adsabs/AstroCLIMB huggingface dataset:
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The distribution of the hydrogen number density (﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩) inside 0.064 pc. (b) The distribution of the number of Compton-scattered photons in the case of the edge-on view inside 0.064 pc. (c) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ inside 0.01 pc. (d) The distribution of the number of Compton-scattered photons inside 0.01 pc. Here we assume the hydrogen number density of the disk of ﹩\mathrm{log}d/{\mathrm{cm}}^{-3}=15﹩.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The distribution of the hydrogen number density (﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩) based on the sub-parsec-scale radiation-driven fountain model inside 0.064 pc. (b) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 8 yr. (c) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 16 yr. (d) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 24 yr. Here we assume the hydrogen number density of the disk of ﹩\mathrm{log}d/{\mathrm{cm}}^{-3}=14﹩.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The distribution of the hydrogen number density (﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩) based on the sub-parsec-scale radiation-driven fountain model inside 0.01 pc. (b) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 8 yr. (c) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 16 yr. (d) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ after 24 yr. Here we assume the hydrogen number density of the disk of ﹩\mathrm{log}d/{\mathrm{cm}}^{-3}=14﹩.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: Same as Figure 2, but for the sub-parsec-scale radiation-driven fountain model.
Paper: Rapid Dust Growth during Hydrodynamic Clumping due to Streaming Instability
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka
Figure caption: Duration time of the pre-clumping phase reported in Li & Youdin (2021). They define the pre-clumping phase using (1) the time at which the first sedimentation phase ends (﹩{t}_{\mathrm{sedi}-\mathrm{tr}}﹩) and (2) the time at which the dust density exceeds 2ρ R/3 (﹩{t}_{\mathrm{pre}-\mathrm{cl}}﹩). These values are collected from their Table 2. The difference ﹩{t}_{\mathrm{pre}-\mathrm{cl}}-{t}_{\mathrm{sedi}-\mathrm{tr}}﹩ that we plot is the pre-clumping period. We refer to the simulations that adopt St ≥ 10−2 and show ﹩{t}_{\mathrm{pre}-\mathrm{cl}}\gt {t}_{\mathrm{sedi}-\mathrm{tr}}﹩. The color of the filled circles represents St adopted in their simulations (see Table 1 in Li & Youdin 2021). In this figure, the pre-clumping periods are given by ﹩{t}_{\mathrm{sim}}-{t}_{\mathrm{sedi}-\mathrm{tr}}﹩ for weak/moderate clumping cases (see the text for details, and also see Table 1 in Li & Youdin 2021). Li & Youdin (2021) also conducted simulations with St = 10−3 (their Z4t0.1, Z3t0.1, and Z2t0.1 runs) and showed pre-clumping periods ≳475Ω−1 (see their Tables 1 and 2), which is longer than τ SI,satΩ−1 in our fiducial model.
Paper: Rapid Dust Growth during Hydrodynamic Clumping due to Streaming Instability
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka
Figure caption: Comparison of our collision velocity model Δv 2 and the simulation results of Bai & Stone (2010; c s = 0.99 km s−1). Solid and dashed–dotted lines show the collision velocities measured in the R10Z3 run of Bai & Stone (2010) with 2D and 3D domains, respectively (see their Figure 13). Dashed lines show our model (Equation (10)). We show the collision velocities of each St with different colors.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: SN 2022joj (black star) is an SN Ia showing normal brightness in B and remarkably shallow Si II features with a relatively low expansion velocity at maximum luminosity, compared to a sample of normal SNe Ia (gray dots) from Zheng et al. (2018) and Burrow et al. (2020). Left: the B-band absolute magnitude vs. the expansion velocity of Si II λ6355 at maximum brightness. Right: the pEWs of the two Si II lines Si II λλ5972, 6355 at maximum brightness. The dashed black line corresponds to the theoretical ﹩{M}_{B,\max }﹩–v Si II  relation of 1D double-detonation models for thin helium shells across a spectrum of progenitor masses in Polin et al. (2019). The colored × symbols show 2D double-detonation models from Shen et al. (2021b) with different C/O core masses (M  c ) and helium-shell masses (M  s ), and viewing angles. For each model, multiple symbols are shown to summarize the effect of different viewing angles, from μ = −0.93 to μ = +0.93 (μ defined as the cosine of the polar angle relative to the point where the helium-shell detonation occurs). Parameters of the candidate double-detonation normal SN Ia SN 2018aoz (Ni et al. 2023) are also overplotted as an orange diamond.