adsabs/AstroCLIMB huggingface dataset:
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: The inferred magnetic field strength, ∣B∣ (top row), and the azimuthally averaged angle between the magnetic field and the line of sight, θB (bottom row). The left column shows the results when adopting a disk-centric description of the magnetic field where θ varies as a function of ϕ, while the right column shows the same when assuming an environmental field where θ is constant. The error bars represent the 16th or 84th percentile range about the posterior median. Gray points show radii where Zeeman broadening cannot be robustly identified as the source of broadening, as discussed in Section 3.4. The vertical dashed line and gray shaded region show the location of the outer continuum gap reported by J. D. Ilee et al. (2022) and S. Das et al. (2024).
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Excitation conditions derived from the fitting of the spectra in addition to the magnetic field properties plotted in Figure 4. The blue and red points show the disk-centric and environmental parameterizations of the magnetic field, respectively. For the local gas density, the arrows represent lower limits to this value, essentially the critical density of the N = 1–0 transition for the given temperature and column density. The gray dashed line for the nonthermal width component represents the 0.08cs prior, while the two horizontal lines in the convolution kernel panel show 1 and 2 times the channel spacing of 80 m s−1.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: The posterior distributions of θB and ϕB across the radial region where the magnetic field was robustly detected. Is is clear that the field transitions from predominantly poloidal (θB = 0°) at ﹩1\mathop{.}\limits^{^{\prime\prime} }1﹩ to one in the plane of the disk (θB = 90°) by ﹩1\mathop{.}\limits^{^{\prime\prime} }5﹩. Across this radial range, there is no clear preference for a ϕB value, with the posterior distribution equally sampling the allowed range as shown in the histograms in the top row.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Demonstrating the different responses to changing the magnetic field strength (left column) and orientation (right column) that the most sensitive hyperfine component (red) and the least sensitive hyperfine component (blue) exhibit. The top row shows the change in line width, as measured by the fit of a Gaussian line profile. The bottom row shows the deviation from a Gaussian line profile, quantified by fG, which describes the fraction of the total intensity that can be described by a Gaussian profile. The other seven hyperfine components will have profiles that fall between these two limiting cases.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Plotting the temperature required to explain the observed line width for each hyperfine component when considering different underlying magnetic field strengths, shown by different colors, and a different CN column density, shown by different line styles. As the sensitivity of a line to Zeeman splitting is independent of the optical depth, lines with middling optical depths are observed to broaden more. The rise and fall in the effective kinetic temperature as a function of optical depth indicates that an unrealistic vertical temperature gradient would need to be invoked in order to explain the observed ratio of line widths without the use of Zeeman splitting.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Showing how the ratio of line widths between the most sensitive hyperfine component and the least sensitive hyperfine component changes as various parameters of the model are increased. Only when the magnetic field strength, ∣B∣, is increased does the ratio increase; for all other parameters, the ratio decreases. This suggests that the signature of Zeeman splitting cannot be mimicked by other model properties. The parameter ranges for the four properties are 0–50 mG for ∣B∣, 20–50 K for Tkin, 0–80 m s−1 for FWHMconv, and 11–15 for ﹩{\mathrm{log}}\,(N({\rm{CN}}))﹩.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Lower limits to the plasma β in the vertical region from where the CN emission emanates, where the median of the β posteriors were plotted. The blue and red points represent the disk-centric and environmental field morphologies, respectively, while the more transparent points are where Zeeman broadening cannot be robustly inferred.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Example of the velocity-deprojected spectrum at ﹩1\mathop{.}\limits^{^{\prime\prime} }4﹩ (gray points with the black line showing a running median with a kernel width of 80 m s−1) and the best-fit model including a disk-centric magnetic field morphology in blue. The model is able to reproduce the data with exceptional fidelity.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: A comparison of the posterior probability distribution for the magnetic field strength at each radial location. Each panel shows the posteriors for the disk-centric parameterization in blue, while the two gray posteriors are for the same model but when the Zeeman sensitivities of the two most sensitive hyperfine components are swapped with the two least sensitive hyperfine components. If the “correct” mapping of sensitivities finds a higher magnetic field strength than the “mixed” mapping, then this is strong evidence that it is truly Zeeman broadening that is observed. Panels where the medians of the distributions are separated by less than the quadrature sum of the standard deviations of the distributions are colored in gray. This appears to be the case for separations ≳2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5. Note that for most radii, the two “randomized” models have posteriors that overlap and cannot be distinguished.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Same as Figure 13 but for the environmental field morphology.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: The posterior distributions for the collider density at each radius. The vertical dashed lines show the inferred lower limit to the density based on the median value of a Gaussian cumulative probability distribution function fit to the distribution.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Example corner plot showing the posterior distributions and covariances for the disk-centric model at ﹩1\mathop{.}\limits^{^{\prime\prime} }4﹩. No significant correlations are found between parameters.
