adsabs/AstroCLIMB huggingface dataset:
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: For NOAA AR 12902 on 2015 September 26, the O I 1355 Å line width in km s−1, the intensity at 2800 Å (formed in the photosphere), and the O I 1355 Å intensity. Black contours are based on intensity thresholding of photospheric bright points in the 2800 Å spectroheliogram. The O I 1355 Å intensity is scaled from 3 to 40 DN.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: For NOAA AR 12902 on 2015 September 26, the JPDF (top panel) between the O I 1355 Å line width in km s−1, and the intensity at 2800 Å (formed in the photosphere) for a subset of the plage region studied in Figure 17. The JPDF only includes locations for which the O I 1355 Å intensity is larger than 10 DN (to avoid noisy profiles with uncertain or inaccurate line widths) and for locations that are within the red contours shown in the spectroheliogram at 2800 shown in the bottom panel.
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Final ejected mass vs. final ejected  56Ni mass of this study (gray circles) compared to observations (blue crosses) and other studies: Kromer et al. (2015; fuchsia downward-pointing triangles) and Lach et al. (2022a; pink upward-pointing triangles).
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Fraction of material of R28 burned to IGE (ϕ qn) at 2.0 s of simulation time. The curvature of the plumes due to the cylindrical geometry of the setup is apparent.
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Comparison of R32 (left panels, least ejected  56Ni mass) and R20 (right panels, most ejected  56Ni mass) over time. The (a) initial flame, (b) fraction of material burned to IGE at 3 s, (c) fraction of material burned to IGE at 20 s, and (d) density at 20 s are shown.
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Final total  56Ni vs. IGE yield of this study with a deflagration explosion mechanism (gray circles) compared to Augustine et al.'s (2019) study with a DDT explosion mechanism (gray crosses).
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Final ejected KE vs. final ejected mass of this study (gray circles) compared to observations (blue crosses) and other studies: Kromer et al. (2015; fuchsia downward-pointing triangles) and Lach et al. (2022a; pink upward-pointing triangles).
Paper: Dimming the Lights: 2D Simulations of Deflagrations of Hybrid C/O/Ne White Dwarfs Using FLASH
Authors: Catherine Feldman, Nathanael Gutierrez, Ellis Eisenberg, Donald E. Willcox, Dean M. Townsley, Alan C. Calder
Figure caption: Total unbound KE (in 1049 erg) vs. total unbound mass (in M ☉) of each realization. The colored points show the same feature highlights as Figure 4.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: The contours of the expected number of burst events in the LISA experiment in the n-﹩{M}_{\mathrm{lim}}﹩ plane. The red line denotes the example of future prospect of burst events per year detected by LISA. The blue dashed line is the boundary that divides the n-M lim plane into two regions where the minimum SMBH mass at z = 6 is lighter than 104 M ⊙ (upper side) or not (lower side).
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Hardening timescales with different M BH,tot as a function of redshift. From top to bottom, the hardening timescales are for M BH,tot = 103 M ⊙, 104 M ⊙, 105 M ⊙, and 106 M ⊙, respectively. For comparison, the thick solid line (blue) shows the Hubble time as a function of z and the thin solid line (black) corresponds to the Hubble time at z = 0.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Theoretical predictions of SGWB A (left panel) and the event rate of GW bursts N mgr (right panel) for the different dynamical friction timescale given by Equation (A1).
