adsabs/AstroCLIMB huggingface dataset:
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: Structural snapshots at evolutionary time steps for the 1 M ⊙, solar composition model, as indicated in Figure 1, are shown. As the model steps through time (marked in the upper-right corner) the nuclear-burning shell (black dashed line; nuclear energy generation rate in erg) moves outwards, as the surface convection zone’s (pink shaded region) size is reduced. The thermohaline region (green shaded region) grows from the hydrogen-burning shell until it meets the base of the convective region. The abundance of lithium (green line) and the ratio of carbon to nitrogen (blue line) are also shown, with units rescaled to fit within the plot. In this simulation, the lithium depletion region and the (C/N)-depleted region are connected to the surface convection zone by the thermohaline front at the same time.
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: The evolutionary track for our canonical thermohaline propagation simulation (1 M ⊙, solar metallicity Z = 0.020) is shown, zoomed in on the red giant branch. Surface gravity is indicated at six time steps, denoted dt. These index the evolutionary times at which the subsequent stellar interior snapshots are taken. The time step indices are revised to begin at one for the purpose of demonstration only.
Paper: Tucana B: A Potentially Isolated and Quenched Ultra-faint Dwarf Galaxy at D ≈ 1.4 Mpc 
Authors: David J. Sand, Burçin Mutlu-Pakdil, Michael G. Jones, Ananthan Karunakaran, Feige Wang, Jinyi Yang, Anirudh Chiti, Paul Bennet, Denija Crnojević, Kristine Spekkens
Figure caption: The CMD of Tucana B from our Magellan IMACS data (see Section 3). In the two left panels, we display the CMD of Tucana B within 1.33 r  h  (16″). Along the left side of the far-left CMD are the typical uncertainties at different r-band magnitudes, as determined by artificial star tests. The dashed line marks the 50% completeness limit. In the center-left panel, we plot 13.5 Gyr, [Fe/H] = −2.5 isochrones (Dotter et al. 2008) at different distances. The blue dotted isochrone is at the distance of the original Tucana dwarf spheroidal (D = 900 kpc), while the orange isochrone is at a distance of 2 Mpc. The two panels on the right show randomly selected equal-area background regions. There is likely significant background galaxy contamination at r 0 ≳ 24.5 mag.(The data used to create this figure are available.)
Paper: Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars
Authors: Shingo Hirano, Masahiro N. Machida
Figure caption: Radial profiles for model B20 at t ps = 0, 1, 2, 3, 10, 30, 100, 300, and 1000 yr after the formation of the first protostar. Panels: (a) magnetic field strength, (b) number of orbital rotations at t ps, N rot = (v rot t ps)/(2π R), (c) radial velocity, and (d) absolute value of the ratio of the radial velocity to the rotational velocity. The line for t ps = 0 yr is not plotted in panel (b) because N rot = 0 for every R at t ps = 0 yr. The dotted line in panel (b) represents the expected N rot at t ps = 105 yr when the first star ends its accretion phase (Figure 1 in Hirano & Bromm 2017) by using the radial profile of rotational velocity at t ps = 1000 yr. The horizontal lines indicate N rot = 1 in panel (b), −v rad = 0 in panel (c), and ∣v rad∣ = ∣v rot∣ in panel (d).
Paper: Tucana B: A Potentially Isolated and Quenched Ultra-faint Dwarf Galaxy at D ≈ 1.4 Mpc 
Authors: David J. Sand, Burçin Mutlu-Pakdil, Michael G. Jones, Ananthan Karunakaran, Feige Wang, Jinyi Yang, Anirudh Chiti, Paul Bennet, Denija Crnojević, Kristine Spekkens
Figure caption: A map of nearby galaxies (from the updated, online version of the Catalog of Neighboring Galaxies; Karachentsev et al. 2004) in supergalactic coordinates, highlighting the isolation of Tucana B. Left: In the supergalactic X–Y plane, looking down on the local plane of galaxies, Tucana B is clearly isolated, with its nearest neighbor being the original Tucana dwarf, at a physical separation of ∼500 kpc. The Large Magellanic Cloud‒sized galaxy IC 5152 is separated by ∼620 kpc (at D ≈ 2 Mpc; Karachentsev et al. 2002). These quoted separations are in 3D space, not just in the supergalactic X–Y plane. Right: We show the supergalactic Y–Z plane, which is defined by the local plane of galaxies, used to roughly define the supergalactic coordinate system.
