adsabs/AstroCLIMB huggingface dataset:
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Normalized histograms for start latitudes at a depth of 5 Mm below the base of the convection zone (top panel; with uniform, normal, and triangular distributions), compared to emergence latitudes for near-critical (t  d  = 20 days) and supercritical (t  d  = 3 days) initial field strengths. The vertical lines are drawn for evaluating low-latitude emergence.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Emergence latitudes of flux tubes as a function of the initial latitude, field strength, and the total rise time (from the beginning of the initial perturbation). On each panel, the marker styles denote the initial depths, as in Figure 2. The symbol size shows the initial field strength on the left and right panels and the linear growth rate on the middle panel. The blue line shows the radial rise relation.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Similar to Figure 7, for different initial magnetic field strengths corresponding to the indicated linear growth times, for p = 0.20 (top panel) and p = 0.66 (bottom panel).
Paper: DIISC-IV. DIISCovery of Anomalously Low Metallicity H II Regions in NGC 99: Indirect Evidence of Gas Inflows
Authors: Alejandro J. Olvera, Sanchayeeta Borthakur, Mansi Padave, Timothy Heckman, Hansung B. Gim, Brad Koplitz, Christopher Dupuis, Emmanuel Momjian, Rolf A. Jansen
Figure caption: A r-band image of NGC 99 obtained at the Vatican Advanced Technology Telescope with all the included Binospec slits placed on the H II regions labeled by their assigned number. The yellow arrow points in the direction of QSO SDSS J002330.58+154744.9, which is a projected distance of 159 kpc away from the galaxy center.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: The radial displacement of the tube apex from the initial location R 0 (left panels) and relative to the base of the overshoot region (right panels) as a function of time, with different starting depths below the convection zone (colors), for a linear growth rate of 20 days (top panels) and 3 days (bottom panels). The gray horizontal band denotes the overshoot region.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Characteristic growth time t  g  for flux tubes in a star with 8Ω⊙, located at depths d 0 below the base of the CZ. The vertical dotted lines show, with the respective colors, the onset field strengths of the buoyancy instability at each depth, i.e., with infinite linear growth time.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Emergence latitudes (left panel) and tilt angles (right panel) as a function of the initial latitude, at an initial depth of d 0 = 5 Mm below the base of the convection zone and t  g  = 20 days. Note the relatively strong poleward deflection for low initial latitudes.
Paper: Low-latitude Magnetic Flux Emergence on Rapidly Rotating Solar-type Stars
Authors: Emre Işık, Sami K. Solanki, Robert H. Cameron, Alexander I. Shapiro
Figure caption: Contours of angular velocity normalized to the maximum at the equator at r = 1 for solar-like (left panel) and cylindrical (right panel) rotation profiles.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolution of the donor-star mass (M 2), orbital period (P), orbital-period derivative (﹩\dot{P}﹩), and mass-transfer rate (﹩{\dot{M}}_{2}﹩) with the mass-transfer timescale (t − t RLOF) of our simulated six NS X-ray binaries. t and t RLOF are the stellar age and the stellar age when the RLOF occurs. The black and red solid circles with error bars denote those known NS LMXBs with a negative and a positive period derivative, respectively. In the panel of ﹩\dot{P}﹩, the black and red curves correspond to the evolutionary stage with ﹩\dot{P}\lt 0﹩ and ﹩\dot{P}\gt 0﹩, respectively, and we only plot the evolutionary stages with ﹩\dot{P}\lt 0﹩ of three NS LMXBs, which can match the observation of three known sources with negative ﹩\dot{P}﹩ for clarity.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolution of six NS X-ray binaries (top panel) and three BH X-ray binaries (bottom panel) in the mass-transfer rate vs. donor-star mass diagram. The initial parameters of those X-ray binaries are the same as in Figures 1 and 2. The horizontal short dotted–dashed line denotes the Eddington accretion rate of an NS.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolutionary tracks of six NS X-ray binaries in the orbital-period vs. donor-star mass diagram. The black and red solid circles with error bars depict those known NS LMXBs whose orbital-period derivatives are negative and positive, respectively.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Same as in Figure 3, but for the orbital-period derivative vs. orbital-period diagram. For clarity, we only plot the evolutionary tracks whose ﹩\dot{P}﹩ are negative and positive in the top and bottom panels, respectively.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolution of three NS X-ray binaries in P − M 2 (top panel), ﹩-\dot{P}-P﹩ (middle panel), and ﹩{\dot{M}}_{2}-{M}_{2}﹩ (bottom panel) diagrams. The black solid circles with error bars denote the three known NS LMXBs with a negative ﹩\dot{P}﹩. In this figure, we adopt the standard MB model with γ = 4.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolutionary tracks of our simulated three BH X-ray binaries in the orbital-period vs. donor-star mass diagram (top panel) and the orbital-period derivative vs. orbital-period diagram (bottom panel). The solid circles with error bars denote the three known BH LMXBs.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Evolution of NS X-ray binaries (top panel) and BH X-ray binaries (bottom panel) in the T eff − P diagram. The solid squares and solid circles with error bars denote the two NS LMXBs and three BH LMXBs with a known spectral type.
