adsabs/AstroCLIMB huggingface dataset:
Paper: Complex Structure around a Circumstellar Disk Caused by Interchange Instability
Authors: Masahiro N. Machida, Shantanu Basu
Figure caption: (a) Disk radius (red; left axis) and mass (blue; right axis) as a function of time after protostar formation. (b) Outflow mass (red; left axis) and outflow momentum (blue; right axis) as a function of time after protostar formation. (c) Azimuthally averaged vertical magnetic field component, Bz, as a function of distance from the protostar at four different epochs. (d) Azimuthally averaged local mass-to-flux ratio, Σ/Bz, normalized by its critical value, ﹩{(2\pi {G}^{1/2})}^{-1}﹩, as a function of distance from the protostar at four different epochs.
Paper: Complex Structure around a Circumstellar Disk Caused by Interchange Instability
Authors: Masahiro N. Machida, Shantanu Basu
Figure caption: (Left panels) Plasma beta, βp, on the equatorial plane. The color bar in panel (a) is different from those in panels (d), (g), and (j). (Middle panels) The ratio of surface density to the z-component of magnetic field strength normalized by the critical value, ﹩{({\rm{\Sigma }}/{B}_{z})}_{{\rm{cri}}}﹩, on the equatorial plane. The contours of ﹩{({\rm{\Sigma }}/{B}_{z})}_{{\rm{cri}}}=1﹩ (white) and 2 (red) are plotted in each panel. The color bar in panel (b) is different from those in panels (e), (h), and (k). (Right panels) Density (n(x) and n(y); right axis) and the ratio of surface density to the magnetic field strength (﹩{({\rm{\Sigma }}/{B}_{z})}_{{\rm{cri}}}(x)﹩ and ﹩{({\rm{\Sigma }}/{B}_{z})}_{{\rm{cri}}}(y)﹩; left axis) along the x- and y-axes on the equatorial plane. The physical quantities are plotted at four different epochs.
Paper: Complex Structure around a Circumstellar Disk Caused by Interchange Instability
Authors: Masahiro N. Machida, Shantanu Basu
Figure caption: Mass inflow and outflow rates (left axis) for box scales of 2200 au (l = 7, top) and 1100 au (l = 8, bottom) are plotted against the elapsed time after protostar formation. The total outflow rate is composed of contributions from the disk wind (or protostellar outflow) and interchange instability. The ratio of inflow to outflow (right axis) is also plotted against the elapsed time after protostar formation.
Paper: Complex Structure around a Circumstellar Disk Caused by Interchange Instability
Authors: Masahiro N. Machida, Shantanu Basu
Figure caption: Density and velocity distribution around the circumstellar disk on the equatorial plane. The time t after the calculation begins and the time tps after protostar formation are indicated at the top of the panel. For reference, a scale bar of 50 au is included.
Paper: The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot
Authors: Haitang Li, Jinhan Guo, Xin Cheng, Chang Zhou, Xiaoli Yan, Jun Chen, Yang Guo, Jacob Oloketuyi, Mingde Ding, Yu Liu
Figure caption: Evolution of the magnetogram. (a) The LOS magnetogram observed by SDO/HMI. The black box shows the field of view in panel (c). (b) Distance–time diagram of the HMI LOS images along the slit AB in panel (a). (c) The normal component (Bz) of the vector magnetogram superimposed over the velocity fields. The black (white) arrows represent the velocity of the positive (negative) polarities. The pink contour represents the PILs. The yellow and red solid lines represent the linear fitting PILs and BP in the yellow box region. (d) Temporal evolution of the negative magnetic flux in the black box region in panel (a) and the BP numbers.
Paper: The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot
Authors: Haitang Li, Jinhan Guo, Xin Cheng, Chang Zhou, Xiaoli Yan, Jun Chen, Yang Guo, Jacob Oloketuyi, Mingde Ding, Yu Liu
Figure caption: A 3D magnetic configuration in simulation. (a)–(b) Collection of magnetic field lines showing the SMA and MFR before and after the filament formation, as seen from the top view. MFR1, MFR2, and SMA represent the magnetic configurations of the filament F1, F2, and AF system observed by NVST in Figures 2(a)–(c), respectively. (c) Side view of panel (b) with selected magnetic field lines. The group of blue, yellow, and green lines delineate the sheared arcades. The red and purple lines delineate the twisted MFR. The gray dashed lines labeled S1, S2, and S3 indicate the positions where planes are taken perpendicular to the MFR axis. (d)–(f) Distribution of current values J on the planes S1, S2, and S3. The black solid lines indicate the concentrated J at BP and X-shaped structures.