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: SN 2022joj (black stars) is an overluminous, fast-evolving SN Ia with a unique color evolution. In comparison, we show the photometric properties of SN 2011fe (normal SN Ia; Pereira et al. 2013), SN 2018cnw (91T/99aa-like), and SN 2018cuw (normal SN Ia with a red early color). Left: multiband light curves. The upper (lower) panel shows the evolution in the g-band (r-band) absolute magnitude. Right: g ZTF − r ZTF color evolution. The gray circles denote the color evolution of 14 nearby (z ≤ 0.05) SNe Ia (open circles) from the ZTF sample with prompt observations within 5 days of first light (Bulla et al. 2020). The phases with respect to ﹩{t}_{B,\max }﹩ (MJD 59,722.77) are measured in the rest frame of the host galaxy. Correction for Galactic extinction has been applied, but K-corrections have not been performed. The epochs of optical spectroscopy are marked with “S” on the top axis.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Optical spectral sequence of SN 2022joj showing the red to blue color transition as the SN rises to its maximum luminosity and the development of prominent absorption features around 4200 Å post-maximum. The rest-frame phase relative to the B-band peak and the instrument used to observe the SN are listed for each spectrum. Spectra have been corrected for E(B − V)MW = 0.032 mag. All spectra are binned with a bin size of 10 Å, except for the low-resolution SEDM spectra. The corresponding wavelengths of the Si II λ6355 line (with an expansion velocity of 10,000 km s−1) and the Ca II IRT (with expansion velocities of both 10,000 km s−1 and 25,000 km s−1) are marked by the vertical dashed lines. The strong optical telluric features (Fraunhofer A and B bands) are marked by the shaded regions.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Comparisons of an early spectrum (−12 days) and a maximum-light spectrum (+0 days) of SN 2022joj (black) with two sets of double-detonation models. For each synthetic spectrum, the phase relative to ﹩{t}_{B,\max }﹩ is listed (the time since explosion is shown in parentheses). Top: comparison with 1D models from Polin et al. (2019) with different C/O core (M  c ) and He shell (M  s ) masses. Bottom: comparison with 2D models from Shen et al. (2021b) with different masses and viewing angles μ. The observed spectra have been corrected for Galactic extinction.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Nebular-phase spectra of SN 2022joj (black); three overluminous SNe Ia (blue), SN 1991T, SN 1999aa, and SN 2018cnw; and a normal SN Ia (gray), SN 2011fe. The right panel zooms in on the features around 7300 Å. The flux has been normalized to the [Fe III] features around 4700 Å. The orange dashed lines correspond to the wavelengths of four [Fe II] lines (7155, 7172, 7453, and 7638 Å), while the purple dotted lines correspond to the wavelengths of two [Ni II] lines (7378 and 7412 Å), both blueshifted by 1000 km s−1. The spectra were downloaded from WiseREP (Yaron & Gal-Yam 2012), with the following original data sources: SN 1991T and SN 1999aa—Silverman et al. (2012); SN 2011fe—Mazzali et al. (2015); SN 2018cnw—this work.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Optical spectra of SN 2022joj (black) and (i) a subluminous SN Ia, SN 1999by (magenta), (ii) a normal SN Ia, SN 2011fe (gray), (iii) two overluminous SNe Ia, SN 1991T and SN 1999aa (blue), (iv) the peculiar SN 2000cx (green), and (v) a normal SN Ia with a red color at early times, SN 2018aoz (orange), near maximum brightness (left panel) and about a month after maximum (right panel). The dashed–dotted lines correspond to the wavelengths of three Si II lines (4128 Å, 5972 Å, and 6355 Å), while the dotted lines correspond to the wavelengths of the S II “W-trough” (both assuming an expansion velocity of 10,000 km s−1). Ti II has been identified from the spectra of SN 1999by and SN 2000cx at around 4200 Å, and the corresponding features are labeled. The spectra were downloaded from WiseREP (Yaron & Gal-Yam 2012), with the following original data sources: SN 2011fe—Pereira et al. (2013), Mazzali et al. (2014); SN 1991T, SN 1999aa, and SN 2000cx—Silverman et al. (2012); SN 1999by—Matheson et al. (2008); SN 2018aoz—Ni et al. (2023).
