolution. Each track originates from the same initial conditions for a 1M⊙–1M⊙ mass binary, and we vary only tidal τ to illustrate the effect of tides on the timescale of orbital evolution.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Exchange in energy (left panel) and angular momentum (right panel) between the rotation and orbit of stars in the binary system, as predicted by the CTL model (P. Hut 1981) when coupled with stellar evolution (I. Baraffe et al. 2015) and magnetic braking (S. P. Matt et al. 2015). Lost energy (red line, left panel) is due to tidal heating, and lost angular momentum (red line, right panel) is due to stellar winds. The black dashed line shows that energy and angular momentum remain conserved over time, showing that the coupling of our equations is behaving as expected.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 1, but with the CPL model. Panels show tidal ﹩{ \mathcal Q }﹩ strengths in the range ﹩4.0\lt {\mathrm{log}}\,({ \mathcal Q })\lt 9.0﹩. Tidal ﹩{ \mathcal Q }﹩ influences the timescale of synchronization and circularization, where lower tidal ﹩{ \mathcal Q }﹩ results in more rapid evolution.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: The estimated flux for the MSP binary systems in the ATNF Pulsar Catalogue. The BW and UL systems are modeled using three size assumptions, because their true density is unknown. (a) The companion radius is 6 × 108 cm. (b) The companion density is 10 g cm−3. (c) The companion density is 30 g cm−3. In any case where the Roche-lobe radius is less than the assumed radius, we use the Roche-lobe radius instead. The BW systems are the most promising known candidates for observation.
Paper: Irradiated Pulsar Planets and Companions as 511 keV Positron Annihilation Line Sources
Authors: Zachary Metzler, Zorawar Wadiasingh
Figure caption: Procedure for filtering for known systems and estimated 511 keV fluxes. Binary MSP systems were selected from those listed in the ATNF Pulsar Catalogue (R. N. Manchester et al. 2005) and its entry definitions. The systems are divided based on the “BINCOMP” column. Systems defined as “He” or “HeT” use the He WD model, those defined as “CO” use the C WD model, and those defined as “MS” happened to be RB systems with Porb < 2 days and used the MS model with the closest mass. The systems defined as “UL” or “ULT” were further divided into BWs, if Porb < 2 days, or UL otherwise.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 3, but for the CPL model.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Fraction of binaries that are synchronized (Porb/Prot1 ≈ 1, orange), subsynchronous (Porb/Prot1 < 1, blue), and supersynchronous (Porb/Prot1 > 1, green) according to the CTL model. The dotted lines show the systems evolved to an age of 1 Gyr, the dark solid lines show 5 Gyr, and the light solid lines show 10 Gyr. For each bin of ﹩{\mathrm{log}}\,\tau ﹩, we compute relative fractions of synchronous, subsynchronous, and supersynchronous in each sample for a given age. The shaded orange region shows the hypothetical lower bound on ﹩{\mathrm{log}}\,{ \mathcal Q }﹩ given that a majority of sources (>90%) are observed to be subsynchronous after 5 Gyr.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Samples from the simulated posterior for the CTL model at an early age of 50 Myr (blue points). The posterior function is sampled using a GP and active learning (K. Kandasamy et al. 2017) using the package alabi (J. Birky et al. 2025, in preparation) in order to visualize the structure of high posterior modes/degeneracies. Points are colored according to their posterior values. Since the posterior spans an order of magnitude range, we present these values as ﹩\hat{P}={\mathrm{log}}\,(-{\mathrm{log}}\,{ \mathcal P })﹩, where lower values of ﹩\hat{P}﹩ (darker blue) represent higher posterior probability. Orange dashed lines mark the true values of the initial parameters.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Distribution of orbital parameters for the CTL (top) and CPL (bottom) models evolved to an age of 5 Gyr, taken from the same simulations as Figures 5–  8. The blue scatterpoints show the initial distribution of parameters (sampled uniformly in eccentricity, orbital period, rotation period, and tidal τ or ﹩{ \mathcal Q }﹩), the black contours show the final distribution of parameters after 5 Gyr of evolution, and the orange range highlights synchronized binaries. At 5 Gyr, there is a clear bimodal separation between systems that are synchronized (Porb/Prot1 ≈ 1) and those that are subsynchronous (Porb/Prot1 < 1).