Paper: The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot
Authors: Haitang Li, Jinhan Guo, Xin Cheng, Chang Zhou, Xiaoli Yan, Jun Chen, Yang Guo, Jacob Oloketuyi, Mingde Ding, Yu Liu
Figure caption: Distance–time diagram. (a), (c) The AIA 171 and 304 Å image showing the slice AB (as bounded by the white dashed line) and the integrated region (the black box). (b), (d) The distance–time diagrams and the temporal evolutions of the integrated EUV fluxes in 171 and 304 Å (the black lines), respectively.
Paper: The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot
Authors: Haitang Li, Jinhan Guo, Xin Cheng, Chang Zhou, Xiaoli Yan, Jun Chen, Yang Guo, Jacob Oloketuyi, Mingde Ding, Yu Liu
Figure caption: Temporal evolution of different parameters. (a)–(b) Velocity in positive and negative magnetic polarities where the absolute magnetic field intensity is larger than 50 G (∣B∣ > 50 G). (c)–(d) Mean shear angle and twist number in the whole region in Figure 3(c). The colored lines represent the fitting curves from the IDL poly_fit.pro program.
Paper: Luminosity Distance and Extinction by Submicrometer-sized Grains
Authors: R. Siebenmorgen, Frank Heymann, R. Chini
Figure caption: The distance ratios ﹩{D}_{L}({A}_{V}^{{\rm{Ref}}})/{D}_{{\rm{Gaia}}}﹩ vs. DGaia for our sample of 33 stars using visual extinction ﹩{A}_{V}^{{\rm{Ref}}}﹩ estimates obtained by extrapolation of the reddening curves (L. A. Valencic et al. 2004; E. L. Fitzpatrick & D. Massa 2007; K. D. Gordon et al. 2009). Different symbols and colors are used to visually represent the various spectral types and luminosity classes as labeled. Stars with a deviation in the distance ratio from unity that are below 3σ in MV are shown by small symbols. The shaded area depicts the top and bottom quartiles of the distribution, with the mean indicated by a dashed line.
Paper: Luminosity Distance and Extinction by Submicrometer-sized Grains
Authors: R. Siebenmorgen, Frank Heymann, R. Chini
Figure caption: Corrected distance ratios DL(AV)/DGaia vs. DGaia. The luminosity distance derived with AV using Equations (A2)–(A3) (diamonds in brown) unifies the distance ratio for all but four stars. These four stars still agree within their errors with a ratio of one. For comparison, the luminosity distance determined from AV is derived by a single-parameter model fit to the reddening in the UBVJHK bands, assuming a mass fraction of submicrometer particles of 0.55 g in a total of 1 g of dust (symbols in color, as denoted in Figure 1). The shaded area depicts the top and bottom quartiles of the single-parameter model distribution, with a mean of one (solid line).
Paper: The Occurrence of Powerful Flares Stronger than X10 Class in Solar Cycles
Authors: Baolin Tan, Yin Zhang, Jing Huang, Kaifan Ji
Figure caption: The latitude distribution of sunspot active regions that occurred during valley phases of SCs 23 (black +, from 1995 December 20 to 1996 October 15), 24 (green ◊, from 2008 May 14 to 2009 March 11), and 25 (red △, from 2019 March 14 to 2020 January 8). The 0 point on the x-axis represents the valley point between the two SCs. The area between two red dashed lines represents the LAZ.
Paper: The Occurrence of Powerful Flares Stronger than X10 Class in Solar Cycles
Authors: Baolin Tan, Yin Zhang, Jing Huang, Kaifan Ji
Figure caption: The results of Poisson regression of the number of ES-flares (Nes) in SC vs. the rms deviation of the DSN (Vd, left) and mean DSN (Vm, right) around the cycle valley. The green thick dashed–dotted line is a heuristic fitting function obtained from linear regression, while the red circle is the predicting results for SC 25 in this work.
Paper: The Occurrence of Powerful Flares Stronger than X10 Class in Solar Cycles
Authors: Baolin Tan, Yin Zhang, Jing Huang, Kaifan Ji
Figure caption: The occurring time of ES-flares in SCs vs. the rms deviation of the DSN (Vd, left) and mean DSN (Vm, right) during the cycle valley. The black parts (including +, the fitted thick dashed–dotted lines, and thin dotted lines) show the time of the first ES-flare in SCs tes1, while the red parts show the mean time of all ES-flares in SC, tesm. The red  ∗  is the predicting results for SC 25 in this work.
