adsabs/AstroCLIMB huggingface dataset:
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Time evolution of orbital elements and integrals of 2010 XC15 and 1998 WT24 during 1000 yr backward integration: (a) semimajor axis, (b) eccentricity, (c) perihelion distance, (d) inclination, (e) longitude of ascending node, (f) argument of perihelion, (g) C 1 integral, and (h) C 2 integral. The time evolution of nominal and averaged values for 2010 XC15 is represented by solid and dashed lines, respectively. The time evolution of nominal and averaged values for 1998 WT24 is represented by dotted and dotted–dashed lines, respectively. The time evolution of clones for 2010 XC15 and 1998 WT24 is shown by gray and black lines, respectively.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Lidov diagram with C 1 and C 2 of NEAs. Larger asteroids (primary) are plotted with larger markers compared to smaller asteroids (secondary) for all pairs. The area to the left of the separatrix (dashed line) is the libration mode (the argument of perihelion librates), and the area to the right is the circulation mode (the argument of perihelion circulates). The forbidden region is hatched. The orbital elements used to calculate C 1 and C 2 were extracted from the Minor Planet Center Orbit Database file as of 2023 May 1.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Energy distribution of FRB 20220912A. (A) The blue step represents the cumulative probability distribution of the energy function, while the red dashed line denotes the best-fit using a broken power-law function. The red region indicates the 1σ range of the fitting. (B) The differential probability distribution of the energy function, with the red line showing the fitting using two lognormal functions. (C) The time-dependent burst energy distribution. The blue dots display the energy of 1076 bursts; red dots denote the median energy; and the blue contours depict a 2D kernel density estimation (KDE) of the bursts. The gray dashed line represents the 90% detection threshold.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Results of polarimetry of polarimetric standard star HD 19820 at each site on each day. The Stokes parameters Q and U normalized by the intensity I, q ≡ Q/I and u ≡ U/I, before and after series of corrections are presented as diamonds and triangles, respectively. The q and u of HD 19820 calculated from P and θ in Schmidt et al. (1992) are shown by hexagons. Bars indicate the 1σ uncertainties. The polarization degrees of HD 19820 after series of corrections and those in Schmidt et al. (1992) are represented by large solid circles and dashed circles, respectively. The deviations ΔP, the polarization degrees in Schmidt et al. (1992) minus those derived here, and Δθ, the position angles of polarization in Schmidt et al. (1992) minus those derived here, are shown.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Semimajor axis (a) vs. minimum eccentricity (e min) of NEAs. Larger (primary) asteroids are plotted with larger markers compared to smaller (secondary) asteroids for all pairs. Orbital elements were extracted from NEODyS-2 as of 2023 May 1.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: The properties of the bursts from FRB 20220912A observed by FAST. (A), (B), (C), (D), and (E) respectively denote the DM, RM, linear polarization, circular polarization, and energy of the bursts. Each burst is depicted by a blue point with error bars, the red points represent the daily median, and the light red area encompasses the 1σ range. (F) displays the number of bursts detected (blue) and the event rate (red), while the yellow bar symbolizes the observation length.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: The waiting-time distribution of FRB 20220912A. The red solid line represents the best-fit model with two lognormal functions, and the red dashed line indicates the best-fit model with a single exponential function.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Example profile from MAVEN inbound orbit #5922 (2017-10-18, SZA ∼29°). (a) MAVEN observations of the radial (B  r , in red) and horizontal (B  h , in blue) components (solid lines), and the crustal magnetic components from the L2019 model (dashed lines). (b) Draped magnetic field calculated by subtracting the crustal components from MAVEN observed magnetic field. The black line denotes the total strength of the draped magnetic field.
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: The [N II] (left), [S II] (middle), and [O I] (right) BPT diagrams for samples at z = 0–6.5. Composite spectra and individually detected CEERS galaxies are displayed as in Figure 3. Composite spectra of star-forming galaxies at z ∼ 1.5 and z ∼ 2.3 from the MOSDEF survey are displayed as “X”s (Shapley et al. 2019). The distribution of z ∼ 0 star-forming galaxies from SDSS is shown in the gray two-dimensional histogram, with the median trend provided in orange. The brown dashed line denotes the median line-ratio sequences derived from the catalog of ∼1000 z = 0 H II regions presented in Sanders et al. (2017; see also Pilyugin & Grebel 2016).