Paper: On the Search for a Generation Mechanism for the Ion Acoustic Waves Observed by the Parker Solar Probe
Authors: Sergio E. Vidal-Luengo, David M. Malaspina, Stefan Eriksson
Figure caption: Real time proximity observations' comparison with Monte Carlo–generated distributions. Left subplots ((a), (c), and (e)) show the real proximity observations between IAWs with current sheets (CS), reconnection exhausts (RE), and ion speed streams (ISS), while subplot (g) shows the real proximity observations between ion speed streams and current sheets. The right subplots ((b), (d), (f), and (h)) show the comparison between real observations percentile location (red dots in standard deviation units) with respect to the simulated distributions for each one of the previously mentioned cases. The blue line corresponds to the limit where the comparison is valid due to the nature of the construction of the pseudocatalogs as results of the binning necessary to replicate the real distributions.
Paper: On the Search for a Generation Mechanism for the Ion Acoustic Waves Observed by the Parker Solar Probe
Authors: Sergio E. Vidal-Luengo, David M. Malaspina, Stefan Eriksson
Figure caption: (a) Burst data example of IAWs using time period from D. M. Malaspina et al. (2024). (b) Burst data example of IAWs using time period from F. S. Mozer et al. (2021). (c) Survey data example from D. M. Malaspina et al. (2024). (d) Survey data example from F. S. Mozer et al. (2021).
Paper: On the Search for a Generation Mechanism for the Ion Acoustic Waves Observed by the Parker Solar Probe
Authors: Sergio E. Vidal-Luengo, David M. Malaspina, Stefan Eriksson
Figure caption: (Left) Example of current sheet detection using the PVI method. (Right). Example of ion speed stream detection using the PVI method. The black curve represents the envelope for the maximum PVI.