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 10, but for the CPL model. The shaded orange region shows the hypothetical lower bound on ﹩{\mathrm{log}}\,{ \mathcal Q }﹩ given that a majority of sources (>90%) are observed to be subsynchronous after 5 Gyr. The shaded blue region shows the hypothetical upper bound ﹩{\mathrm{log}}\,{ \mathcal Q }﹩ given that a majority of sources (>90%) are observed to be subsynchronous after 5 Gyr.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 12, but for 5 Gyr.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 14, but for 5 Gyr.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Likelihood sensitivity for the CTL (top) and CPL (bottom) models. The results for both models indicate that the model goodness-of-fit (as quantified by a Gaussian likelihood, with uncertainties described in Section 3.2) is most sensitive to the initial orbital period.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 12, but for the CPL model.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Sensitivity of the period ratio (orbital period/primary rotation period) for the CTL (top) and CPL (bottom) models. At ages 5–10 Gyr, τ and ﹩{ \mathcal Q }﹩ dominate the final period ratio Porb/Prot1.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Simulated one-dimensional likelihood for CTL (left) and CPL (right) models evaluated at an age of 50 Myr. Each of the colored lines shows the likelihood value as a function of varying τ or ﹩{ \mathcal Q }﹩ for different “true” values (−3, −2, −1, 0, +1) for τ, and (4, 5, 6, 7, 8) for ﹩{ \mathcal Q }﹩. For both plots, blue lines represent weaker tides and red lines represent stronger tides. The y-axis shows the likelihood value when τ is allowed to vary and is compared to the fiducial simulation (with the values of Table 4, and uncertainties of Table 3). On the y-axis, we compress the magnitude range for visualization by showing the likelihood as ﹩{\mathrm{log}}\,(-{\mathrm{log}}\,{ \mathcal L })﹩, where lower values of ﹩{\mathrm{log}}\,(-{\mathrm{log}}\,{ \mathcal L })﹩ (higher on the y-axis) represent higher likelihood values (similar to Figures 12–            15). The magenta dashed line and arrows indicate the range of tidal values that are strong enough to cause tidal locking by an age of 50 Myr. Similarly, the cyan arrows and shaded regions show the range of tidal values that are strong enough to cause synchronization, and the gray arrows and shaded regions show the range of tidal values that are strong enough to cause circularization.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Examples showing how solutions with different ﹩{\mathrm{log}}\,\tau ﹩ are degenerate at different ages. The black line highlights the solution for ﹩{\mathrm{log}}\,\tau =0﹩. The thick gray vertical lines mark the ages 50, 500, and 5 Gyr as used in Figures 18–           20. The colored dashed lines show the solutions for the secondary likelihood peak at each age: at 50 Myr, the likelihood has peaks at ﹩{\mathrm{log}}\,\tau =0﹩ and −1.73; at 500 Myr, the likelihood has peaks at ﹩{\mathrm{log}}\,\tau =0﹩ and −2.17; and at 5 Gyr, the likelihood has peaks at ﹩{\mathrm{log}}\,\tau =0﹩ and 0.66. The color scale is consistent with Figures 1–2 and 18–           20, where darker red represents stronger tides and darker blue represents weaker tides. The colored dots highlight where the evolutions intersect.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Samples from the simulated posterior for the CTL model at a late age of 5 Gyr (from Figure 13) zoomed in on the marginal distribution of initial orbital period and eccentricity. The dashed orange line shows the true initial orbital period that would be unknown, and the green dashed line shows the final orbital period that would be observed. The solid lines show the curve of Porb,i and ei for a constant value of orbital angular momentum. The orange solid curve shows the initial orbital angular momentum (Jorb,i = 1.80 × 1045 kg m−2), and the green solid line shows the final orbital angular momentum (Jorb,f = 1.61 × 1045 kg m−2). Instead of converging to the true initial orbital period, the posterior is biased toward picking solutions with Porb,i ≈ Porb,f (as seen by the overlapping horizontal dashed lines). Furthermore, we see that the high posterior samples lie along the curve of final orbital angular momentum, meaning that the posterior is more informative of the final conditions than it is of the initial conditions that we are trying to infer.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 16, but for the CPL model. Two degeneracy features emerge from the blue sampled posterior points: those flat across eccentricity with Porb,i ≈ Porb,f (with negligible values of tidal dissipation), and those with curved Porb,i–ei degeneracy (with stronger values of tidal dissipation).