Paper: Tucana B: A Potentially Isolated and Quenched Ultra-faint Dwarf Galaxy at D ≈ 1.4 Mpc 
Authors: David J. Sand, Burçin Mutlu-Pakdil, Michael G. Jones, Ananthan Karunakaran, Feige Wang, Jinyi Yang, Anirudh Chiti, Paul Bennet, Denija Crnojević, Kristine Spekkens
Figure caption: Tucana B as seen in the DESI Legacy Imaging Surveys sky browser (left) and in the deeper Magellan r-band IMACS data (right), where it is more clearly resolved into stars. North is up and east is to the left. The diffuse object to the east of Tucana B is likely a background dwarf galaxy associated with a galaxy group at z = 0.036 (Díaz-Giménez & Zandivarez 2015), which is centered to the northeast and has several other similar, diffuse objects associated with it.
Paper: Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars
Authors: Shingo Hirano, Masahiro N. Machida
Figure caption: Thermal evolution models of the zero-metallicity star-forming clouds as a function of the gas number density. The black line is the base model theoretically obtained by the chemical reaction calculation (Omukai et al. 2008; Machida & Nakamura 2015). The colored lines, the adopted models in this study, are variants of the black line using the stiff-EOS technique with threshold density n th = 1016 cm−3 (red) and 1019 cm−3 (blue), respectively.
Paper: Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars
Authors: Shingo Hirano, Masahiro N. Machida
Figure caption: Time evolution of the protostar properties for models B00 (gray), B20 (blue), B15 (red), and B10 (yellow). Panels: (a) number of protostars, (b) total mass of protostars M frag,tot and mass of the most massive (primary) protostar ﹩{M}_{\mathrm{frag},\mathrm{prim}}﹩, and (c) ratio of rotational velocity to the Keplerian velocity of the primary protostar.
Paper: Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars
Authors: Shingo Hirano, Masahiro N. Machida
Figure caption: Cross-sectional view on the z = 0 plane around the most massive protostar at t ps = 0, 10, and 1000 yr after the first protostar formation from left to right. Panels: (top) gas number density in model B00, (middle) gas number density in model B20, and (bottom) absolute magnetic field strength in model B20. The box sizes are 20 au in the left and middle panels and 1000 au in right panels, respectively.
Paper: Tucana B: A Potentially Isolated and Quenched Ultra-faint Dwarf Galaxy at D ≈ 1.4 Mpc 
Authors: David J. Sand, Burçin Mutlu-Pakdil, Michael G. Jones, Ananthan Karunakaran, Feige Wang, Jinyi Yang, Anirudh Chiti, Paul Bennet, Denija Crnojević, Kristine Spekkens
Figure caption: Absolute magnitude as a function of half-light radius of Tucana B and other isolated, quenched dwarfs in the outskirts of the Local Group (Cetus: McConnachie & Irwin 2006; Tucana: Saviane et al. 1996; And XVIII: McConnachie et al. 2008; KKR25: Makarov et al. 2012; Eri II: Crnojević et al. 2016a). Also plotted are the dwarf satellites of the Milky Way (McConnachie 2012; Carlin et al. 2017; Muñoz et al. 2018; Mutlu-Pakdil et al. 2018). Tucana B is the faintest and smallest of the isolated, quenched Local Group dwarfs.
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Spectrum analysis results of GRB 220426A with the Band function. Here, the bottom-right panel plots the evolution of α and β in this burst and GRB 090902B (from Table 1 of Abdo et al. 2009).
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Spectral fitting results with CPL-mBB and the power-law spectral model (left panel) and theoretical inverse Compton spectrum of the CPL-mBB photons (right panel).
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Evolution of kT ph, F ph, Γph, r ph, and R 0 in the course of the burst.
