adsabs/AstroCLIMB huggingface dataset:
Paper: The Role of Magnetic Skeleton in Solar Flare Filaments Activity
Authors: Juan Guo, Huaning Wang, Jingxiu Wang, Xiaoshuai Zhu, Jing Huang, Shanqiang Chen, Bingxian Luo, Siqing Liu, Yuanyong Deng, Jiaben Lin
Figure caption: Magnetic skeleton and energy release in the flare filament activity process. Panel (a) and (b): temporal and spatial evolution of the RHESSI HXR emissions with contours at 90% of the maximum for 6–12 KeV, 50–100 KeV, and 100–300 KeV during 02:06–02:29 UT over AIA 131 Å and 171 Å images, respectively (different colors correspond to different time or energy bands marked in panel (a)). The curves in panel (b) are the horizontal moving speeds of the looptop RHESSI HXR sources 3–6 KeV, 6–12 KeV, and 12–25 KeV as time (different colors correspond to different energy bands as that in Figure 2). The evolution of the HXR sources of the three energy bands is similar. Panel (c)–(d): magnetic skeleton over the AIA 131 Å and 171 Å images. The purple lines in panel (d) are the sheared arcades in Figure 3. The eruption of sheared arcades resulted in the local severe M9.3 flare with instantly up to 300 Kev HXR emission in phase 1.
Paper: The Role of Magnetic Skeleton in Solar Flare Filaments Activity
Authors: Juan Guo, Huaning Wang, Jingxiu Wang, Xiaoshuai Zhu, Jing Huang, Shanqiang Chen, Bingxian Luo, Siqing Liu, Yuanyong Deng, Jiaben Lin
Figure caption: Overview of the event. Panel (a): HMI line-of-sight magnetogram at 02:00 UT before the flare, the negative sunspot N3 in the penumbra of the positive sunspot P2, composing the δ structure of the active region. Panel (b): AIA 171 Å image showing the M9.3 flare in the impulsive phase (severe flare in a small local region resulted in blooming and smear when CCD was imaging). The contours in panel (a)–(b) are for ±200 G of B los. Panel (c): flare emission fluxes in AIA EUV, GOES SXR, and RHESSI HXR.
Paper: Efficient Stochastic Template Bank Using Inner Product Inequalities
Authors: Keisi Kacanja, Alexander H. Nitz, Shichao Wu, Marco Cusinato, Rahul Dhurkunde, Ian Harry, Tito Dal Canton, Francesco Pannarale
Figure caption: The evolution of the template bank as proposed, templates are added within bounded τ 0 bins. Once the first τ 0 region is sufficiently filled, the algorithm proceeds to the next region, which is overlapped with the previous bin by 50%. Points are proposed until the whole bank is sufficiently filled. The orange points correspond to the proposed points. The small colored points correspond with the accepted templates. The color bar represents the τ 0 bins explored by the method. Bank generation can be parallelized by generating it across different τ 0 bins.
