adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Progenitor System of the Type Ia Supernova 2021aefx
Authors: Griffin Hosseinzadeh, David J. Sand, Peter Lundqvist, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, 一泽 董, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey A. Kwok, Saurabh W. Jha, Jay Strader, Esha Kundu, Stuart D. Ryder, Joshua Haislip, Vladimir Kouprianov, Daniel E. Reichart
Figure caption: Extinction-corrected color curves of SN 2021aefx compared to SN 2011fe (Zhang et al. 2016) and other SNe Ia with early excesses: SN 2012cg (Marion et al. 2016), iPTF14atg (Cao et al. 2016), SN 2017cbv (Hosseinzadeh et al. 2017), and SN 2019yvq (Burke et al. 2021). For the purposes of the logarithmic time axis, we adopt explosion estimates from the aforementioned authors and use MJD0 = 59529.19 (Section 3.1) for SN 2021aefx. The early color behavior of SN 2021aefx is similar to SN 2017cbv, but the abrupt change in slope (in U − B and other colors) happens earlier (at ∼2 days instead of ∼5 days). In the companion-shocking interpretation, this implies a tighter binary and thus a more compact companion (Kasen 2010).
Paper: Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
Authors: Tsuyoshi Tokuoka, Akio K. Inoue, Takuya Hashimoto, Richard S. Ellis, Nicolas Laporte, Yuma Sugahara, Hiroshi Matsuo, Yoichi Tamura, Yoshinobu Fudamoto, Kana Moriwaki, Guido Roberts-Borsani, Ikkoh Shimizu, Satoshi Yamanaka, Naoki Yoshida, Erik Zackrisson, Wei Zheng
Figure caption: (Top) Observed kinematic ratio, ΔV obs/2σ tot, as a function of the stellar mass. Our measurement of MACS1149-JD1 shown by the five-pointed star is compared with those of two z ∼ 6 galaxies (Smit et al. 2018) shown by the circles and the distribution of measurements of z ∼ 2 star-forming galaxies (Förster Schreiber et al. 2009) shown by the shaded area. The horizontal line at ΔV obs/σ tot = 0.4 is an empirical boundary between the rotation-dominated and dispersion-dominated systems (Förster Schreiber et al. 2009). (Bottom) Kinematic ratio, V rot/σ  V , based on dynamical modeling (Section 4) as a function of redshift. The estimation for MACS1149-JD1 is shown by the five-pointed star. The box plots at z < 4 are taken from Wisnioski et al. (2015) and show the median (middle bar) as well as the central 50th percentile (box) and 90th percentile (vertical lines) of the sample distribution in each survey (see Wisnioski et al. 2015 for the references). The box plot at z ∼ 6 is the result of quasar host galaxies (Neeleman et al. 2021). The circles at z ∼ 4.5 are results of massive rotational galaxies (Lelli et al. 2021; Rizzo et al. 2021). The blue and magenta solid lines show semiempirical models based on Toomre’s disk instability parameter, Q crit = 1.0 (quasistable thin gas disk; Wisnioski et al. 2015) with stellar masses of 1010.5 M ⊙ and 109.4 M ⊙, respectively. The shaded areas around the lines indicate the range of Q crit = 0.67 (thick gas disk) and Q crit = 2.0 (star and gas composite disk) cases (Wisnioski et al. 2015).
Paper: Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
Authors: Tsuyoshi Tokuoka, Akio K. Inoue, Takuya Hashimoto, Richard S. Ellis, Nicolas Laporte, Yuma Sugahara, Hiroshi Matsuo, Yoichi Tamura, Yoshinobu Fudamoto, Kana Moriwaki, Guido Roberts-Borsani, Ikkoh Shimizu, Satoshi Yamanaka, Naoki Yoshida, Erik Zackrisson, Wei Zheng
Figure caption: Top left: ALMA [O III] 88 μm emission moment-0 map contours on the HST/WFC3 F160W image of MACS1149-JD1 at z = 9.1. The contours show +3σ, 4σ, 5σ, and 6σ with σ = 9.4 mJy km s−1 beam−1. The synthesized beam ellipse is shown in the bottom left corner. The circle and inverse-triangle indicate the centers of [O III] emission dynamical disk (Section 4) and ultraviolet (UV) emission, respectively. Top right: [O III] line spectrum integrated over the area where the line was detected at >3σ. The gray shaded region indicates the ±1σ noise level. The solid curve is the best-fit Gaussian profile. Bottom left: [O III] line velocity field overlaid on the line moment-0 contours. The velocity field is depicted only in the area where the Gaussian line profile fitting is favored with confidence >5σ (see Section 3). Bottom right: [O III] line velocity dispersion map overlaid on the line moment-0 contours. The depicted area is the same as the velocity field.