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Theoretical predictions of SGWB amplitude A at f = 1yr−1 (left panel) and the event rate of GW bursts N mgr (right panel), including the effect of the hardening phase.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: The optical spectrum of CPD −29 2176 shown in red (upper spectrum), with a comparison to the B0V star τ Sco from the ESPaDOnS archive shown as a blue line. The spectra are offset for clarity, and the spectrum of τ Sco was shifted in radial velocity to match the γ-velocity of the binary presented by Richardson et al. (2023). In the lower panel, we also show the Hα profile scaled down by a factor of 10 for clarity.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: The Fourier analysis of each sector of the TESS data shown in different colors and line styles. The negative-valued black spectrum represents the Fourier analysis of the light curve containing all four sectors. We also note some frequency groups with the designations g0, g1, and g2 on the top.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: The long-term photometric variability of CPD −29 2176 as observed with ASAS as well as the Fourier spectrum of the light curve. The Fourier spectrum shows a timescale of 600–700 days, but the light curve is not periodic as it does not phase into these periods.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: Equivalent Width measurements of CPD −29 2176 for the optical hydrogen lines.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: Equivalent Width measurements of CPD −29 2176 for the two strong optical helium lines we measured.
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: The short-term variability of CPD −29 2176 as observed by TESS. Each of the four sectors of TESS photometry is shown in a separate panel as indicated.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: Combined normalized distribution functions of the primary population of ISN H from all entry points at 100 au. Panels from left to right show the parallel and two perpendicular components. The bulk speed is subtracted from the parallel component, and positive parallel speeds correspond to atoms moving faster than the bulk flow toward the Sun. The top and bottom rows present the results obtained without and with accounting for the AS in collisions. The red histogram presents the results of the Monte Carlo simulations, and the blue and green lines show the analytic model derived in Appendix B, and the Maxwell approximation (Table 1), respectively. The shape of the Maxwell distribution in the pristine VLISM (T = 7500 K) is shown with a dashed gray line.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: Model predictions based on aFINM2019 (black circles) and modified aFINM for the two cases with (green squares) and without (blue triangles) AS compared to IBEX-Lo observations (red circles) of ISN H for the year 2011 (E-Step 1, spin bin 14). The black line is the Gaussian fit to aFINM2019 and the red line is the Gaussian fit to IBEX data. The dashed black line shows the peak longitude of the ISN H signal and the gray area shows the uncertainty region.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: ISN H flow peak longitude based on IBEX observations at spin bin 14 (84° from the NEP). Blue triangles with error bars are found by fitting a Gaussian function to the ISN H signal for the years 2009–2012 and 2017–2018. Blue x marks used for the years 2013 and 2014 are obtained based on the highest observed data points. Bottom panel: μ eff obtained based on our analysis for aFINM2019 (black), modified aFINM without AS (red), and with AS (green) circles with error bars for the spin bin 14 data. The black line represents μ 0 based on Kowalska-Leszczynska et al. (2018b; IKL).
Paper: Optical Properties and Variability of the Be X-Ray Binary CPD-29 2176
Authors: Clarissa M. Pavao, Noel D. Richardson, Jonathan Labadie-Bartz, Herbert Pablo, André-Nicolas Chené
Figure caption: The maximum observed Hα equivalent width compared to the orbital period for Be XRBs. We highlight CPD −29 2176 and LS I + 61 303.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: The μ eff obtained from our analysis for aFINM2019 (black), modified aFINM without AS (red), and with AS (green) circles with error bars for spin bins 14 and 15 data vs. total irradiance. The linear correlation between μ 0 from (Kowalska-Leszczynska et al. 2018b; IKL) and total irradiance is shown by the blue line with light blue the uncertainty region. The black, red, and green lines represent the linear fit to black, red, and green data points respectively. The data points presented by x marks are not included in the linear fit as they are associated with the years 2013 and 2014 where a χ 2 analysis is not possible. The gray uncertainty region is associated with aFINM2019 (black line).
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: Model predictions based on aFINM2019 compared to IBEX-Lo observations of ISN H for the year 2011 (E-Step 1, spin bin 14) adopted from Rahmanifard et al. (2019). The green and orange lines show model predictions for actual IBEX observations and Sun-pointing Earth location and reference frame. The black line is the Gaussian fit to model predictions averaged over the times when IBEX data is available (black data points) and the red line is the Gaussian fit to IBEX data (red data points). The dashed black line shows the peak longitude of the ISN H signal and the gray area shows the uncertainty region.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: As in Figure 1, but for the secondary population.