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Similar to Figure 2, but showing six additional example profiles from MAVEN orbits. (a) Inbound orbit #2134 (2015 November 4, SZA ∼50°); (b) inbound orbit #2282 (2015 December 2, SZA ∼72°); (c) inbound orbit #2710 (2016 February 20, SZA ∼90°); (d) inbound orbit #3126 (2016 May 8, SZA ∼58°); (e) inbound orbit #5928 (2017 October 19, SZA ∼28°); and (f) inbound orbit #6057 (2017 November 11, SZA ∼36°).
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: The O32 vs. R23 diagram for samples at z = 0–9.3. Composite spectra and individually detected CEERS galaxies are displayed as in Figure 5. Composite spectra of star-forming galaxies at z ∼ 2.3 and z ∼ 3.3 from the MOSDEF survey are displayed as “X”s (Sanders et al. 2021). The distribution of z ∼ 0 star-forming galaxies from SDSS is shown in the gray two-dimensional histogram, with the median trend provided in orange. The brown dashed line denotes the median sequence of z = 0 H II regions.
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: The [N II] (left column), [S II] (middle column), and [O I] (right column) BPT diagrams at z = 2.0 − 6.5. Each row displays individual galaxies and composite spectra for a single redshift interval. Arrows denote 3σ upper limits when the weakest line was not detected. The gray two-dimensional histogram shows the distribution of z ∼ 0 star-forming galaxies from SDSS, while the orange line provides the median trend of this sample. The black solid line displays the local empirical demarcation between star-forming galaxies and AGN from Kauffmann et al. (2003; [N II] BPT) or Kewley et al. (2006; [S II] and [O I] BPT diagrams).
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: The O32 vs. R23 diagram at z = 2.0–9.3. Both line ratios have been corrected for dust reddening. Each row displays individual galaxies and composite spectra for a single redshift interval. The gray two-dimensional histogram and orange line show z ∼ 0 star-forming galaxies as in previous figures.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Geographic location of draped magnetic field profiles observed by MAVEN. The black dots denote the location of profiles free of crustal magnetic anomalies (crustal field <30 nT below 500 km altitude), among which 141 profiles with SZA <30° are marked in red.
Paper: Variability of Draped Interplanetary Magnetic Field in the Subsolar Martian Ionosphere
Authors: J.-P. Huang, Y.-Q. Hao, H.-Y. Lu, J. Cui
Figure caption: Distribution of draped magnetic field strength at different altitudes for the 141 selected profiles.
Paper: Triplet Pairing in Neutron Matter
Authors: Eckhard Krotscheck, Panagiota Papakonstantinou, Jiawei Wang
Figure caption: The figure shows dependence of the superfluid gap for 1S0 (black solid line), 3P2–3F2 (blue solid line), and 3P0 pairing (red solid line) with the Reid interaction on the Fermi wavenumber k F. Also shown is the 3P0 pairing gap when the spin–orbit interaction is turned off (red dashed–dotted line). Note that the scale on the left-hand side of the figure refers to 1S0 and 3P0 states, whereas the scale on the right refers to the 3P2–3F2 channel.
Paper: Triplet Pairing in Neutron Matter
Authors: Eckhard Krotscheck, Panagiota Papakonstantinou, Jiawei Wang
Figure caption: Examples of the Feynman diagrams included in the effective interaction. Each red wavy line represents a particle-hole irreducible vertex. Each blue wavy line depicts a bare interaction. (a) is a simple example of a “chain” diagram. (b) and (c) are simple examples of “ladder” diagrams, which may just consist of bare interactions (diagram (b)) or the rungs of the ladder may contain chain (diagrams (c)). Diagrams (d) and (e) show simple examples of “twisted-chain” diagrams.
Paper: Triplet Pairing in Neutron Matter
Authors: Eckhard Krotscheck, Panagiota Papakonstantinou, Jiawei Wang
Figure caption: The figure shows the interaction of a pair of neutrons in a spin-triplet state (solid line), the resulting spin-triplet pair distribution function g  T (r) (short-dashed line), and the spin–orbit potential (long-dashed line).