Paper: Orbital-period Changes of Low-mass X-Ray Binaries Driven by Magnetic Braking
Authors: Yun-Ning Fan, Yong Shao, Wen-Cong Chen
Figure caption: Same as Figure 1, but for our simulated three BH LMXBs. The black solid circles with error bars denote the three known BH LMXBs.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: (a) The Galactic distribution of detected IVCs and HVCs in an all-sky H I map. (b) WHAM maps of the known HVC and IVC complexes that are potentially associated with the detected ionized clouds. (a) The Galactic distribution of detected IVCs (diamond) and HVCs (circle) with an all-sky H I velocity map from the 21 cm HI4PI survey (T. Westmeier 2018). Our clouds are potentially part of the known IVC and HVC complexes, Complex C, Complex K, and Complex gp. The three complexes are presented with boxed outlines having a color corresponding to their average LSR velocity. In panel (b) the WHAM maps for Complex C (left), Complex K (center), and Complex gp (right) are shown. The black boxes correspond to the locations of the known complexes. The Hα intensity is integrated for the LSR velocity ranges of each complex, presented at the top of each map. The LSR velocity ranges are from H. van Woerden et al. (2004). We note that the WHAM survey covers a velocity range of roughly [−100, 100] km s−1, thus it only covers a small fraction of the velocity range of Complex C. The range of intensities varies for each map, as indicated by the corresponding color bar. The H I map from the HI4PI survey (HI4PI Collaboration et al. 2016) is presented with blue contours with column densities of N HI = 1019.5, 1019, and 1018 cm−2 for Complex C, Complex K, and Complex gp, respectively. We show the location of our three sight lines that are potentially associated with the complexes (magenta stars).
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: Kinematic modeling of LSR velocity for each sight line and observed LSR velocity of the detected IVCs (diamond) and HVCs (circle). LSR velocity is a function of distance from the Sun (left y-axis), and the maximum distance is given by the distance to the targeted halo stars. We present the predictions of inflow (blue shaded), outflow (red shaded), and stagnant (hatched) models with the parameters given in Table 4. The colors of the data points denote the categorization of inflow (blue), outflow (red), and ambiguous (gray).
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: Column density ratios of N V/C IV vs. Si IV/C IV, comparing the observed and predicted values by various ionization mechanisms, CIE (black), isobaric (olive) and isochoric (brown) cooling, and turbulent mixing layers (plus mark). Nonequilibrium cooling depends on metallicity as the models of 0.1 (dotted), 1 (solid), and 2 Z ⊙ (dashed) show.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: C IV fraction to the total carbon and column density ratios of Si IV and C IV predicted by isobaric (olive) and isochoric (brown) nonequilibrium radiative cooling at 0.1, 1, and 2 Z ⊙ metallicity. The observed column density ratios of Si IV and C IV are within the gray shaded range.
