adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Left panel (fiducial): critical semimajor axes for disruption (acrit, cyan line) compared to those for binary-disk decoupling (adecD, orange) and binary-stellar migration decoupling (adecM, purple), for fiducial values and the E. Sirko & J. Goodman (2003) disk models. acrit is also drawn for different mass ratios (q = 0.1 dotted cyan, and q = 0.39 dashed cyan), but the variation is within the width of the q = 1 line. Disruption is allowed when the cyan line falls above the purple and orange lines. Right panel (parameter dependence): critical disruption separations drawn for three stellar densities parameterized by the stellar radius. The shaded regions indicate ranges of possible decoupling separations given a range of disk parameters. The solid (dashed) lines show decoupling radii for fiducial disk parameters for the E. Sirko & J. Goodman (2003; N. I. Shakura & R. A. Sunyaev 1973) disk model. Dotted orange and purple lines denote disk models with the same parameters in the extremes of the shaded regions, highlighting the inverse dependence of the two types of decoupling on disk parameters.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Hydrogen column density (left) and dust temperature map (right) of F-NE. The black contours denote the 13CO (J = 2–1) emission integrated velocity from −70 to −62.5 km s−1, which starts from a 5 K km s−1 and with a step of 11.5 K km s−1. The red circles mark the H II regions identified by L. D. Anderson et al. (2014). The white crosses and pink diamonds represent dense dust clumps from the ATLASGAL and Hi-GAL catalogs, respectively.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Infrared and 13CO (J = 2–1) emissions of F-NE. Cyan, magenta, and yellow backgrounds show the 24, 8, and 4.5 μm emission, respectively. The black contours denote the 13CO (J = 2–1) emission integrated velocity from −70 to −62.5 km s−1. The cyan crosses and triangles are Class I and II YSOs, respectively. The red circles mark the H II regions identified by L. D. Anderson et al. (2014).
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Position–velocity plot of the 13CO (J = 2–1) emissions in the two regions labeled with dashed rectangles in Figure 3, where the integration range is the width between two long arrow lines. The colored background represents the brightness temperature of 13CO (J = 2–1). The horizontal dashed lines represent system velocities of subfilaments F-north, F-NE-north, and F-NE-south.
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Schematic of the circumbinary disk (CBD) plus star around a 3:1 mass ratio supermassive black hole binary with components MP and MS at the critical separation acrit (Equation (8)), where the maximum extent of the tidal radius of the binary (red dashed line) is equal to the distance to the edge of the circumbinary cavity. At this separation, the star begins to be tidally stripped once per conjunction of the secondary black hole and star. Each binary component may have its own accretion disk (mini-disk) not shown.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: Velocity plot along the skeletons of filaments F-NE-north and F-NE-south labeled with colored lines in Figure 1. Each cross corresponds to 1 pixel with signal-to-noise ratio greater than 5σ in the 13CO (J = 2–1) emission of the skeleton. The red stars represent dense clumps in the ATLASGAL catalog located within F-NE.
Paper: Evidences of Two Merging Elongated Filaments Associated with AGAL323.444+0.096 and Star Formation
Authors: Yingxiu Ma, Jianjun Zhou, Jarken Esimbek, Dalei Li, Andrej M. Sobolev, Xindi Tang, Willem Baan, Gang Wu, Macleod Gordon, Yuxin He, Ke Wang, Tie Liu, Dongdong Zhou, Kadirya Tursun, Dmitry A. Ladeyschikov, Weiguang Ji, Hailiang Shen
Figure caption: 13CO (J = 2–1) spectra extracted from collision regions corresponding to red circles in Figure 3. The dashed lines denote the system velocity of F-NE-north and F-NE-south, which is −67.38 and −65.25 km s−1, respectively.
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Left panel (fiducial): gravitational-wave properties of the SMBHB when stellar stripping begins. The solid black line represents the sensitivity of LISA while the gray lines are SMBHB inspiral tracks for the labeled binary masses, mass ratio, and redshift. The vertical cyan line is the critical rest-frame frequency where the fiducial star at rcav = 2a (Ncav = 2) will begin to be stripped, for all SMBH masses (corresponding to the cyan lines in Figure 2). The dotted cyan lines show how this moves down and to the left with increasing redshift. The cyan stars show where disruption would begin for the different binary masses at z = 1 (the largest symbol representing the fiducial case). Above the purple-and-orange dashed line, disk- or migrator-decoupling may occur before the disruption begins (Figure 2). Right panel (parameter dependence): the same as the left panel but demonstrating dependence on source redshift, lower stellar density (thin cyan R = 3RMS line), or increased CBD cavity size (dashed rcav = 4a vertical line).