Paper: Reinvestigating the Gamow Factor of Reactions on Light Nuclei
Authors: Eunseok Hwang, Heamin Ko, Kyoungsu Heo, Myung-Ki Cheoun, Dukjae Jang
Figure caption: The ratio of both enhancement factors, ﹩{f}_{\mathrm{mod},s}(\rho ,T,{V}_{0},{V}_{1})/{f}_{g,s}(\rho ,T)﹩, as a function of temperature and density. The red dot marks the solar core condition in Table 2.
Paper: Triplet Pairing in Neutron Matter
Authors: Eckhard Krotscheck, Panagiota Papakonstantinou, Jiawei Wang
Figure caption: The figure shows the superfluid gap for 1S0 (black line), and the 3P0 pairing (red line) for the effective interaction derived by parquet-diagram summation from the Reid interaction.
Paper: The Effects of Nonequilibrium Velocity Distributions on Alfvén Ion-cyclotron Waves in the Solar Wind
Authors: Jada Walters, Kristopher G. Klein, Emily Lichko, Michael L. Stevens, Daniel Verscharen, Benjamin D. G. Chandran
Figure caption: Diffusion operator ﹩\hat{G}f﹩ (Equation (2)) as a function of k ∥ and v ⊥ indicates regions where energy is transferred from the distribution to the fields (red) or vice versa (blue). Color bars in the bottom row apply to the entire column. ﹩\hat{G}f﹩ is dimensionless but proportional to ﹩{({n}_{j}/{n}_{0})/(v/{v}_{{\rm{A}}})}^{4}﹩ where n 0 ≡ ∫d 3 f  j . ﹩\hat{G}﹩ calculations are shown for Interval 2 forward Alfvén mode (left) and backward Alfvén mode (right) for the first bi-Maxwellian model (top), second bi-Maxwellian model (middle), and I-I data (bottom). ﹩{\mathfrak{G}}﹩ is plotted against the right-hand y-axis and given by the cyan line with error bounds as described in the text, with the associated growth (solid green line) or damping (dashed line) rates plotted against the left-hand y-axis. ﹩{\mathfrak{G}}﹩ is dimensionless but proportional to ﹩{({n}_{j}/{n}_{0})/(v/{v}_{{\rm{A}}})}^{7}﹩. Where ﹩{\mathfrak{G}}﹩ is positive, we find a corresponding instability (positive γ). For the forward Alfvén mode, gray contours are 8 logarithmically spaced levels between ∣5e − 5∣ and ∣.01∣ for both positive (solid) and negative (dashed) values. For the backward Alfvén mode, contours are 8 logarithmically spaced levels between –0.25 and –1e-2 and 8 logarithmically spaced levels between 1e-5 and 0.05.
Paper: The Effects of Nonequilibrium Velocity Distributions on Alfvén Ion-cyclotron Waves in the Solar Wind
Authors: Jada Walters, Kristopher G. Klein, Emily Lichko, Michael L. Stevens, Daniel Verscharen, Benjamin D. G. Chandran
Figure caption: Bi-Maxwellian core-and-beam models (left and center columns) and I-I data (right column) for Intervals 1 (top row) and 2 (bottom). Vertical lines correspond to the resonant velocity at which an instability terminates for the I-I data (red lines), first bi-Maxwellian model (blue lines), and second bi-Maxwellian model (green lines). Dashed and solid lines indicate resonant velocities associated with the forward and backward Alfvén modes, respectively. The velocity range is trimmed in this figure to highlight the structure of the VDF, with the actual velocity ranges used in the ALPS calculation spanning v ∥ ∈ [−207, 205] km s−1 and v ⊥ ∈ [0, 378] km s−1 for Interval 1 and v ∥ ∈ [−204, 202] km s−1 and v ⊥ ∈ [0, 356] km s−1 for Interval 2. While the color scale is linear, gray contours show the shape of ﹩{\bar{f}}_{p}﹩ across 10 logarithmically spaced levels between 0.01 and 0.9.