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 18, but for 5 Gyr.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Orbital and rotational evolution for randomized initial conditions with strong tides (orange, ﹩{\mathrm{log}}\,\tau =0﹩) and weak tides (blue, ﹩{\mathrm{log}}\,\tau =-2﹩). Axes plot the rotation period (days), orbital period (days), and eccentricity. The dashed portion of the lines shows the trajectory before rotational torque balance, and the solid portion shows after. At rotational torque equilibrium (i.e., when tidal torque balances with magnetic braking), evolution trajectories converge to the shaded manifold, in which all (Porb, Prot, e) solutions are constrained to a very precise two-dimensional subspace of three dimensions.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Evolution of the Porb/Prot ratio for the primary star in a 1M⊙–1M⊙ binary system assuming only CTL tides. The system is evolved with an initial eccentricity of e = 0.2 and initial rotation periods of Prot,1 = Prot,2 = 0.5 day for different initial orbital periods: 5 days (left), 10 days (middle), and 15 days (right).
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 21, but for the CPL model. In Figure 20, the solution for ﹩{\mathrm{log}}\,{ \mathcal Q }=8﹩ shows a double peak in likelihood. The black line highlights the solution for ﹩{\mathrm{log}}\,{ \mathcal Q }=8﹩. The blue dashed line shows the solution for the secondary likelihood peak: at 5 Gyr the likelihood has peaks at ﹩{\mathrm{log}}\,{ \mathcal Q }=8﹩ and ﹩{\mathrm{log}}\,{ \mathcal Q }=6.78﹩.
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same as Figure 18, but for 500 Myr.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Results of FitTeD-XSPEC fitting to GSN 069 data, including seven X-ray spectra and two UV spectra from 2010 to late 2019. Top: evolution of the 0.3–2.0 keV X-ray luminosities (gray) and UV luminosities at 2000 Å (blue). Shaded regions represent the model-predicted values, at the 68% credible intervals, while the data points show realizations at the observed epochs. Gray symbols indicate data from XMM-Newton (diamonds), Swift/XRT (circles), and the XMM-Newton slew survey (star). Note that the slew survey data were not included in the fit, but are nonetheless reproduced by the model within uncertainties. Bottom: SEDs at the epochs of the XMM-Newton observations (and HST, in 2014 and 2018). The left panel shows observed fluxes (including absorption and extinction), while the right panel shows intrinsic luminosities corrected for both. In both panels, the X-ray spectra are unfolded to the maximum a posteriori solution.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Evolution of the physical properties of GSN 069’s accretion disk. Left: time evolution of key disk properties, from top to bottom: monochromatic luminosities, Eddington ratios, and surface density (at ISCO and at rorb, see Section 4.3). Right: disk properties at representative epochs: SED (top), radial temperature profile (middle), and radial surface density profile (bottom). Different colors correspond to distinct epochs as defined in Table 1.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Schematics of the implementation of relativist time-dependent disk framework into FitTeD; from the seven free parameters, to the disk’s SED as a function of time. See the text in Section 2 for details.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Corner plot of the marginalized posterior from the FitTeD-XSPEC fit of GSN 069. The contours are 68% and 99% credible regions.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Comparison between the results of the time-dependent modeling (FitTeD-XSPEC) and the SED fitting from Paper I. The gray shaded region indicates the “effective outer radius” from the time-dependent fit, defined as the radius where the surface density drops to 1% of its maximum value. The two purple error bars represent the Rout estimates from the “high-spin mode” of the 2014/2018 SED fitting presented in Paper I.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Inferred Eddington-normalized mass accretion rate of GSN 069 as a function of time. The red line illustrates the apparent transition value between the presence (absence) of QPE at low (high) accretion rates. Figure inspired by G. Miniutti et al. (2023a). The observed behavior is the opposite of predicted by disk instability models.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Schematics of the ray-tracing geometry. The coordinates bx and by lie in the observer plane; x and y in the disk plane. A schematic photon trajectory from the inner disk is shown, and the observer-disk inclination angle is denoted i.