Paper: Metallicity Mapping of the Ionized Diffuse Gas at the Milky Way Disk–Halo Interface
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, J. Xavier Prochaska, Yong Zheng, Mary E. Putman, Drummond B. Fielding, Jay Strader
Figure caption: The estimated N HI and metallicity of the ionized DHI clouds. The color shows H I fraction over the total hydrogen. We note that most clouds are more than 90% ionized, and the existence of metal-poor gas clouds is in the form of ionized clouds.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Examples of fits and special cases. Top left panel: single-Gaussian plus a power-law model for the [Ne V] emission line at 14.32 μm in the IR spectrum of NGC 7314; see Section 3.1. Top right panel: double-Gaussian plus a power-law model for the [Ne V] emission at 14.32 μm in the IR spectrum of NGC 4102. This model included the nearby [Cl II] 14.37 μm line. The reported flux for this source is that of the first Gaussian curve only (blue line); see Section 3.3.1. Bottom left panel: double-Gaussian plus a power-law model for the [Ne V] emission at 24.32 μm in the IR spectrum of NGC 4507. These spectra had a blueshifted velocity peak, which may suggest the presence of outflows. In such cases we also consider the flux of the second Gaussian, thus, the total flux (red line) for this line is the sum of the fluxes of both Gaussians; see Section 3.3.2. Bottom right panel: triple-Gaussian plus a power-law model for the [O IV] emission at 25.89 μm in the IR spectrum of NGC 7469. This spectrum included a blueshifted velocity peak as well as emission at longer wavelengths. In this case, we adopt a similar method as for the blue excess by considering the fluxes of the first and second Gaussian lines as the total flux of the emission line (blue line + orange line). The reported flux determination varies depending on the specific case; see Section 3.3.4.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Comparison of the detection fraction for the MIR lines studied in this work with the NIR [Si VI] and [Si X] lines from J. S. den Brok et al. (2022) as a function of the logs of the line (top panel) and hard X-ray (central panel) luminosities. The MIR lines in this work have significant detections in ≳85% of local AGN, meaning they are almost twice as likely to be detected than their NIR counterparts. The bottom panel shows the detection rate vs. the ionizing potential for the MIR emission lines studied here.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Log of the emission line flux vs. log of the X-ray flux (left panels) and log of emission line luminosity vs. log of X-ray luminosity (central and right panels) for [Ne V] 14.32/24.32 μm, [O IV] 25.89 μm, and [S III] 18.71/33.48 μm. A linear regression fit in the form Y = α · X + β was performed on the data, where Y and X represent the log of line flux/luminosities and the log of X-ray flux/luminosities, respectively; α and β represent the slope and y-intercept of the linear fits, respectively. The linear fit values can be found in Table 2. The confidence intervals are also shown on the plots.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Median ratio between the flux/luminosity of the lines and the 14–150 keV (top four panels) and bolometric (bottom four panels) flux/luminosity for all five emission lines studied here, vs. black hole mass, column density, Eddington ratio, and X-ray luminosity. The filled red squares represent [Ne V] 14.32 μm, the filled green diamonds represent [S III] 18.71 μm, the filled blue circles represent [Ne V] 24.32 μm, the filled orange triangles represent [O IV] 25.89 μm, and the filled purple stars represent [S III] 33.48 μm. The range in N H is very narrow since the bolometric luminosities in K. K. Gupta et al. (2024) were obtained for a sample of unobscured AGN.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: The number of sources as a function of obscuring column density [log(N H)], black hole mass [log(M BH)], intrinsic 14–150 keV X-ray luminosity [log(L 14–150 keV)], and Eddington ratio (log(λ Edd)] for the parent BASS sample (darker shades) and the sample with MIR spectra used in this work (lighter shades).
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: Log of emission line luminosities vs. log of bolometric luminosities (obtained from the spectral energy distribution analysis of K. K. Gupta et al. (2024), represented by ﹩{L}_{{\mathrm{bol}}^{* }}﹩) for the lines studied here. We performed a linear regression fit in the form Y = α · X + β, where Y and X represent the logs of the line and bolometric luminosities, respectively; α and β represent the slope and y-intercept of the linear fits, respectively. The linear fit values can be found in Table 3, with errors. The confidence intervals on the best fit are shown as shaded areas.