Paper: Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
Authors: Tsuyoshi Tokuoka, Akio K. Inoue, Takuya Hashimoto, Richard S. Ellis, Nicolas Laporte, Yuma Sugahara, Hiroshi Matsuo, Yoichi Tamura, Yoshinobu Fudamoto, Kana Moriwaki, Guido Roberts-Borsani, Ikkoh Shimizu, Satoshi Yamanaka, Naoki Yoshida, Erik Zackrisson, Wei Zheng
Figure caption: Top row: the [O III] 88 μm line moment-0 map; middle row: the [O III] line velocity field; bottom row: the UV continuum image. Left: the observations; middle: the models; right: the residuals. All images are shown in the source plane corrected for the gravitational lensing effect.
Paper: Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
Authors: Tsuyoshi Tokuoka, Akio K. Inoue, Takuya Hashimoto, Richard S. Ellis, Nicolas Laporte, Yuma Sugahara, Hiroshi Matsuo, Yoichi Tamura, Yoshinobu Fudamoto, Kana Moriwaki, Guido Roberts-Borsani, Ikkoh Shimizu, Satoshi Yamanaka, Naoki Yoshida, Erik Zackrisson, Wei Zheng
Figure caption: Image-plane channel map from −150 km s−1 (left) to +200 km s−1 (right) with a 50 km s−1 step. Top: the observed cube; middle: the model cube; bottom: the residual.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Top: polar expansion of δ v ◦, from the face-on deprojection in Figure 5, and with a 1D rotation curve (no meridional flows). The horizontal dashed line corresponds to R  f  = 28  au. The vertical yellow and green lines each indicate the directions of the disk major and minor axis, respectively. Middle: extraction of δ v ◦ at R  f  = 28 au, δ v ◦( x  =  f  PA,i,ψ (R  f , ϕ)). Bottom: intrinsic velocity field  u , assuming that the red side of the flip is entirely due to azimuthal velocity deviations, while the blue side is due to either radial or vertical components, such that u  z  > 0 corresponds to a wind, and u  R  < 0 to stellocentric accretion. The x-axis of all plots corresponds to offset azimuth and is oriented in the direction of disk rotation.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Nonaxial kinematics in the disk of HD 100546. (a) The velocity centroid v ◦ from Figure 2(c). (b) v ◦ after subtraction of the axially symmetric flow, ﹩{v}_{\circ }^{m}﹩, including radial and vertical components (i.e., meridional flows) in the rotation curve. (c) ﹩{v}_{\circ }-{v}_{\circ }^{m}﹩, same as (b) but without meridional flows. The single red and blue contours correspond to ±0.7  km s−1. (d) Continuum from Figure 1(a), with an overlay of the contours for ﹩{v}_{\circ }-{v}_{\circ }^{m}﹩ from (c).