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Result of solving Equation (20) including tidal stripping from both the primary and secondary SMBHs, up to the point of full disruption, for a γ = 5/3 polytropic star and the fiducial system (Table 1). This shows the last 32 encounters (stripping events) representing the final ≈27 days before full disruption, during which time the majority of the star is stripped. The onset of tidal stripping begins at t = 0, ≈21 yr before full disruption at time tc. The SMBHB will merge ≈246 yr after the full disruption. Times are in the source frame. Results are representative of solutions with Ncav = 2 and intermediate binary mass ratios (see Section 3.2).
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Purple-and-yellow colored contours (with highlighted values in black) of log10 of the maximum accretion rate enhancement for a steady-state α-disk and the system parameters labeled in the figure. Thick solid lines show the limits of where disk properties allow for consistent migration of the star to the critical disruption radius. Red lines delineate the space via Condition (5); green is the gap opening condition of A. Crida et al. (2006); orange is for disk decoupling; and purple is for migrator-decoupling (see Section 2). Arrows point in the direction where consistent solutions exist. The upper-right region with factors of hundreds to thousands enhancements in the accretion rate is allowed for the parameters chosen here. The cyan star denotes the fiducial system, for which Figures 5 and 6 show example evolutions.
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Left panel: the average stellar stripping rate (black line) and solution to Equation (30) for the amplitude of the accretion rate onto the binary (orange), computed from the beginning of the disruption process to full stellar disruption (gray dashed line). Right panel: continuation of the left panel after full stellar disruption and the final decay. We use fiducial system parameters (Table 1) corresponding to the event modeled in Figure 5.
Paper: Stellar Stripping and Disruption in Disks around Supermassive Black Hole Binaries: Repeating Nuclear Transients Prior to LISA Events
Authors: Daniel J. D'Orazio, Christopher Tiede, Lorenz Zwick, Kimitake Hayasaki, Lucio Mayer
Figure caption: Show here are the timescale to strip material from the star τ*, the time between stripping events Trep, and the SMBH binary orbital period at the onset of stripping Pcrit vs. cavity size. Each of the plotted quantities is independent of SMBHB mass. The shaded blue range represents the weak binary mass ratio (q ∈ [0.1, 1]) dependence of the time between stripping events.
Paper: Characterizing TESS-identified Quadruple- and Higher-order Eclipsing Binaries. I. Speckle Imaging with DSSI and HRCam
Authors: Steven R. Majewski, James W. Davidson, Robert F. Wilson, Elliott P. Horch, Paul M. McKee, Evan Fagan, Gabriel N. Hartwell, Veselin B. Kostov, Cassiopeia N. Adams, Torrie Sutherland, Andrei Tokovinin, John C. Wilson
Figure caption: The Gaia DR3 RUWE as a function of the separation of Q+EBs. The orange circles represent the eight Q+EBs that are resolved by both speckle imaging and Gaia, while the blue circles represent those systems resolved only by speckle imaging. The stack of crosses shown at a separation of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩05 represents the HQNDs in Table 2, assigned a separation corresponding to the approximate resolution limit for our speckle imaging. For the resolved systems, the size of the symbol represents the relative magnitude difference of the two components. The Gaia-resolved systems show a clear trend where those with smaller separations have smaller brightness contrasts but larger RUWE. The shaded region to the left indicates the area below the approximate diffraction limit of the speckle imaging, which is 50 mas for both telescopes used, accounting for the wavelengths adopted for observations at each site.
Paper: Characterizing TESS-identified Quadruple- and Higher-order Eclipsing Binaries. I. Speckle Imaging with DSSI and HRCam
Authors: Steven R. Majewski, James W. Davidson, Robert F. Wilson, Elliott P. Horch, Paul M. McKee, Evan Fagan, Gabriel N. Hartwell, Veselin B. Kostov, Cassiopeia N. Adams, Torrie Sutherland, Andrei Tokovinin, John C. Wilson
Figure caption: A representative sample of DSSI reconstructed images from the resolved systems in Table 1. Sources are organized left to right from brightest (TIC 344541836; G = 7.88) to dimmest (TIC 375325607; G = 13.14). The panels show the reconstructed image in the 692 nm channel (top, blue-tinted panels) and in the 880 nm channel (bottom, red-tinted panels). For each panel, north is up and east is to the left. The white arrow points to the real secondary source to distinguish it from the ghost image mirrored 180° in position angle. The flux scaling is logarithmic to highlight the detected sources. The Δm contrasts between primary and secondary are given in Table 1.