Paper: Efficient Stochastic Template Bank Using Inner Product Inequalities
Authors: Keisi Kacanja, Alexander H. Nitz, Shichao Wu, Marco Cusinato, Rahul Dhurkunde, Ian Harry, Tito Dal Canton, Francesco Pannarale
Figure caption: Subsolar mass neutron star search template bank with 10 million templates. Mass ranges from 0.1 to 2 for the primary mass and 0.1 to 1 for the secondary mass. The signals are fixed to to 512 s by varying the lower frequency cutoff indicated in the color bar.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The integrated CO(1–0) spectra for the 28 CARMA GOALS galaxies. Each spectrum was created by using the moment0 map (shown in Figure 2) as a clip mask and totaling all flux within the mask in each channel. The areas shaded in fuchsia denote the channels used to calculate the total flux. The rms noise per channel is shown in the upper left-hand corner below the galaxy name. In all cases, the CO(1–0) is detected to be very high signal to noise. The six CARMA objects (UGC 02369, CGCG 468-002, Arp 299, VV 250, CGCG 142-034, and NGC 6670), where two different galaxies were differentiable in our data have had their spectra separated and plotted in the corner of the panel.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The CO(1–0) integrated intensity (moment0) maps from CARMA (white contours) are overlaid on the three-color g r i images from PanSTARRS (K. C. Chambers et al. 2016) for the 28 CARMA GOALS galaxies, ordered based on their R.A. For each map, north is up and east is to the left. The red bar in the lower left-hand corner demarcates 10″ in each field (with the corresponding physical scale listed). The beam is shown in the lower right-hand corner in red. The gray dotted borders represent the size of the CO-only moments from Figures 2 and 3.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: Best-fitting models to the SEDs. The black line shows the best overall model. In some cases, the fit was improved by including a torus component from the AGN (shown in red) in addition to the galactic emission (shown in blue). The fit achieved with just galactic emission in those cases is shown in purple. See Section 3.3 for discussion on the fitting process. PDFs for SFR in the last 10 Myr and, as relevant, fraction of IR luminosity arising from the AGN component are shown as insets. When a galaxy is modeled both with and without an AGN component, both of the resulting SFR PDFs are shown. These generally do not show much difference, indicating that the inclusion of an AGN component does not affect our derived SFR significantly.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The mean velocity (moment1) maps of CO(1–0) of the 28 CARMA GOALS galaxies. The size scales are identical to those used in Figure 2.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The CO(1–0) integrated intensity (moment0) maps of the 28 CARMA GOALS galaxies. The black bar in the lower left-hand corner demarcates 10″ in each field. The beam is shown in the lower right-hand corner in yellow, confirming that all galaxies are well-sampled.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The 100 GHz continuum images of the 16 continuum-detected CARMA GOALS objects. The field of view is equivalent to what was used in Figures 2 and 3. In most cases, the continuum is unresolved by CARMA.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The ratio between the SF predicted by the 100 GHz continuum and SED fitting, showing that for the majority of the these sources, the 100 GHz emission cannot come from a star formation origin.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Evolution of the effective temperature T eff as a function of the age, for both the pure M ZAMS = 6.85 M ⊙ CO-core and hybrid models. The black horizontal dotted line indicates a T eff = 12,000 K.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Comparison of the period spacing ΔΠ i  as a function of the periods of the modes Π i  for the CF88 and HIN models (upper and lower panels, respectively). The green dashed line shows the value of the asymptotic period spacing.
Paper: The Molecular Cloud Life Cycle. II. Formation and Destruction of Molecular Clouds Diagnosed via H2 Fluorescent Emission
Authors: Blakesley Burkhart, Shmuel Bialy, Daniel Seifried, Stefanie Walch, Erika Hamden, Thomas J. Haworth, Keri Hoadley, Shuo Kong, Madisen Johnson, Sarah Jeffreson, Mark R. Krumholz, Min-Young Lee, Amiel Sternberg, Neal J. Turner
Figure caption: Cloud evolution for MC1 (left panel) and MC2 (right panel), comparing ratios of H2 formation to SFR vs. H2 dissociation to SFR. Points are from the numerical simulation, and color indicates time as shown in the color bar inset in the figure. The diagonal black line is the 1–1 line, representing the H2 formation–destruction steady state (J  F  = J  D ).
Paper: The Molecular Cloud Life Cycle. II. Formation and Destruction of Molecular Clouds Diagnosed via H2 Fluorescent Emission
Authors: Blakesley Burkhart, Shmuel Bialy, Daniel Seifried, Stefanie Walch, Erika Hamden, Thomas J. Haworth, Keri Hoadley, Shuo Kong, Madisen Johnson, Sarah Jeffreson, Mark R. Krumholz, Min-Young Lee, Amiel Sternberg, Neal J. Turner
Figure caption: Total mass of H2 formed (green line), total mass of H2 dissociated (black line), total sink mass formed (blue line), and total sinks of molecular gas (purple line) for MC1 (top panel) and MC2 (bottom panel) vs. time.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Obliquity rapidly goes to zero when the nodal precession frequency, g, is greater than the orbital precession constant, α. The horizontal axis shows calculated values of α/∣g∣ for our sample, with the corresponding obliquity, ϵ, in degrees, on the vertical axis, calculated using Equation (5).