Paper: BASS. XLI. The Correlation between Mid-infrared Emission Lines and Active Galactic Nuclei Emission
Authors: M. Bierschenk, C. Ricci, M. J. Temple, S. Satyapal, J. Cann, Y. Xie, Y. Diaz, K. Ichikawa, M. J. Koss, F. E. Bauer, A. Rojas, D. Kakkad, A. Tortosa, F. Ricci, R. Mushotzky, T. Kawamuro, K. K. Gupta, B. Trakhtenbrot, C. S. Chang, R. Riffel, K. Oh, F. Harrison, M. Powell, D. Stern, C. M. Urry
Figure caption: The 14–195 keV X-ray luminosities as a function of redshift for the sample with MIR spectroscopy used in this work (red stars) compared to the complete BAT-selected sample (gray points). The majority of the objects with Spitzer/IRS spectra have z < 0.1, and span nearly the full range of luminosities seen in the wider BASS population.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: Fourier amplitude spectra and the prewhitening process for the light curves of TIC 400562821. The first two panels show three radial independent frequencies (i.e., F, F1, and F2). The bottom panel shows the residual after subtracting 23 significant frequencies. The blue dotted curve refers to the detection limit of S/N = 4.0.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: Diagnostic plots of combination frequencies matching the nonlinear response template (the Template). Symbols with black circles: relative phases and amplitude ratios of TIC 400562821. Symbols without black circles: relative phases and amplitude ratios of the HADS stars of the Template.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: A 2 day section of TESS light curves of TIC 400562821. The amplitude of the light curve is about 0.1 mag. BJD is Barycentric Julian Date.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: The amplitude tracking plots demonstrate the lack of variability in the pulsation amplitudes of TIC 400562821.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Example of the flux variation for an injected fake source with an [O I] line profile based on the instrumental LSF. (A) Result for one cube of the first epoch. (B) Same as (A) but for a cube of the second epoch. For each case the line was modeled so as to have a similar flux to the one of HT Lup B at the respective epoch, to better estimate the impact on a comparable source. For both cases, the post-processed profiles remain almost identical to the preprocessed ones.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Spectra of HT Lup A retrieved for each of the available data cubes. Top, middle, and bottom panels correspond to the first, second, and third data set respectively. The black line in each panel corresponds to the mean spectrum for each data set. In addition to evident Hα emission, HT Lup A does not appear to exhibit any other lines associated with accretion.
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Illustration of the polarization of electron spins by elastic scattering in a Coulomb field produced by an ion. The interaction between the electron magnetic moment  μ   e  and the induced magnetic field  B  eff causes the precession of the electron spin  S  associated with its magnetic moment around  B  eff. The scattered electron is polarized with the spin perpendicular to the scattering plane (﹩\hat{{\boldsymbol{y}}}\hat{{\boldsymbol{z}}}﹩) made by  v  and  r  with the normal vector  n  if the Larmor precession is much faster than the interaction time.
Paper: The Potential for Long-lived Intermediate-mass Black Hole Binaries in the Lowest Density Dwarf Galaxies
Authors: Fazeel Mahmood Khan, Fiza Javed, Kelly Holley-Bockelmann, Lucio Mayer, Peter Berczik, Andrea V. Macciò
Figure caption: Stellar mass density profile of our dwarf galaxy sample as described in Table 1. The vertical dashed lines show the 3D stellar density at the IMBH influence radius for the corresponding model. Our models span roughly 4 orders of magnitude in central density, and the densest model is still several orders of magnitude less dense than nucleated dwarfs.
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Illustration of the CISA effect on an aligned grain with electron spinup (black arrows). When a chiral molecule (i.e., an L- or D-molecule) approaches the grain surface, the charge redistribution process causes the dominance of D-electrons from the L-molecule and L-electrons from the D-molecule at the pole of the molecule (marked by the σ − sign) near the grain surface, due to the CISS effect. The exchange interaction between the grain electron spin (black arrow) and the molecular electron spin (thick black arrow) favors the D-molecules with antiparallel spins (i.e., attractive) and disfavors L-molecules with parallel spins (i.e., repulsive), following the Pauli exclusion principle. Thus, the rate of adsorption for D-molecules to the grain is higher than for L-molecules.