Paper: The Effect of Angular Scattering Imposed by Charge Exchange and Elastic Collisions on Interstellar Neutral Hydrogen Atoms
Authors: F. Rahmanifard, P. Swaczyna, E. J. Zirnstein, J. Heerikhuisen, A. Galli, J. M. Sokół, N. A. Schwadron, E. Möbius, D. J. McComas, S. A. Fuselier
Figure caption: As in Figure 5 but for spin bin 15 (90° from the NEP).
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: The mass relation between DM halo and SMBHs at z = 6. We plot our initial mass relation obtained from the halo merger tree and Equation (2) with ﹩{M}_{\mathrm{lim}}=1.0\times {10}^{8}{M}_{\odot }{h}^{-1}﹩ as colored triangles. The different color represents the different power-law index n in Equation (2); n = 1.0 in blue, n = 1.4 in orange, and n = 1.8 in green. The faint black and red small circles represent the observed mass relation at z = 0 and z = 6 (Shimasaku & Izumi 2019), respectively. We also plot the local relation given by Ferrarese (2002) in a black dotted line.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: The mass relation between DM halos and SMBHs at z = 0. The upper three panels show the dependence on the power-law index n with the fiducial ﹩{M}_{\mathrm{lim}}=1.0\times {10}^{8}{M}_{\odot }{h}^{-1}﹩ and the lower three panels show the dependence on the minimum halo mass ﹩{M}_{\mathrm{lim}}﹩ with n = 1.4. In each panel, colored circles represent the mass relations in the simulation, and the colored dashed line is the fitting power-law line for the simulation result at z = 0. The faint, small black circle and the black dotted line are the same as in Figure 3. Also, in all panels, we plot the initial mass relation at z = 6 with the colored triangles.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Comparison of the theoretical predictions in our coevolution model and the PTA observational results. The left panel shows the theoretical predictions of the characteristic strain in the cases with n = 1.0 (blue), 1.4 (orange), and 1.8 (green) for ﹩{M}_{\mathrm{lim}}=1.0\times {10}^{8}{M}_{\odot }{h}^{-1}﹩, and the upper bound obtained from the PPTA project (Shannon et al. 2015) is represented by a triangle. We also include the possible signal of SGWB corresponding to the common-spectrum process reported from the recent NANOGrav experiment (Agazie et al. 2023a) represented by the red band and the sensitivity curve expected for the future PTA experiment by SKA with the black dashed–dotted line (see, e.g., Campeti et al. 2021). The right panel shows the contours of the amplitude of the characteristic strain at f = 1yr−1 on the n-﹩{M}_{\mathrm{lim}}﹩ plane.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Illustration for the merger of two systems (DM halos with SMBHs) in our model. The heavier system consists of a DM halo with mass M H (a dashed circle in red) and two SMBHs (black-filled circles with red outlines). One SMBH is at the center of the DM halo, and the other SMBH is falling to the center. The lighter system includes a DM halo with mass M L (a dashed circle in blue) and an SMBH at the center (black-filled circles with blue outlines). Through the DM halo merger, a new system has a DM halo with mass M H + M L (a dashed circle in navy) and two SMBHs coming from the heavier system (one is at the center, and the other is falling to the center). If P < 0.3, we neglect the SMBH from the lighter system in the new system (the left branch). Otherwise, we assume that the lighter system is falling into the center of the new system with the dynamical friction timescale determined by P and leads to the SMBH coalescence.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: The characteristic strain amplitude of the SGWB from SMBH binaries for the cases with n = 1.0 (left) and 1.4 (right). ﹩{M}_{\mathrm{lim}}=1.0\times {10}^{8}{M}_{\odot }{h}^{-1}﹩ is fixed. The upper and lower panels show the contribution from each mass bin and each redshift bin, respectively.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: The distribution of the expected number of burst events that would be detected in the LISA with respect to the peak frequency. The left panel shows the dependence on the power-law index in our coevolution model with fixing ﹩{M}_{\mathrm{lim}}=1.0\times {10}^{8}{M}_{\odot }{h}^{-1}﹩. The right one shows the result of changing the limiting mass for the case with n = 1.4.