Paper: The Effects of Nonequilibrium Velocity Distributions on Alfvén Ion-cyclotron Waves in the Solar Wind
Authors: Jada Walters, Kristopher G. Klein, Emily Lichko, Michael L. Stevens, Daniel Verscharen, Benjamin D. G. Chandran
Figure caption:  ALPS dispersion solutions for real and imaginary frequencies ω  r  and γ. The forward (left column) and backward (right) Alfvén solutions are presented for Interval 1 (top panels) and 2 (bottom). The ω  r  solutions for the first (blue lines) and second (green lines) bi-Maxwellian models are qualitatively similar to the I-I data (red lines) solution, but the γ behavior differs significantly. For instance, the bi-Maxwellian models are unstable for the backward Alfvén solution for Interval 1 while the I-I data yields a stable solution. The forward Alfvén solution in Interval 2 is unstable in model 2 while model 1 and I-I data are stable. The ALPS scan is performed for k ∥ d  p  between 0.01 and 10, and we choose the limited range presented here to constrain the scan to the region where the resonant velocity is within the limits of the input distribution and γ/ω  r  < 1/e.
Paper: The Effects of Nonequilibrium Velocity Distributions on Alfvén Ion-cyclotron Waves in the Solar Wind
Authors: Jada Walters, Kristopher G. Klein, Emily Lichko, Michael L. Stevens, Daniel Verscharen, Benjamin D. G. Chandran
Figure caption: Perpendicular (top row) and parallel (right) diffusion operators, Equations (3) and (4), for the bi-Maxwellian models 1 and 2 (left and middle columns) and I-I data (right) for the Interval 2 forward Alfvén solution. The color scheme follows that presented in Figure 3. The models have qualitatively similar structures, but exhibit different ﹩{\hat{G}}_{\perp }f﹩ and ﹩{\hat{G}}_{\parallel }f﹩. This can be compared to the complexity seen in the I-I data, where the same broad structures are not observed. For model 1 and the I-I data, gray contours are 8 logarithmically spaced levels between ∣5e − 4∣ and ∣0.03∣ for both positive (solid) and negative (dashed) values. For model 2, gray contours are 8 logarithmically spaced levels between ∣5e − 3∣ and ∣0.3∣ for positive and negative values.
Paper: Properties of Electron-scale Magnetic Reconnection at a Quasi-perpendicular Shock
Authors: Ao Guo, Quanming Lu, San Lu, Shimou Wang, Rongsheng Wang
Figure caption: Distribution of the reconnection electric field at X points from Ω i0 t = 9–13.61. (a) Distribution of the X points in the ﹩\left|{E}_{R}\right|-x^{\prime} ﹩ space. The orange line plots the ﹩\left|{E}_{R}\right|﹩ averaged on the X points located near a given ﹩x^{\prime} ﹩. (b) Count rates of the X points on x-axis in the shock rest frame, which is the total number of X points that appeared at ﹩x^{\prime} ﹩ divided by the number of time steps (n step) when the location ﹩x^{\prime} ﹩ is included in the diagnostic domain (x = 120–140d i0). (c) Distribution of the reconnection electric field ﹩\left|{E}_{R}\right|﹩.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: Left: a comparison between the irradiation luminosity and the X-ray luminosity. Right: a comparison between the irradiation luminosity and the spin-down luminosity. The IDs of BWs are labeled in blue, while RBs are labeled in red. tMSPs (ID: 18, 20) are marked as red stars. The upper limit of irradiation luminosity of PSR J1622–0315 (marked by a red square box) is calculated using the effective temperature. The RBs and BWs occupy two distinct regions in the L irr–L x plot. The dotted lines in the L irr–﹩\dot{E}﹩ plot correspond to different ﹩{L}_{\mathrm{irr}}/\dot{E}﹩ ratios. PSR J1311–3430 (ID: 7) is the only source in our study that has ﹩{L}_{\mathrm{irr}}\gt \dot{E}﹩.
Paper: Properties of Electron-scale Magnetic Reconnection at a Quasi-perpendicular Shock
Authors: Ao Guo, Quanming Lu, San Lu, Shimou Wang, Rongsheng Wang
Figure caption: Spatial distribution of identified X points and O points. (a) Identified X (magenta “x”) and O (green dot) points marked on the in-plane magnetic field line (black line). (b) Histogram of X (magenta) and O (green) point distribution on the x-axis.