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: Comparison of the Sedona synthetic spectra at maximum luminosity indicates that Ti dominates the 4200 Å features in a double-detonation model. Two 1D Sedona models (blue + salmon pink) are run using the density and chemical profile of a slice between the viewing angles μ = −0.467 and μ = −0.333 of the M  c  = 0.96 M ⊙ and M  s  = 0.042 M ⊙ model from Boos et al. (2021). While the synthetic spectrum in the original 2D Sedona model can be well reproduced in a 1D run (blue), the model with all the titanium isotopes removed (salmon pink) cannot reproduce the remarkable 4200 Å features and exhibits a peak at ∼4100 Å.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: The LRIS spectrum reveals an Hα emission line from the host galaxy at 6742.4 Å, corresponding to z = 0.02736. Left: the Hα emission in the observed 2D and 1D spectra. This emission line sits in a region free of strong night-sky lines and is unlikely to be due to bad sky subtraction. Right: image of the host galaxy and the position of SN 2022joj, with the orientation of the LRIS slit overplotted.
Paper: SN 2022joj: A Peculiar Type Ia Supernova Possibly Driven by an Asymmetric Helium-shell Double Detonation
Authors: Chang Liu, 畅 刘, Adam A. Miller, Samuel J. Boos, Ken J. Shen, Dean M. Townsley, Steve Schulze, Luke Harvey, Kate Maguire, Joel Johansson, Thomas G. Brink, Umut Burgaz, Georgios Dimitriadis, Alexei V. Filippenko, Saarah Hall, K-Ryan Hinds, Andrew Hoffman, Viraj Karambelkar, Charles D. Kilpatrick, Daniel Perley, Neil Pichay, Huei Sears, Jesper Sollerman, Robert Stein, Jacco H. Terwel, WeiKang Zheng, Matthew J. Graham, Mansi M. Kasliwal, Leander Lacroix, Josiah Purdum, Benjamin Rusholme, Avery Wold
Figure caption: The color–color diagrams using UVOT photometry show that SN 2022joj (black star) has very unusual UV−optical colors at maximum luminosity compared to normal SNe Ia (gray dots; a sample of 29 normal SNe Ia from Brown et al. 2018). The arrows mark how SN 2022joj would move in each color–color space if there were host reddening with a visual extinction of A  V,host = 1 (assuming R  V  = 3.1).
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: Outcomes of MT, as a function of accretion efficiency and specific AM. The ordinate shows the fraction of interacting systems which undergo stable MT f SMT. The remainder (1 – f SMT) experience unstable MT, possibly resulting in a merger. The abscissa indicates different values of the specific AM parameter f  γ , with f  γ  = 0 corresponding to isotropic reemission and f  γ  = 1 corresponding to mass loss from the L2 point. Different curves represent different values of the MT efficiency parameter β = {1.0, 0.5, 0.0}, corresponding to the red dashed, blue dotted, and green dotted–dashed lines, respectively. The solid black lines show the inconstant COMPAS default β Comp (see text for further details). Panel (a) shows f SMT for the first interaction in a given binary. Panel (b) shows this fraction at the End state (see Section 2.2). Here, f SMT corresponds to the fraction of interacting binaries that have experienced only stable MT throughout all prior interactions. The donor’s response to mass loss is ζ * = ζ Comp for all curves. As expected, f SMT decreases with increasing f  γ  (if β ≠ 1) at both epochs. Notably, there is a subset of binaries which are only stable if the MT is nonconservative, and if f  γ  ≲ 0.2 (as can be seen in Figure 1, an increase in β and a decrease in f  γ  both increase the likelihood of stability for a given system).
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: The Roche-lobe response to MT ζ  L  for different values of the mass ratio q = M  a /M  d , efficiency β, and specific AM of nonaccreted material. Here, the specific AM is parameterized by a  γ , the distance from the binary center of mass at which the nonaccreted material decouples from the system, in units of the semimajor axis a. The light and dark green horizontal lines mark the positions of the donor and accretor, respectively, with the donor always positioned toward the bottom. The upper and lower bounds correspond to the positions of the L2 and L3 Lagrangian points, respectively, which slowly vary in absolute value between ∼[1.2, 1.275]a for this range in q. The pink horizontal line represents the L1 point, and a  γ /a = 0.0 demarcates the binary center of mass. The range considered for AM loss in our proxy parameter f  γ , thus represents the space between the dark green M  A  line and the top of the axis.