Paper: Spectral Analysis of GRB 220426A: Another Case of a Thermally Dominated Burst
Authors: Li-Tao Deng, Da-Bin Lin, Li Zhou, Kai Wang, Xing Yang, Shu-Jin Hou, Jing Li, Xiang-Gao Wang, Rui-Jing Lu, En-Wei Liang
Figure caption: Same as Figure 3, but with the CPL-mBB spectral model in the fittings.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: Selected 13CO J = 2−1 channel maps. A point source is seen at a projected distance of 1.″4 with a position angle of 161° (east from north). The dashed ellipses show the projected circular orbit of an object with an orbital semimajor axis of 206 au. Near the center of the AS 209 disk, the inner disk appears as a point source because of an annular gap around ≃0.″5 (Law et al. 2021a; see also Figure 3). The synthesized beam is presented in the lower-left corner of each panel. The color map starts at 5σ ≃ 2.3 mJy beam−1.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: Selected 12CO J = 2−1 channel maps. The upper panels show an annular gap. The black dashed ellipses present the projected circular orbit with a radius of 206 au. Lower panels show a large velocity perturbation on the southern side of the disk (highlighted with black circles). A similar perturbation is not present on the northern side of the disk, emphasizing the localized nature of the perturbation. The synthesized beam is presented in the lower-left corner of each panel. The color map starts at 5σ ≃ 3.3 mJy beam−1.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: (a) The CPD temperature required to explain the observed 13CO emission, as a function of the CPD diameter. The upper horizontal axis shows the planet mass corresponding to the CPD diameter assuming that the CPD radius is 1/3 of the Hill radius: ﹩{R}_{\mathrm{CPD}}={(1/3){R}_{\mathrm{Hill}}=(1/3)({M}_{p}/3{M}_{* })}^{1/3}﹩. The dashed horizontal line shows AS 209's circumstellar disk temperature at 206 au, 22 K (Law et al. 2021b). The gray-shaded region shows the planet mass constrained by the width of the 12CO gap, 0.42–4.2 M Jup, adopting a range of disk viscosities α = 10−4–10−2 (see Section 4.1). (b) A lower limit to the CPD gas mass inferred from the 13CO emission (blue) and an upper limit to the CPD gas mass inferred from the null detection of C18O (red). The dashed curves show M CPD = 1.0, 0.3, 0.1, and 0.03 M  p  (from left to right). (c) The CPD dust mass inferred from the nondetection of the continuum emission. The solid curve assumes a maximum grain size of 1 mm, while the dashed curve assumes a maximum grain size of 1 μm. (d) The CPD dust-to-gas mass ratio obtained from the inferred CPD gas and dust masses. In this figure, the black solid/dashed curves show lower (temperature in panel (a)) or upper (dust mass in panel (c)) limits, while the gray hatched regions present the allowed region in the parameter space bounded by limits from the 13CO (blue) and C18O (red) data.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: A summary figure showing the coincidence of the CPD candidate with the 12CO/scattered-light gap and 12CO velocity kink. (a) Radial profiles of the normalized (black) 12CO integrated intensity and (red) the near-infrared scattered light (from Avenhaus et al. 2018; scaled by r 2 to account for the drop in the incident stellar photons). The shaded region shows 1.″4–2.″0, the approximate radial location of the 12CO gap. (b) Radial profile of the normalized 13CO integrated intensity along the azimuthal location of the CPD (see Figure 3). (c) 12CO channel map at 4.8 km s−1. The location of the 12CO gap is shown with the gray dashed ellipses. Black contours show the dust continuum from Andrews et al. (2018). (d) A zoom-in of the blue box in panel (c), showing the velocity kink in 12CO (background color map) within the 12CO gap (black dashed curves). The blue contours show 13CO emission at 10σ and 15σ levels. Note that the CPD candidate is located at the center of the 12CO gap and coincides with the velocity kink in 12CO, highly suggestive of the presence of an embedded planet. The synthesized beams for 12CO and 13CO data are shown in the lower-left and lower-right corners of the panel, respectively.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: (Red) Radial profile of the 13CO integrated intensity along the location of the point source, averaged over ±2° in position angle around the point source. (Black) Azimuthally averaged radial profile of the 13CO integrated intensity excluding the point source. The gray and red shaded regions show the standard deviation of the integrated intensity in each 0.″05 radial bin. The point source is seen well above the azimuthally averaged integrated intensity. The gap at ≃0.″5–0.″6 is consistent with the 13CO gap previously reported by Law et al. (2021a). The size of the major axis of the synthesized beam is shown with the black horizontal bar.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: (Left) C18O J = 2−1 channel map at 4.8 km s−1, which is the velocity that the 13CO point source has the largest intensity. (Right) The combined MAPS + DSHARP continuum image. The color table is saturated toward the disk center and stretched to better show faint emission at large radii. In both panels, the white contours show the 13CO J = 2−1 emission at 4.8 km s−1 at 5σ and 10σ levels. In the lower-left corner of each panel, synthesized beams for the C18O and continuum data are shown with yellow ellipses while the synthesized beam for the 13CO data is shown with white ellipses.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: (Left) Peak intensity as a function of the beam minor axis. (Right) Integrated intensity as a function of the beam minor axis. Note that both peak intensity and integrated intensity stay constant when the beam is ≲120 mas, suggesting that the CPD is spatially unresolved. When the beam is >120 mas, the peak intensity and integrated intensity increase due to the contamination from the circumstellar disk. In both panels, blue points present intensities in the fiducial image cube whereas red points present intensities in the image cube where the half-channel shift is applied.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: Same as Figure 2, but without the JvM correction. Note that the CPD is clearly seen in the JvM-uncorrected image.