Paper: Properties of Electron-scale Magnetic Reconnection at a Quasi-perpendicular Shock
Authors: Ao Guo, Quanming Lu, San Lu, Shimou Wang, Rongsheng Wang
Figure caption: Temporal evolution of the magnetic field strength ﹩\bar{B}﹩ from Ω i0 t = 9–13.61. Here, ﹩\overline{B}﹩ is the magnetic field strength ﹩\overline{B}=\sqrt{{B}_{x}^{2}+{B}_{y}^{2}+{B}_{z}^{2}}﹩ averaged over y-direction.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: A complementary P–﹩\dot{P}﹩ diagram of the pulsars in spider systems shown in logarithmic scale where ﹩{\dot{P}}_{-21}=\dot{P}/{10}^{-21}﹩. The characteristic magnetic field strengths are indicated by dashed gray lines. The IDs of BWs are labeled in blue, while RBs are labeled in red. tMSPs are marked as red stars. The magenta line shows the MSP spin-up line according to Liu et al. (2022).
Paper: Properties of Electron-scale Magnetic Reconnection at a Quasi-perpendicular Shock
Authors: Ao Guo, Quanming Lu, San Lu, Shimou Wang, Rongsheng Wang
Figure caption: Distribution and correlation between the reconnection electric field and the guide field at X points from Ω i0 t = 9–13.61. (a) Distribution of the X points in the ﹩\left|{E}_{R}\right|-{B}_{g}﹩ space. (b) Distribution of the guide field B  g  at X points.
Paper: Reinvestigating the Gamow Factor of Reactions on Light Nuclei
Authors: Eunseok Hwang, Heamin Ko, Kyoungsu Heo, Myung-Ki Cheoun, Dukjae Jang
Figure caption: The PP as a function of E for the reactions in Table 1, adopting the fitted V 0 and ﹩{r}_{0}﹩ in Singh et al. (2019). The green solid, red dashed–dotted, and blue dashed lines indicate the ﹩{\hat{P}}_{W}(E,{V}_{0})﹩, ﹩{\hat{P}}_{G}(E)﹩, and ﹩{\hat{P}}_{\mathrm{mod}}(E,{V}_{0},{V}_{1})﹩, respectively. The vertical dashed line marks the Coulomb barrier ﹩({V}_{1})﹩ for each reaction.
Paper: Reinvestigating the Gamow Factor of Reactions on Light Nuclei
Authors: Eunseok Hwang, Heamin Ko, Kyoungsu Heo, Myung-Ki Cheoun, Dukjae Jang
Figure caption: The PP for the D+D reaction as a function of E and V 0. The solid and dotted–dashed lines represent ﹩{\hat{P}}_{G}(E)﹩ and ﹩{\hat{P}}_{\mathrm{mod}}(E,{V}_{0},{V}_{1})﹩, respectively. The color bar on the right indicates value of V 0 for ﹩{\hat{P}}_{\mathrm{mod}}(E,{V}_{0},{V}_{1})﹩. The black vertical dashed line marks the Coulomb barrier, V 1 = 0.206 MeV for the D+D reaction. A subplot provides magnified plot within the energy range from 0.7 keV to 13 keV.
Paper: Reinvestigating the Gamow Factor of Reactions on Light Nuclei
Authors: Eunseok Hwang, Heamin Ko, Kyoungsu Heo, Myung-Ki Cheoun, Dukjae Jang
Figure caption: The Gamow peak energies ﹩E{{\prime} }_{G}﹩ and E  G  as a function of temperature. The blue solid and red dashed lines indicate ﹩E{{\prime} }_{G}﹩ and E  G , respectively.
Paper: Quasiperiodic Oscillation in Short Gamma-Ray Bursts from Black Hole–Neutron Star Mergers
Authors: Yan Li, 彦 李, Rong-Feng Shen, 荣锋 申, Bin-Bin Zhang, 彬彬 张
Figure caption: Light curve and QPO modeling of GRB 130310A. Panel (a): to clearly show the QPO feature, the raw light-curve data of GRB 130310A are first smoothed through a five-point moving average (black line). Then we use the sum of two power laws (red line), to de-trend the decay phase of the light curve. This gives a better fit to the decaying trend than either a single power law or an exponential. Panel (b): residuals of the de-trending, which show a QPO signature during T 0 + (4.4 ∼ 4.9)s. Panel (c): lastly, we apply out jet precession model (Equation (18); red line) to fit the overall decaying light curve, where the temporal profile of the jet intrinsic radiative intensity adopts the two power-law function in panel (a). The precession period is 80 ms.