Paper: The Occurrence of Powerful Flares Stronger than X10 Class in Solar Cycles
Authors: Baolin Tan, Yin Zhang, Jing Huang, Kaifan Ji
Figure caption: The distribution of the very large flares stronger than X10 (S-flare) during SC 21–25. The black dots are the DSNs with a smoothed curve (red). The purple pluses (+) mark the S-flares with the class of X10–X14.3 and the red pluses (+) mark the ES-flares (>X14.3). The vertical black and red dashed–dotted lines mark the valley and peak points of each cycle, respectively. Here, we also highlight the strongest flares for each SC.
Paper: Luminosity Distance and Extinction by Submicrometer-sized Grains
Authors: R. Siebenmorgen, Frank Heymann, R. Chini
Figure caption: The absolute reddening curves E(λ − V) of the sample, shifted by an offset for better visibility. Data points (circles) cover the range 0.09−2.2 μm and are complemented at infinite wavelengths by  −AV (Table 1). The best fit (cyan) with contributions from the amorphous carbon and silicates (brown), and submicrometer-sized grains (gray), are shown, with model parameters listed in Table 2. Notable is the dominance of the submicrometer-sized grains in the infrared and their wavelength-independent contribution to the optical/far-UV, respectively.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Cumulative distribution of X-ray burst energy for SGR 1806-20. The scattered points are the binned cumulative distribution of the energy of SGR 1806-20. The red solid line is a broken power-law fitting of the data. The break point is at 1.48 × 1038 erg, which is shown as the black dashed line. The power-law index changes from 0.57 ± 0.01 to ﹩1.1{8}_{-0.05}^{+0.06}﹩ at the break point.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Schematic diagram of the model. Weak and strong FRBs are assumed to be triggered from fracture regions of different sizes. Weak FRBs can be triggered from the small zone on the magnetar surface (∝L2) and crust depth (Rc). The energy released by weak FRBs scales as L3. Strong FRBs are confined by the magnetar crust depth, and the seed of strong FRBs can only grow from the large zone on the surface (∝L2). The energy of strong FRBs relies purely on the fracture area, scaling as L2. This difference in dimensionality has consequences for the scaling properties from weak to strong FRBs, as shown in Figure 1.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Fitting results of the energy function for the three repeating FRBs using the power-law model with an exponential cutoff. (a) The black scattered points with error bars are the cumulative energy function of repeating FRB 20121102A. The dotted gray line indicates the detection completeness threshold, which is the same as in Figure 1. The blue solid line is the fit of the power-law model with an exponential cutoff. (b) Same as panel (a) but for FRB 20201124A. (c) Same as panel (a) but for FRB 20220912A.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Energy functions for three repeating FRBs and earthquakes.  (a) The red rectangular points are the cumulative distribution of burst energy of FRB 20121102A. The red dotted line at 4.5 × 1036 erg indicates the 90% detection completeness threshold. The broken power-law fit to the cumulative distribution of energy is the solid red curve, with the break point at 1.3 × 1038 erg indicated by the red dashed vertical line. Blue circles are the cumulative distribution of burst energy of FRB 20201124A. The dotted blue line at 2.0 × 1036 erg indicates the 95% completeness assuming the median of the burst bandwidths (H. Xu et al. 2022). The broken power-law fit to the cumulative distribution of energy is the blue solid curve, with the break point at 1.1 × 1038 erg indicated by the blue dashed vertical line. Green crosses are the energy function of FRB 20220912A. The green dotted line at 1.0 × 1036 erg indicates the 90% detection completeness threshold (Y.-K. Zhang et al. 2023). The broken power-law fit to the cumulative distribution of energy is the green solid curve, with the break point at 1.1 × 1038 erg indicated by the green dashed vertical line. (b) The cumulative magnitude distribution of a worldwide catalog of earthquakes that covers the years 1900 to 1989 and is complete for magnitude (m) larger than 7.0 (J. F. Pacheco et al. 1992). The broken power-law fit is the solid red curve, with the break point at 7.6 indicated by the dashed vertical line.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Constraints on the parameters of the broken power-law distribution for FRB 20220912A and earthquakes. (a) The panels on the diagonal show the 1σ histogram for each parameter obtained by marginalizing the other parameters for FRB 20220912A. The off-diagonal panels show two-dimensional projections of the posterior probability distributions for each pair of parameters, with contours to indicate 1σ–3σ confidence levels. The fit parameters are shown in Table 1. (b) Same as panel (a) but for earthquakes.