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Moment maps in 12CO(2–1) using double-Gaussian fits in velocity. (a) The two-Gaussian velocity-integrated intensity. (b) The velocity dispersion extracted using the two Gaussians (this image has been median filtered). (c) The velocity centroid of the brighter Gaussian. (d) The amplitude of the brighter Gaussian, ﹩{I}_{1}^{A}﹩. (e), (f) Same as (c) and (d), but for the fainter Gaussian (with amplitude ﹩{I}_{2}^{A}﹩, these images have been median filtered). In (e), the continuum ring is overlaid against ﹩{I}_{2}^{A}﹩ in a single contour at 1/20 peak and is roughly outlined as a region of fainter amplitude.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Rotation curve in HD 100546. The regions in cyan correspond to the total extent of the bright continuum ring. From top to bottom, we show (1) the azimuthal rotation curve ﹩{\tilde{v}}_{\phi }(R)﹩. The dashed horizontal lines are comparison Keplerian profiles with the corresponding stellar mass. The curve labeled “mid” is an extrapolation to the disk midplane assuming vertical Keplerian shear. (2) The vertical velocity component curve ﹩{\tilde{v}}_{z}(R)﹩, where ﹩{\tilde{v}}_{z}\gt 0﹩ points away from the disk midplane. (3) The radial velocity component ﹩{\tilde{v}}_{r}(R)﹩, where ﹩{\tilde{v}}_{r}\gt 0﹩ points away from the star. (4) The opening angle of the cone tracing the unit opacity surface for 12CO(2–1).
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Continuum at 225 GHz. (a): Model image I  m  obtained with uvmem, with an effective beam 0.″018 × 0.″012 at 26° (as estimated with a elliptical Gaussian fit to the central source, which appears unresolved). (b) Restored image, with a Briggs robustness parameter of 0, corresponding to a beam of 0.″024 × 0.″016 at PA 31.1. The noise in the image is 9 μJy beam−1.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Face-on view of the nonaxial kinematics in the disk of HD 100546. Annotations follow from Figure 4.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: (a) Sky view of the Doppler flip in the disk of HD 100546, as in Figure 4(d), but overlaid on a version of the uvmem model image that has been processed with an unsharp mask (as described in Pérez et al. 2020). The gray contours, at 6%, 7%, and 8% maximum, are chosen to highlight structure along the ring. (b) Same as (a), but from a face-on perspective.
Paper: 60 Candidate High-velocity Stars Originating from the Sagittarius Dwarf Spheroidal Galaxy in Gaia EDR3
Authors: Hefan Li, Cuihua Du, Jun Ma, Jianrong Shi, Heidi Jo Newberg, Yunsong Piao
Figure caption: Panel (a): Distribution of the velocity and the half-light radius normalized distance of stars relative to the Sgr when they are at the closest point. Stars with probability P Sgr > 50% originating from the Sgr are shown in blue points. Orange points represent stars with a probability of P Sgr > 84%. The black line shows the density at the spherical shell as a function of the half-light radius normalized distance from the Sgr center. The candidate star probably from Sgr found by Huang et al. (2021) is shown in the red star. Panel (b): Backward time vs. normalized distance between the star and the Sgr during the closest approach. The symbols are the same as in panel (a). The black horizontal dashed line shows the backward time when the Sgr arrives at its pericenter.
Paper: 60 Candidate High-velocity Stars Originating from the Sagittarius Dwarf Spheroidal Galaxy in Gaia EDR3
Authors: Hefan Li, Cuihua Du, Jun Ma, Jianrong Shi, Heidi Jo Newberg, Yunsong Piao
Figure caption: Distribution of total velocity v GC vs. Galactocentric distance r GC for stars with P Sgr > 50%. Black points with error bars represent stars with the probability of correlation with Sgr P Sgr > 0.5. The brown star with error bars is the candidate star that is probably from the Sgr found by Huang et al. (2021). The four different colored dashed lines are the escape velocity curves derived from the different Milky Way potential models (Bovy 2015; McMillan 2017; Eilers et al. 2019; Cautun et al. 2020).
Paper: 60 Candidate High-velocity Stars Originating from the Sagittarius Dwarf Spheroidal Galaxy in Gaia EDR3
Authors: Hefan Li, Cuihua Du, Jun Ma, Jianrong Shi, Heidi Jo Newberg, Yunsong Piao
Figure caption: Color–magnitude diagram of stars with probability originating from the Sgr greater than 50% (black points) compared to the Sgr (red pixels; Vasiliev & Belokurov 2020) and the Sgr stream (blue contour lines; Vasiliev et al. 2021). The color of the pixel is coded by the logarithmic number density relative to the maximum density. The contour lines are equal logarithmic number density lines with an interval of 0.5 dex.