Paper: Probing the Mass Relation between Supermassive Black Holes and Dark Matter Halos at High Redshifts by Gravitational Wave Experiments
Authors: Kazuya Furusawa, Hiroyuki Tashiro, Shuichiro Yokoyama, Kiyotomo Ichiki
Figure caption: Dynamical friction timescale t df as a function of redshift z, which is given by Equation (3). The thick solid line (blue) shows the Hubble time as a function of z, and the thin solid line (black) corresponds to the Hubble time at z = 0. We plot the timescale for different mass ratios of two merging halos, P = 0.2, 0.3, 0.4, and 0.6, from top to bottom.
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption:  MESA simulations of the past and future luminosity of the Sun assuming no central BH (left), a central BH of initial mass 10−11 M ⊙ (center), and one of 10−10 M ⊙ (right). The solar age and luminosity are indicated as well as the mass of the BH. Unlike the first two models, the model on the right is obviously not compatible with the present Sun. In both of the right panels, it takes ∼1 Gyr for the BH to transition from supplying 1% to supplying 100% of the solar flux. When the BH approaches the point of supplying 20% of the solar luminosity, nuclear reactions begin to wane and eventually cease. The Sun then dims to half its current luminosity over the span of 100 Myr. Over the course of the next 300 Myr, the BH grows to a mass of 5 × 10−5 M ⊙, at which point it produces the full solar luminosity. Soon thereafter, the Sun expands into a red giant, and does so at a much greater pace than in the normal case: instead of taking 6 Gyr for the Sun to double in luminosity, it is achieved with the aid of the BH in ∼300 Myr. Finally, the accretion luminosity drives the Sun to slowly expand over the course of several gigayears until it produces a maximum of more than 10 L ⊙ before the simulation terminates. The BH in the bottom of the middle panel having a mass of 10−6 M ⊙ is depicted with its actual Schwarzschild radius (∼3 mm); more massive BHs are too large to show (e.g., ∼30 m at 10−2 M ⊙) on this plot.
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption: Analytic accretion estimates for the lifetimes of MS stars born harboring a PBH. Contours of constant age are given by black lines; for low-mass BHs, the lifetimes of the stars are unchanged (brown shading), but as the BH mass approaches the stellar mass, the ages go to zero (blue shading). The colors indicate the percentage of the normal MS lifetime that the star will live before being swallowed by the BH; brown on the top indicates that the star will survive at least as long as its ordinary MS lifetime, and white indicates that the BH cuts the star’s lifetime short by half. The thick white-dashed line shows the Bondi–Eddington transition, i.e., when the BH is massive enough for its accretion luminosity to reach the Eddington limit. The white lines in the middle show a comparison between the luminosity from accretion and the luminosity from fusion, showing for example that a 1 M ⊙ star could attain 1 L ⊙ from slowly falling into a BH of 10−4 M ⊙. The white-dashed lines on the right show when the BH is 1%, 10%, and 50% of the stellar mass, showing for example that a 1 M ⊙ star born about a BH of 0.1 M ⊙ could live for ≳300 Myr.
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption: Kippenhahn diagrams showing the evolution of the interior of the Sun with and without a central BH. The left panels show the mass distribution, with regions of energy generation and transport indicated. The right panels show the radial distribution, with the radius of the photosphere (black line) and the solar radius (horizontal dashed line) indicated. The top panels correspond to a normal solar evolution model evolved through the MS until core hydrogen exhaustion and up through hydrogen shell burning as a red giant. The bottom panels show a model that is consistent with the present Sun with a BH growing at its center. Nuclear fusion (red) provides the bulk of the solar luminosity until the BH is of sufficient mass to quench the reactions. The BH drives convection (hatches), which mixes the innermost parts of the core, and eventually the entire star. Note the differences in the y-axis scale between the panels.