Paper: Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk
Authors: Jaehan Bae, Richard Teague, Sean M. Andrews, Myriam Benisty, Stefano Facchini, Maria Galloway-Sprietsma, Ryan A. Loomis, Yuri Aikawa, Felipe Alarcón, Edwin Bergin, Jennifer B. Bergner, Alice S. Booth, Gianni Cataldi, L. Ilsedore Cleeves, Ian Czekala, Viviana V. Guzmán, Jane Huang, John D. Ilee, Nicolas T. Kurtovic, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, François Ménard, Karin I. Öberg, Laura M. Pérez, Chunhua Qi, Kamber R. Schwarz, Anibal Sierra, Catherine Walsh, David J. Wilner, Ke Zhang
Figure caption: Same as Figure 3, but the radial integrated intensity profiles are derived using the JvM-uncorrected image.
Paper: Formation of Low-mass Black Holes and Single Millisecond Pulsars in Globular Clusters
Authors: Kyle Kremer, Claire S. Ye, Fulya Kıroğlu, James C. Lombardi, Scott M. Ransom, Frederic A. Rasio
Figure caption: Time of TDE vs. stellar mass for all main-sequence star+neutron star TDEs occurring in our CMC cluster models. Black circles indicate standard main-sequence stars, and open blue circles indicate stars with masses above the turnoff mass (shown as a solid gray curve), which are likely observationally identified as blue straggler stars. The solid black (blue) curves show the median disrupted mass vs. time for the main-sequence star (blue straggler star) TDEs.
Paper: Formation of Low-mass Black Holes and Single Millisecond Pulsars in Globular Clusters
Authors: Kyle Kremer, Claire S. Ye, Fulya Kıroğlu, James C. Lombardi, Scott M. Ransom, Frederic A. Rasio
Figure caption: Evolution of accretion disks for the first ∼year after tidal disruption. In the left (right) column we show the evolution of a 0.4 M ⊙ (1 M ⊙) disk. Top panels show the accretion rate onto the neutron star, middle panels show the total (cumulative) mass accreted, and bottom panels show the total spin angular momentum accreted. Solid curves indicate where the mass transfer rate is sufficiently high to “smother” the magnetic field (in this case the field—assumed here to be 1011 G—does not play an important role in the accretion flow) while dashed lines indicate the point in evolution where magnetic energy density dominates the accretion flow. Finally, as horizontal dotted lines in the bottom panels, we show neutron star spin angular momentum values for a few representative spin periods.
Paper: Formation of Low-mass Black Holes and Single Millisecond Pulsars in Globular Clusters
Authors: Kyle Kremer, Claire S. Ye, Fulya Kıroğlu, James C. Lombardi, Scott M. Ransom, Frederic A. Rasio
Figure caption: On the left-hand vertical axis (blue points), we show the fraction of isolated MSPs observed vs. core radius over half-light radius for various Milky Way globular clusters. Open stars (circles) denote clusters that have (have not) undergone core collapse. The size of the points is scaled by the total number of MSPs (single or binary) observed in that cluster. On the right-hand vertical axis (black points), we show the total number of neutron star+star TDEs occurring in our various CMC Catalog cluster models (again black stars and circles denote core-collapsed and non-core-collapsed clusters, respectively). We argue the overabundance of isolated MSPs observed in the most centrally concentrated clusters can be explained in part by the increased rate of TDEs in these systems.
Paper: Identification of Inertial Modes in the Solar Convection Zone
Authors: Santiago A. Triana, Gustavo Guerrero, Ankit Barik, Jérémy Rekier
Figure caption: Observed HFR vorticity wave frequencies (relative to the Carrington frame) from mode-coupling analysis (MCA, orange error bars) and from ring-diagram analysis (RDA, deep-pink error bars) compared to numerical inertial-mode frequencies for E  =  2.1 × 10−4 and δ = 0.29 R ⊙ (blue-violet line with stars). We include observed, numerical, and analytical sectoral Rossby-mode frequencies (as observed in a frame rotating at Ω⊙/2π = 453.1 nHz) for reference. Shaded areas represent the possible effect on the eigenfrequencies induced by the solar differential rotation. See main text for further details.