Paper: A Universal Break in Energy Functions of Three Hyperactive Repeating Fast Radio Bursts
Authors: Q. Wu, F. Y. Wang, Z. Y. Zhao, P. Wang, H. Xu, Y. K. Zhang, D. J. Zhou, J. R. Niu, W. Y. Wang, S. X. Yi, Z. Q. Hua, S. B. Zhang, J. L. Han, W. W. Zhu, K. J. Lee, D. Li, X. F. Wu, Z. G. Dai, B. Zhang
Figure caption: Constraints on the parameters of the broken power-law distribution for FRB 20121102A and FRB 20201124A. (a) The panels on the diagonal show the 1σ histogram for each parameter obtained by marginalizing the other parameters for FRB 20121102A. The off-diagonal panels show two-dimensional projections of the posterior probability distributions for each pair of parameters, with contours to indicate 1σ–3σ confidence levels. The fit parameters are shown in Table 1. (b) Same as panel (a) but for FRB 20201124A.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: From top to bottom: light curve of the third IXPE observation of GX 13+1 obtained in the 2–8 keV combining the three telescopes binned in 200 s and the corresponding hardness ratio as a function of time with the same binning; NICER 20 s binned light curve in the 0.7–12 keV band, normalized to 50 detectors, and the corresponding hardness ratio as a function of time. In the first two panels the light-blue shaded bars mark the Swift-XRT observation periods, and the black horizontal dashed–dotted line reports the threshold applied to select the dip state periods (corresponding to the gray vertical shaded bars) in the spectropolarimetric analysis (count rate <28 counts s−1) with respect to off-dip (count rate ≥28 counts s−1). The vertical black dashed lines reported in these panels show the periods we applied to select the dips in the pcube model-independent analysis. In the fourth panel, the horizontal dashed–dotted black line marks the threshold separating the dip time intervals (hardness ratio >0.44) from the off-dip intervals (hardness ratio ≤0.44) in the NICER data.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: Polarization properties of GX 13+1 as a function of time during the third IXPE observation. The panels from top to bottom show PD, PA, q = Q/I, u = U/I, and the hardness ratio along the observation. The gray points in the top four panels show the 2–8 keV count rate (right axis). Left panels: a constant binning of ∼5.2 hr is adopted. Right panels: the observation is divided into six time bins, two of them corresponding to the dips, and the other four covering intervals before, after, and between the two dips. Errors are at 68% CL.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: MAXI folded light curve and hardness ratio of GX 13+1 using the ephemeris of R. Iaria et al. (2014). The periodic dip defines zero phase. The orbital phase intervals covered in the three IXPE observations (IXPE 1, 2, 3) are marked with vertical orange strips. It is apparent that the spectral hardness increases when the source count rate decreases.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: Best-fit spectral fits from NICER during dip and off-dip states in Observation IDs 77010102 and 77010103.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: Comparison between the polarization in the first two IXPE observations of GX 13+1 (left) and this new one (right) to compare the polarization of the dips and of the source in off-dip states. Contours are at 90% CL.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: HID obtained from IXPE data, using the same energy bands (4–8 keV and 2–4 keV) and the same binning (200 s) as in A. Bobrikova et al. (2024a, 2024b). The colors follow the same time behavior as in Figure 1, and the color bar is on the right.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: Normalized Stokes parameters q = Q/I and u = U/I in different energy bins as obtained by pcube in IXPEOBSSIM. The error bars are at 68% CL. No significant trend of the polarization with energy is observed.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Evolution of CSSs on the stellar mass–metallicity diagram and their classification. Thin trajectories represent individual galaxies that end up in the region of CSSs. The CSSs selected according to our criteria at z = 0 in TNG50 can be classified as BSF-CSSs (blue triangles) or TS-CSSs (red triangles). The black solid line represents the fitted data for ordinary dwarf galaxies in TNG50. The gray arrow in the upper right corner of the main panel indicates the uniform 0.75 dex rescaling we apply to the metallicities of TNG50 galaxies in this figure, to better align them with the observed scaling relation (E. N. Kirby et al. 2013). We calculate the stellar mass of each CSS within the effective radius, re. For comparison, M32 is represented by the blue star. We approximate M32’s mass within re based on the total mass from J. Kormendy & L. C. Ho (2013). The selected M32-like CSSs in TNG50 are indicated by black circles. The distribution of ordinary dwarf galaxies at z = 0 is plotted as the gray shaded region. The adjusted metallicity distributions at z = 0 (solid lines) and at the time of the earliest progenitor according to the merger tree (dashed lines), as well as the metallicity distributions of ordinary dwarfs at z = 0, are shown as histograms in the right panel. In the top panel, we show the ratio of maximum stellar mass to the mass at z = 0 for all CSSs, with the mass-loss fraction shown on the right-hand axis. The blue star in this panel represents the mass ratio between the outer stellar halo of M31 (Mouter halo, M31; e.g., K. M. Gilbert et al. 2012) and the stellar mass of M32 (M*,M32). Other legends are consistent with the main panel.