Paper: On the Search for a Generation Mechanism for the Ion Acoustic Waves Observed by the Parker Solar Probe
Authors: Sergio E. Vidal-Luengo, David M. Malaspina, Stefan Eriksson
Figure caption: (Left) Histogram of IAW waiting times. (Right) RMSE of the fitting.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: Gaia astrometric parameters and color–magnitude diagram for RSG 5 and RSG 5-WD. Left panel: (A) the color–magnitude diagram (BP − RP vs. G band) of the star cluster with isochrone fits. The solid blue line represents the fit for an age of 35 million years (Myr), while the dashed blue lines represent the fit for ages of 30 Myr and 40 Myr. The black dots represent the member stars of the star cluster, while the red pentagram represents RSG 5-WD. The black arrows indicate the positions of the main-sequence turn-off and the main-sequence turn-on. (B) Spatial coordinate distribution of RSG 5 members and RSG 5-WD. (C) Proper motion distribution of RSG 5 members and RSG 5-WD. (D) Parallax distribution of RSG 5 members and RSG 5-WD. (E) The histogram represents the probability distribution of the RV of the magnetically trapped half-ring of ionized circumstellar debris, calculated in A. A. Cristea et al. (2025). The red dashed line indicates the average RV of the RSG 5 member stars, and the shaded area represents the 3σ level uncertainty. Right panel: (F) the solid lines represent the theoretical cooling tracks for WDs with masses ranging from 0.6 to 1.28 M⊙, while the black solid line indicates the 60 Myr cooling age track, both based on a thick-hydrogen carbon-oxygen model. The vertical dashed lines mark the boundaries of the ZZ Ceti instability strip.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: An example illustrating how binary interaction can result in the formation of the observed white dwarf within 35 Myr. (A) The evolution of the binary star on the Hertzsprung–Russell diagram from the BSE result. (B) The evolutionary flow chart according to the BSE result. In the flow chart, the full name of the corresponding abbreviation: MS + RD: main sequence + red dwarf; RLOF: Roche-lobe overflow; 1st CE: first common envelope phase; He Star + RD: helium star + red dwarf; Case BB RLOF: case BB Roche-lobe overflow (the mass loss of a helium star due to Roche-lobe overflow); 2nd CE: second common envelope phase; WD: white dwarf. (C) The evolution of the binary star on the Hertzsprung–Russell diagram from MESA (terminated at WD+RD stage due to MESA’s merger resolution limits). (D) The evolutionary flow chart. In the flow chart, the full name of the corresponding abbreviation is the same as panel (B).
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: RSG 5-WD spectrum with Zeeman components of hydrogen indicated. (A) The blue section spectrum of RSG 5-WD from the Keck I telescope. (B) The wavelength as a function of magnetic field for the hydrogen lines. The green line represents the hydrogen absorption lines in the spectrum, and the shaded area indicates the corresponding magnetic field range. (C) Same as (A), but for the red section spectrum. (D) The Hα emission line range. The red solid line represents a double Gaussian fit to the double-peaked Hα emission line, while the dashed lines indicate the corresponding peak positions. (E) Same as (B), but for the red section spectrum. The average fit magnetic field strength is about 210 MG.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: RSG 5-WD light curve and power spectrum. (A) ZTF g-band light curves folded with a period of 6.556 minutes. The square markers represent binned data, where every 20 points are averaged into a bin. (B) Same as (A), but for r-band light curves. (C) The power spectrum in the g band. The gray shading highlights the frequency corresponding to the maximum value of the power spectrum. (D) The power spectrum in the r band.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: Comparison of RSG 5-WD system ages and physical parameters under three different IFMR. Upper panel: the MIST IFMR from J. D. Cummings et al. (2018); middle panel: the PARSEC IFMR from J. D. Cummings et al. (2018); lower panel: the IFMR from P. Marigo et al. (2020). The physical parameters include main-sequence age (MS age), cooling age, total age, initial mass, and final mass.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: The phase-resolved spectra of RSG 5-WD. (A) The blue-end spectra from program C266. We arranged the spectra in order of phases from top to bottom, and the percentage represents the relative flux ratio, where the reference spectrum is set to 100%. (B) The red-end spectra program C266.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: Phase-averaged spectrum with the best-fitting blackbody model. The black line represents the spectra of RSG 5-WD from Keck, the red line indicates the best-fit result, and the yellow shaded area represents the 25%–75% confidence interval based on the MCMC fitting.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: Corner plots. Corner plots for parameter estimates based on Gaia photometry.
Paper: A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr
Authors: Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge, Chengyuan Li
Figure caption: Initial binary mass combinations capable of producing a CO white dwarf. Red points represent those combinations that yield a CO WD with a mass between 1.02 and 1.06 M⊙. The outcome of all these combinations is a single WD, with its companion having been engulfed during the most recent common envelope phase. The colors represent the final mass of the WD produced by these binary combinations. Note that each point in the figure actually represents many overlapping points, each with different initial periods, resulting in WD masses that vary accordingly (thus, the color represents only the outcome for one of the periods).