Paper: 60 Candidate High-velocity Stars Originating from the Sagittarius Dwarf Spheroidal Galaxy in Gaia EDR3
Authors: Hefan Li, Cuihua Du, Jun Ma, Jianrong Shi, Heidi Jo Newberg, Yunsong Piao
Figure caption: Histogram of the metallicity distribution of stars with probability originating from Sgr greater than 50%.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Selected channel maps derived from the double-Gaussian fits to the 12CO(2–1) datacube of HD 100546 presented here. The label at the bottom right of each image correspond to v LSR in km s−1. From top to bottom, each row shows the observed maps (obs), then the double-Gaussian model image (mod), then that corresponding to the brighter Gaussian (g 1), and finally to that of the fainter Gaussian (g 2). The two Gaussian components show conspicuous differences, and each roughly corresponds to the front and back disk surfaces.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Example line of sight profiles in the HD100546 12CO(2-1) data for for two selected locations, with offset R.A. (α) and Dec. (δ) in arcsec as indicated. The locations for each line of sights are also plotted on the integrated line intensity map and on the second moment of the double-Gaussian fit.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Selected channel maps obtained with double-Gaussian fits to the 12CO(2–1) datacube of HD 163296, reimaged from archival ALMA data. Annotations follow from Figure 9.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Moment maps in 12CO(2–1) toward HD 163296, obtained with double-Gaussian fits in velocity. Annotations follow from Figure 2.
Paper: The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches
Authors: Simon Casassus, Miguel Cárcamo, Antonio Hales, Philipp Weber, Bill Dent
Figure caption: Channel maps from the 12CO(2–1) datacube. The corresponding line of sight v LSR, in km s−1, is annotated in black in each image. The continuum from Figure 1 is outlined in contours. The beam is 0.″038 × 0.″024/0.0, and the noise is 1.02 mJy beam−1.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: Top panels: the background maps are the running-differential vertical Lorentz force (δ F  z ) maps while the yellow arrows represent the running-differential horizontal Lorentz force (δ F  h ) imposed on S1 and S2 enclosed by the blue contours, which are for −1000 G of B  z . Middle panel: the black/violet curve is the time profile of mean δ F  h  imposed on S1 and S2/mean δ F  z  in the region framed by the dashed rectangle shown in the upper panels, which is the same as that in the upper panels of Figure 5. Bottom panel: the time profile of the mean angle formed between the horizontal local Lorentz force and the horizontal local velocity, which is obtained in the region enclosed by the blue contours in the upper panels. The three dotted lines correspond to the moments of three figures in the upper panels from left to right. The arrows in panels (d) and (e) refer to the time when the moving direction of sunspot S1 was reversed, that is, 18:22 UT, as shown in Figure 2.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: (a) Time profile for the displacement of the target sunspot S1. The displacement was derived from the CoM calculation to the major part of the target sunspot smaller than 30000 DN/pixel in the continuum maps. It should be noted that the curve is two curves joined on the left and right sides of 10:00 UT on August 17 (the junction position is marked by the short dotted line) because, at about that time, the target sunspot separated from the initial one completely. The linear fitting function for different moving speeds is drawn with dashed lines labeled with the corresponding speed value. Longer vertical dotted lines separate the three phases. (b) The emission flux variation in AIA 94, 131, 171, 304, and 1600 Å of the AR.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: Images of AIA 1600, 304, and 171 Å overlaid with the contours of the ±1000 G (blue/lime) vertical magnetic field at 18:00, 18:24, and 19:00 UT on August 17 in the first, second, and third rows, respectively. Top panels: snapshots about 24 minutes before the peak time of the flare. The subfigure in panel (a) shows an enlarged view of the AIA 1600 Å image in the boxed region. The dashed circles labeled with BP1 and BP2 show the two brightening points in the image. The subfigure in panel (b) displays the enlarged view of the AIA 304 Å image in the same boxed region in panel (a) at 08:15 UT and 17:59 UT on August 17, respectively. The arrow in the right subfigure points to the braided structure in the filament. The two dashed circles are the same as the circles in panel (a). The two coronal loop systems are indicated by the annotations “Loops1” and “Loops2” in panel (c). Middle panels: snapshots about 4 minutes before the peak time of the flare. The slits T1 and T2 in panels (e) and (f) are used to investigate the motion of the filament and Loops1, respectively. Bottom panels: snapshots about 36 minutes after the peak time of the flare. Auxiliary lines plotted near the loop apexes on panels (c) and (i) exhibit the contracting motion.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: Top panels: The background maps are the vertical photospheric magnetic field (B  z ) while the arrows represent the horizontal magnetic field (B  h ). The blue/lime contours are for the ±1000 G of B  z . Bottom panel: the mean B  h  variation calculated from the region framed by the black dashed rectangle in the top panels. The three dotted lines correspond to the moments of three figures in the upper panels from left to right. The arrow in panel (d) refers to the time when the moving direction of sunspot S1 was reversed, that is, 18:22 UT, as is shown in Figure 2.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: Time–distance diagrams of slits T1 and T2 shown in Figures 2(e) and (f). The blue dashed line signifies the start time of the flare, and the launching time of the filament eruption and the contraction of Loops1 are delineated by the two green dotted lines, respectively. The white dashed lines represent the linear fitting for the motion of the filament and Loops1.