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: The donor response to mass loss ζ ad as a function of donor radius, for selected ZAMS masses. The solid, black lines are the COMPAS default ζ Comp (see text for details). The blue lines show ζ Ge20 (dotted, blue) and ﹩{\tilde{\zeta }}_{\mathrm{Ge}20}﹩ (dotted–dashed, blue), from Ge et al. (2020), corresponding to their models for fully adiabatic mass loss, and an artificially isentropic convective envelope, respectively. The dashed, orange lines represent the ζ Claeys14 prescription (Claeys et al. 2014). Values for ζ ad here can be compared to those in Figure 1 for ζ  L  to determine MT stability. However, the ζ values from Claeys et al. (2014) and Ge et al. (2020) are derived from their respective critical mass ratios, which implicitly require that the mass loss is fully conservative, and thus can only be compared to ζ  L  where β = 1. Additionally, since Ge et al. (2020) account for the delayed dynamical instability, ζ Ge20 and ﹩{\tilde{\zeta }}_{\mathrm{Ge}20}﹩ do not represent the initial donor radial response to mass loss, but rather the effective ζ ad that should be compared against ζ  L  to determine stability. The vertical lines represent the radii in our models when the stellar type transitions to the named type, where HG, BGB, CHeB, and EAGB, correspond to Hertzsprung gap, base of the giant branch, core-helium burning, and early asymptotic giant branch types, respectively. In practice, we interpolate both the radii and masses. Note that the y-axis is linear below 1 and logarithmic above, to distinguish the regions of interest better.
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: Distributions of the binary orbital separations before and after the first episode of MT. Panel 1 shows the orbital separations before (pre-MT, upper half) and after (post-MT, lower half) the interaction. The post-MT distributions have been inverted. Only systems which undergo stable MT during this first interaction are included. Panel 2 shows the orbital tightening ratios ﹩{a}_{\mathrm{post}}/{a}_{\mathrm{pre}}﹩ for the same systems. Both use the default stellar response ζ Comp and efficiency β Comp. The colors in both panels correspond to different values of the specific AM loss parameter f  γ , as indicated in the legend, where f  γ  = 0 corresponds to isotropic reemission and f  γ  = 1 is mass loss from the L2 point (see text for discussion).
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: Stable MT fraction, for all model variations. As in Figure 4, we plot the fraction of interacting systems which experienced only stable MT f SMT during the first MT event (solid, red curve), and by the End state (green, dashed curve), see Section 2.2. Model names are listed on the abscissa. The leftmost starred model is the COMPAS default. Models on the left have a fixed donor radial response to mass loss ζ Comp while the accretion parameters β and f  γ  are varied. Those on the right have a varied donor response via the stability condition (assuming fully conservative MT).
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: The initial conditions and outcomes of the first MT event for binaries sampled from the Traditional Sampler and Moe & Di Stefano (2017) distributions. The plots show the sampled values for initial mass ratio and periapsis, with the size of the symbol indicating the initial primary mass. Periapsis is more indicative of future evolution than semimajor axis for the Moe & Di Stefano (2017) sampler (which includes nonzero eccentricities), because we circularize about the periapsis when MT starts (see text). The marker shape indicates the outcome of the first binary interaction. The color represents the stellar type of the primary when it first interacts with its companion. Noninteracting binaries are indicated with a black X. The cluster of short-period, equal mass ratio binaries from the top plot corresponds to overcontact binaries, which are then equilibrated to have equal masses.
Paper: The Impact of Angular Momentum Loss on the Outcomes of Binary Mass Transfer
Authors: Reinhold Willcox, Morgan MacLeod, Ilya Mandel, Ryosuke Hirai
Figure caption: Initial condition distributions from Moe & Di Stefano (2017) for single stars (blue), isolated binaries (green), and binaries which are the inner components of hierarchical systems (orange). Inner binaries make up more than half of all systems and are preferentially found at very tight separations with unequal mass ratios.