Paper: Characterizing TESS-identified Quadruple- and Higher-order Eclipsing Binaries. I. Speckle Imaging with DSSI and HRCam
Authors: Steven R. Majewski, James W. Davidson, Robert F. Wilson, Elliott P. Horch, Paul M. McKee, Evan Fagan, Gabriel N. Hartwell, Veselin B. Kostov, Cassiopeia N. Adams, Torrie Sutherland, Andrei Tokovinin, John C. Wilson
Figure caption: The average detection limits for the targets in our sample from DSSI in the 692 nm channel (top) and in the 880 nm channel (bottom). The gray lines show the detection limits from each of the targets with an HQND, and the colored dashed line is the mean of all the detection curves. Targets with speckle-resolved companions are denoted with open circles (sometimes accompanied by right-pointing arrows, the latter to indicate those lying beyond the range of plotted separations).
Paper: Characterizing TESS-identified Quadruple- and Higher-order Eclipsing Binaries. I. Speckle Imaging with DSSI and HRCam
Authors: Steven R. Majewski, James W. Davidson, Robert F. Wilson, Elliott P. Horch, Paul M. McKee, Evan Fagan, Gabriel N. Hartwell, Veselin B. Kostov, Cassiopeia N. Adams, Torrie Sutherland, Andrei Tokovinin, John C. Wilson
Figure caption: Relative parallax error, ϵπ/π, as a function of Q+EB system angular separation. Similar to Figure 3, the vertical stack of crosses at a separation of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩05 represents the HQNDs, assigned a separation corresponding to the approximate resolution limit for our speckle imaging; the shaded region to the left indicates the area below this formal diffraction limit. Q+EBs resolved by both our speckle imaging and Gaia are denoted with a black open circle (albeit sometimes shaded with interior coloring). As in Figure 3, the size of the points corresponds to the relative magnitude difference of the two components as determined from our speckle imaging. Points with a purplish hue correspond to objects with Gaia RUWE ≲ 1.4, which is where Gaia is able to well fit a single-star astrometric solution to describe its observations, and it is often adopted as a delimiter above which sources are often suspected of multiplicity (C. Fabricius et al. 2021). The dotted and dotted–dashed lines at separations of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4 and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩7 correspond to the approximate angular resolution achieved by Gaia DR2 and the visual binary completeness limit of Gaia DR3, respectively (Gaia Collaboration et al. 2018; C. Fabricius et al. 2021).
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: Time evolution of bar strength A2(t) for models with different halo spins: λ = 0 (black), λ = 0.10 (green), and λ = −0.10 (red). From top to bottom, panels are ordered by decreasing fdisk, and from left to right, by increasing Toomre Q. For models exhibiting effective bar formation (﹩\max \{{A}_{2}(t)\}\geqslant 0.15﹩), dashed lines indicate exponential fits to the initial growth phase of A2(t) in the corresponding color.
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: Left panel: variation in bar formation timescale Δτbar as a function of fdisk, where Δτbar is defined as the difference between the prograde (or retrograde) spin models and their zero-spin counterparts. Upward filled triangles denote prograde models; downward unfilled triangles denote retrograde models. Only models with well-defined Δτbar values are included. Point colors indicate the Toomre Q of each model. Small horizontal offsets are applied to reduce overlap among points with the same fdisk. Right panel: zoom-in view of the left panel, limited to ∣Δτbar∣ ≤ 1 Gyr.
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: The “Fujii diagram”: distribution of τbar versus fdisk for models with effective bar formation. Data point colors indicate Toomre Q values. Marker shapes denote halo spin: circles for λ = 0, upward filled triangles for λ = 0.10, and downward unfilled triangles for λ = −0.10. For comparison, we show the Fujii relation from the high halo mass models of J. Bland-Hawthorn et al. (2023) in a black dotted–dashed line (Equation (5)) and the empirical relation from B.-H. Chen & J. Shen (2025) in colored solid lines (Equation (6)). Overall, models with different spin values follow the general empirical trends, with halo spin introducing additional variations in τbar.
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: Left panel: time evolution of A2 (solid lines) for model fd0.60Q1.6 and its prograde and retrograde halo spin counterparts, with colors indicating halo spin. The corresponding variations of the vertical angular momentum ΔLz of the disk (dotted–dashed lines) and DM halo (dashed lines) are also shown. Right panel: zoom-in on the early evolution; for better visualization, we restrict the range of A2 to [0, 0.25] and ΔLz to [−100, 0]. Dotted lines show ΔLz for the inner disk (R < 10 kpc, ∣z∣ < 2.5 kpc).