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Locations of our suite of disk models in the space of surface density Σ and disk angular velocity Ω. Purple circles indicate those models that undergo runaway cooling and fragmentation (Section 3.3), while a blue symbol denotes the single simulation that evolved into a quasi-steady state supported by gravitoturbulence (Section 3.2). Shown for comparison with solid colored lines are contours of the dimensionless neutrino cooling timescale τcool,0. We see that τcool,0 ≲ 10 (below the red solid line) delineates our fragmenting models. Also shown are contours of the local mass accretion rate ﹩\dot{M}﹩ (Equation (12); black solid lines) and the local clump mass unit ∼ Jeans mass in solar masses (Equation (13); blue dashed lines). Along the top horizontal axis, we show the disk radius in gravitational radii rg ≡ GM•/c2 for a central BH of mass M• = 3 M⊙.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Properties of the self-bound clumps from the fragmenting simulation O16T1.5e10. Top panel: mass histogram. Middle panel: average Ye (left axis) and associated Chandrasekhar mass MCh(Ye) (right axis; Equation (1)). Clumps in the gray shaded region have masses ≳MCh and hence are expected to continue to collapse to form NSs. Bottom panel: average density in units of the initial midplane density.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: For the fiducial slow cooling (nonfragmenting) simulation, a typical snapshot showing the (x, y) profiles through the midplane (z = 0) of density, temperature, local cooling time, equilibrium electron fraction, and chemical potential. Lengths are expressed in units of the vertical scale height H.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: For the fiducial slow cooling (nonfragmenting) simulation, a typical snapshot showing vertical (x, z) profiles through the y = 0 plane of density, temperature, local cooling time, equilibrium electron fraction, and chemical potential. Lengths are expressed in units of the vertical scale height H.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Final snapshot of the vertical (x, z) structure of density, temperature, dimensionless cooling time, electron fraction Ye, and electron degeneracy parameter μ/kT taken along a constant y = −3 slice from the fragmenting simulation O16T1.5e10. Lengths are expressed in units of the vertical scale height H.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Similar to Figure 4 but showing a slice through the midplane from the end of the fragmenting simulation O16T1.5e10. Lengths are expressed in units of the vertical scale height H.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Effective strain amplitude as a function of frequency hc(f) (Equation (B15)) for a subsolar NS–NS (dashed blue line) and subsequent NS–BH merger (dashed orange line) in a collapsar disk at a distance of 100 Mpc. We have assumed two NSs of equal mass M = 0.1 M⊙ merging with a central BH of mass M• = 3 M⊙. The NS binary is assumed to start from an initial separation equal to the Hill radius rH (Equation (B3)) and orbits at a distance r = 200 Rg from the BH. For comparison, we show the approximate 1σ sensitivity of current and third-generation ground-based GW observatories (F. Iacovelli et al. 2022a, 2022b) If an appropriate signal template can be constructed, the square of the signal-to-noise of an event is represented as the area between hc and detector noise on a log-f plot. For details, see Appendix B.
Paper: Gravitational Instability and Fragmentation in Collapsar Disks Supports the Formation of Subsolar Neutron Stars
Authors: Yi-Xian Chen, Brian D. Metzger
Figure caption: Electron/positron pressure fraction (left panel), thermal cooling time tcool in seconds (middle panel), and ratio of the electron capture timescale ﹩{t}_{\mathrm{cap}}﹩ (Equation (A18); right panel) in the ρ–T space. The fact that tcapt ≪ tcool throughout the majority of the parameter space suggests that electron capture reactions are typically fast compared to the cooling rate of the plasma, justifying our assumption of an equilibrium electron fraction in the disks of interest where neutrino cooling is relevant. A red dotted line again denotes the contour ﹩{ \mathcal G }=1﹩ (Equation (A10)) corresponding to significant α-particle formation.