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Sample of confirmed exoplanets orbiting M-dwarf host stars. Our sample consists of planets with R  p  = 0.5–16.8R ⊕, with the majority smaller than Neptune and with periods less than 300 days (first panel). The stellar temperatures (second panel) vary between 2560 and 4900 K. The H-band magnitudes (third panel) vary between 14.2 and 3.47. Lastly, we only consider multiplanet systems (fourth panel) with between two and seven planets in the system.
Paper: The Molecular Cloud Life Cycle. II. Formation and Destruction of Molecular Clouds Diagnosed via H2 Fluorescent Emission
Authors: Blakesley Burkhart, Shmuel Bialy, Daniel Seifried, Stefanie Walch, Erika Hamden, Thomas J. Haworth, Keri Hoadley, Shuo Kong, Madisen Johnson, Sarah Jeffreson, Mark R. Krumholz, Min-Young Lee, Amiel Sternberg, Neal J. Turner
Figure caption: The time evolution of the total H2 formation rate in the cloud (green dashed line), H2 dissociation (black line), and SFRs (blue line). SFR and H2 dissociation rates have been smoothed with a spline function. The top row shows results for MC1, and the bottom row shows results for MC2.
Paper: The Molecular Cloud Life Cycle. II. Formation and Destruction of Molecular Clouds Diagnosed via H2 Fluorescent Emission
Authors: Blakesley Burkhart, Shmuel Bialy, Daniel Seifried, Stefanie Walch, Erika Hamden, Thomas J. Haworth, Keri Hoadley, Shuo Kong, Madisen Johnson, Sarah Jeffreson, Mark R. Krumholz, Min-Young Lee, Amiel Sternberg, Neal J. Turner
Figure caption: Ratios of J  F  to J  D  (black line), J  F  to SFR (purple line), and J  D  to SFR (blue line) for MC1 (top panel) and MC2 (bottom panel) vs. time.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: On-sky density distribution of very (and extremely) metal-rich giant stars, with [M/H]XP ≥ +0.3 from Gaia Data Release 3 XP spectra, in three different [M/H]XP bins. The top panel (containing ∼85% of all these stars) shows a flattened, disk-like distribution, concentrated toward the inner Galaxy. This central concentration increases toward higher metallicity (middle panel). The bottom panel, showing the distribution of EMR stars with [M/H]XP ≳ 0.5, shows a striking change in morphology compared to the bin with 0.3 < [M/H]XP < 0.4: the distribution is dominated by a central knot with a sharp cutoff at a projected radius of RGC,proj ∼ 1.5 kpc. The relative prominence of this knot increases by an order of magnitude from the previous bin (see also Figure 2). Note that in all three panels, the imprint of dust extinction is apparent at the lowest latitudes; and the bar may contribute to the slight ±l asymmetry. Foreground stars closer than 4 kpc from the Sun have been removed (see sample selection criteria at the end of Section 2.1).