Paper: Sunspot Shearing and Sudden Retraction Motion Associated with the 2013 August 17 M3.3 Flare 
Authors: Yanjie Zhang, Zhe Xu, Qingmin Zhang, Jun Dai, Haisheng Ji
Figure caption: The trajectories of sunspots S0, S1, S2, S3, S4, and S5 as shown in the upper panels of Figure 1. The color varying from white to dark blue stands linearly for a different time from 17:00 UT on August 16 to the flare starting time. The red curves of each sunspot exhibit their track during the flaring time until 19:30 UT on August 17. The trajectories of sunspots S4 and S5 started at 10:00 UT on August 17. The black segment in the track of sunspot S1 is due to S4 separating completely from S1 at about 10:00 UT on August 17, which is described in detail in the paper.
Paper: Remarkable Correspondence of the Sagittarius A* Submillimeter Variability with a Stellar-wind-fed Accretion Flow Model
Authors: Lena Murchikova, Christopher J. White, Sean M. Ressler
Figure caption: Approximate 230 GHz synchrotron emissivity, j  ν , calculated using Equation (57) of Leung et al. (2011) for the three simulations used in this work. Regions with plasma σ ≡ 2p mag/(ρ c 2) > 1 are assigned zero emissivity. We reorient the angle of viewing such that the flows are similarly aligned; in all cases, the average direction of the angular momentum vector is pointing upward. Left: SANE torus simulation. Middle: MAD torus simulation. Right: β w = 102 MAD winds simulation. Both MAD simulations have more extended emitting regions than the SANE torus simulation. Furthermore, the MAD torus displays more small-scale turbulence in the emitting regions than the MAD winds. The light curves in Figure 3 reflect these differences, with both MAD simulations displaying longer-term variations than the SANE simulation. Additionally, the MAD winds light curve is much smoother than the other light curves because of the comparative lack of small-scale turbulence.
Paper: Remarkable Correspondence of the Sagittarius A* Submillimeter Variability with a Stellar-wind-fed Accretion Flow Model
Authors: Lena Murchikova, Christopher J. White, Sean M. Ressler
Figure caption: Variability structure function of Sgr A* at 230 GHz. Comparison of simulations and observations. The structure function obtained from observed light curves is depicted with empty black circles. Left: simulations of the SANE Sgr A* accretion flow with torus initial conditions as seen from 5° (yellow) and from 45° (red) off the spin axis of the black hole. Middle: simulations of the MAD Sgr A* accretion with torus initial conditions as seen from 5° (purple) and from 45° (gray) off the spin axis of the black hole. Right: MAD stellar-wind-fed Sgr A* accretion simulations with strong magnetization β w = 102 (blue) and weak magnetization β w = 106 (green) of the stellar winds. The simulated structure functions are normalized by coefficients c comb to align with the observed values. The coefficients are as follows: For the SANE torus, c comb = 0.72 (i = 5°) or 0.6 (i = 45°); for the MAD torus, 0.45 or 0.4 for the same inclinations; for the MAD winds, c comb = 0.7 (β w = 102) or 1.15 (β w = 106).