Paper: Characterizing TESS-identified Quadruple- and Higher-order Eclipsing Binaries. I. Speckle Imaging with DSSI and HRCam
Authors: Steven R. Majewski, James W. Davidson, Robert F. Wilson, Elliott P. Horch, Paul M. McKee, Evan Fagan, Gabriel N. Hartwell, Veselin B. Kostov, Cassiopeia N. Adams, Torrie Sutherland, Andrei Tokovinin, John C. Wilson
Figure caption: Light curves of TIC 470710327 taken on the nights of 2023 October 19 (top) and October 20 (bottom) UT from the ARCSAT telescope at APO. Superposed on the light curves are the averaged Δm values from DSSI speckle observations using the ARC 3.5 m telescope, with those made in the 692 nm filter shown in blue and those made in the 880 nm filter shown in red. The averaged Δm values on the 19th (top panel) have seeing × separation greater than 0.6 and are therefore considered upper limits. The error bars shown on all Δm points are the standard deviations from Table 7.
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: First row: time evolution of A2(t) for three models with λ = 0 (black), λ = 0.10 (green), and λ = −0.10 (red). Solid lines show the baseline models from Figure 2; dashed and dotted lines correspond to models with 2 and 10 times the number of particles (Np) in both the DM halo and stellar disk. Second row: exponential fits to the initial growth phase of A2(t) for each case.
Paper: Dependency of the Bar Formation Timescale on the Halo Spin
Authors: Bin-Hui Chen, Sandeep Kumar Kataria, Juntai Shen, Meng Guo
Figure caption: Face-on views of the forming bars near the saturation of their exponential growth for several models with Q = 1.4. From bottom to top, fdisk increases. From left to right are the models with retrograde, zero, and prograde halo spin.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Distributions in parameter space of the light curves listed in Table 1 (Mno). Projections on the W vs. P, W vs. A, W vs. ﹩{\varphi }_{{\rm{\min }}}﹩, W vs. Δ, and W vs. C planes are displayed from left to right. Different colors are used depending on the value of the index i of the spectral type Mi-j as shown in the inserts. The crosses show the mean values ± rms deviations of the coordinates.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Distributions in parameter space of the light curves listed in Tables 1 (Mno), 3 (W < 0.3), 4 (W > 0.3), and 5 (C rich). Black crosses show the light curves of Table 1 as averaged in Table 2. Colored crosses show the mean ± rms deviation of the coordinates for the samples of Tables 3–5. Projections on the W vs. P, W vs. A, W vs. ﹩{\varphi }_{{\rm{\min }}}﹩, W vs. Δ, and W vs. C planes are displayed from left to right. Different colors are used to distinguish between the different samples as shown in the insert.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Dependence of the light-curve parameters W and A on the effective temperature T(K) and mass-loss rate ﹩\dot{M}﹩ (10−8 M⊙ yr−1) quoted by J. Bergeat & L. Chevallier (2005) for 15 carbon-rich stars of the Table 5 (C-rich) sample. Open circles show four stars close to the Table 4 (W > 0.3) sample, V CrB, U Cyg, RZ Peg, and R Ori, which are excluded from the linear fits displayed as red lines.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Distributions in parameter space of the light curves listed in Table 3 (W < 0.3). Projections on the W vs. P, W vs. A, W vs. ﹩{\varphi }_{{\rm{\min }}}﹩, W vs. Δ, and W vs. C planes are displayed from left to right. Different colors are used to distinguish between M (red) and S (blue) spectral types.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: The left and central panels display extreme cases of broad (RS Cyg, W = 0.66) and narrow (X Cep, W = 0.16) profiles, respectively. The right panel illustrates schematically the definition of parameters WR and W1/5, of which W is the geometric mean.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Distribution of the humpy curves in the parameter space. Different colors are used to distinguish between the Table 3 (W < 0.3), 4 (W > 0.3), and 5 (C-rich) samples, and different symbols to distinguish between hump types b, c, and d as shown in the inserts.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: From left to right: projections of the parameter space distributions of the Tables 3 (blue) and 5 (green) samples on the P vs. A, P vs. ﹩{\varphi }_{{\rm{\min }}}﹩, P vs. C, and P vs. Δ planes. Ellipses are centered on the mean coordinates and have half axes equal to their rms deviations.
Paper: From the Light Curves of Long Period Variables to Their Evolution along the Asymptotic Giant Branch
Authors: Pham Tuyet Nhung, Mai Nhat Tan, Do Thi Hoai, Pierre Darriulat
Figure caption: Dependence of ﹩{\varphi }_{{\rm{\min }}}﹩ (upper row) and Δ (lower row) on C for the samples of Tables 1 (Mno), 3 (W < 0.3), 4 (W > 0.3), and 5 (C rich), respectively, from left to right. Linear fits are shown for the Tables 1, 3, and 5 samples.