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: Kinematics of the EMR knot of the Galaxy, here taken as [M/H]XP > 0.45 to slightly enlarge the sample. Top left: mean LOS velocity. Top right: vertical velocity dispersion projected onto the sky. Bottom left: LOS velocity dispersion of stars with radial velocities from Gaia. Bottom right: LOS dispersion from SDSS/APOGEE DR17, which also covers the very center that is too extincted to be “seen” by Gaia. There is modest mean rotation of 35 km s−1 at ∣l∣ ∼ 7° from the Galactic center. The LOS velocity dispersion rises rapidly from ∼75 km s−1 at ∼7° from the Galactic center to nearly 120 km s−1 toward the Galactic center, only seen in the SDSS/APOGEE DR17 data. The knot appears to be a dynamically hot system with little rotation. The steep central rise of the LOS velocity dispersion points toward radial orbits. At least four stars (typically 10) have contributed to the calculation of the mean velocities or dispersions at all pixels shown.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: The longitudinal number density profile of the VMR stars toward the center of the Milky Way. These are the same stars as shown in Figure 1, but integrated over Galactic latitude (excluding ±3° because of the severe dust extinction). The dashed line just illustrates a Gaussian of σ = 10° centered on ∣l∣ = 0 in order to illustrate the level of asymmetry induced by dust extinction. While for the least metal-rich bin (0.3 < [M/H]XP < 0.4) the density peak of the central knot is only ∼3× above the surrounding (in projection) disk-like distribution, this contrast has grown to 100× in the EMR bin ([M/H]XP > 0.5): EMR stars are basically only found in the ≲1 kpc knot.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: Central concentration of different mono-abundance population in the inner Milky Way, shown as the angular distance from the Galactic center, ΘGC which includes the bulk (68%) of the stars, as a function of [M/H]XP. At the Galactic center, 10° corresponds to a projected distance of 1.5 kpc. The dramatic change in appearance seen in Figure 1 is reflected here as a large drop of ΘGC([M/H]XP) that is rather abrupt given the [M/H]XP uncertainties. The initial sample defined at the end of Section 2.1 was used, but only stars within 90° of the Galactic center were considered. Obviously, dust extinction affects this distribution in complex ways, but its effect should be similar for populations of different [M/H]XP.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: Color–magnitude distribution of the EMR giants (with [M/H]XP > +0.45) within 15° of the Galactic center, shown in gray as the (reddening-insensitive) T eff,XP vs. the absolute magnitude in the WISE W1 band, M W1. Overlaid are three sets of Padova isochrones (A. Bressan et al. 2012) for ages of 2–9 Gyr, and for metallicities of +0.3, +0.5, and +0.7. The CMD positions imply that the stars have a considerable range of ages (∼3–10 Gyr). More detailed fitting is precluded by the limited distance (parallax) precision, which lead to M W1 uncertainties of ∼0.2 mag; typical T eff uncertainties are ≲50 K (R. Andrae et al. 2023b).
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: MDF of stars within ∣l∣, ∣b∣ < 10° of the Galactic center (black), compared to those 20° further out in Galactic longitude (lavender). The central MDF shows a distinct peak of VMR stars, reflecting the presence of a tightly confined knot in all metallicity bins of Figure 1. The EMR stars ([M/H]XP ≥ +0.5) are exclusively present at the center. This illustrates that the central knot does not only contain EMR stars (which are confined to it), but also other, and more, VMR stars [M/H]XP > +0.2, with a peak at [M/H]XP = +0.35.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Distribution of the most abundant elements for a hybrid CONe-core model at 105 K, pre- and post-Rayleigh–Taylor rehomogenization (upper and lower panels, respectively).
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Same as Figure 12, but for the CO-core and hybrid WD models of Figure 11 (upper and lower panels, respectively).
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Same as Figure 12, but for the CF88 model computed with different branching ratios, as indicated in the upper left-hand corner of each panel.
Paper: Impact of Current Uncertainties in the 12C+12C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
Authors: Francisco C. De Gerónimo, Marcelo M. Miller Bertolami, Tiara Battich, Xiaodong Tang, Márcio Catelan, Alejandro H. Córsico, Yunjun Li, Xiao Fang, Leandro G. Althaus
Figure caption: Chemical profile of the M ZAMS = 6.85 M ⊙ hybrid and pure CO-core models (upper and lower panels, respectively) at 12,000 K. The shaded region depicts the crystallized portion of the core, which reach crystallization levels of 56.5 and 41.8%, respectively.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Seven BH-HMXBs in a mass-ratio against the orbital-period diagram. Blue symbols mark objects with a high overfilling factor R/R L and low eccentricity e. Gray symbols show wind mass-transferring objects or HMXBs with a near naked helium star donor. Blue open circles, with white dots inside that scattered in the colored area, are the critical mass ratios for the dynamical-timescale mass transfer of massive stars in different evolutionary states. The upper boundary of the blue region is a fit of the critical mass ratio as a function of the orbital period.