adsabs/AstroCLIMB huggingface dataset:
Paper: Detailed Study of Stars and Gas in a z = 8.3 Massive Merger with Extreme Dust Conditions
Authors: Anishya Harshan, Roberta Tripodi, Nicholas S. Martis, Gregor Rihtaršič, Maruša Bradač, Yoshihisa Asada, Gabe Brammer, Guillaume Desprez, Vince Estrada-Carpenter, Jasleen Matharu, Vladan Markov, Adam Muzzin, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Victoria Strait, Chris Willott
Figure caption: (a) O32-R23 diagram using dust-corrected emission line ratios. (b) R3-R2 diagram, overlaid with shock (M. G. Allen et al. 2008) and AGN (B. A. Groves et al. 2004) models from MAPPINGS in pink and red, respectively (described in Section 3.3). (c) O3Hg-O32 AGN diagnostic from G. Mazzolari et al. (2024) indicating presence of AGN. (d) Electron density diagnostic from PyNeb indicates that the electron density of MACS0416-Y1 is between 10 and 350 cm−3. (e) SFR vs. stellar mass of the four resolved components of the galaxy and the integrated galaxy with SFR main sequence from P. Popesso et al. (2023) at z = 8. (f) Stellar mass–metallicity for the four resolved components of the galaxy and the integrated galaxy with metallicity taken from DENSE BASIS SED fitting. (g) Molecular gas surface density (﹩\mathrm{log}{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩)–stellar mass surface density (log ﹩{\Sigma }_{{M}_{* }}﹩) of the integrated galaxy show that MACS0416-Y1 is more gas rich compared to cosmic noon and local galaxies. (h) SFR surface density (log ΣSFR)–molecular gas surface density (log ﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩) plot of the integrated galaxy show that MACS0416-Y1 has similar SFE to cosmic noon galaxies. In all panels, error bars where not visible are small.
Paper: Detailed Study of Stars and Gas in a z = 8.3 Massive Merger with Extreme Dust Conditions
Authors: Anishya Harshan, Roberta Tripodi, Nicholas S. Martis, Gregor Rihtaršič, Maruša Bradač, Yoshihisa Asada, Gabe Brammer, Guillaume Desprez, Vince Estrada-Carpenter, Jasleen Matharu, Vladan Markov, Adam Muzzin, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Victoria Strait, Chris Willott
Figure caption: The 2D and 1D spectrum from the NIRSpec MSA in two slits overlaid on the MACS0416-Y1 NIRCam F277W image (panel (a)). Panel (b) shows the interpolated model of the continuum used and emission lines fits in purple, the 1D spectrum is shown in black, and the error is shown in red. Panel (c) shows the spectrophotometric fit to integrated NIRCam photometry (blue circles) and NIRSpec prism spectrum (gray line) from Bagpipes (blue line) and the dust emission model fit to ALMA photometry (red).
Paper: Detailed Study of Stars and Gas in a z = 8.3 Massive Merger with Extreme Dust Conditions
Authors: Anishya Harshan, Roberta Tripodi, Nicholas S. Martis, Gregor Rihtaršič, Maruša Bradač, Yoshihisa Asada, Gabe Brammer, Guillaume Desprez, Vince Estrada-Carpenter, Jasleen Matharu, Vladan Markov, Adam Muzzin, Lamiya Mowla, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Victoria Strait, Chris Willott
Figure caption: MACS0416-Y1 in multiwavelength imaging. (a) The 353 GHz dust continuum emission map obtained from B7 ALMA observations of MACS0416-Y1. Contours are drawn at 2, 3, 4, 5, 6, 7σ with σ = 5 μJy beam−1. The same contours are overlaid on NIRCam imaging. (b) Image in NIRCam F277W, which shows the three stellar components of the galaxy along with the ALMA beam. (c) Red, green, and blue (RGB) image in UV using NIRCam F115W, F150W, and F200W. The UV emission is offset from the dust continuum showing dust obscured star formation in the galaxy. (d) RGB image in optical using NIRCam F277W, F356W, and F444W. The three clumps are marked. (e) The observed PSF-homogenized photometry of resolved components of the galaxy along with the best-fit model SED from DENSE BASIS. (f) The nonparametric star formation histories of the three resolved clumps and the galaxy halo inferred using DENSE BASIS. All components show older stellar populations and a recent burst, with the majority of the stars being formed in the galaxy halo.
Paper: Constraining the Progenitor of the Nearby Type II-P SN 2024ggi with Environmental Analysis
Authors: Xinyi Hong, Ning-Chen Sun, Zexi Niu, Junjie Wu, Qiang Xi, Jifeng Liu
Figure caption: Posterior probability distributions of mean stellar log ages of model stellar populations and the host stellar extinction. The numbers on top of and the dashed lines in each histogram show the median value with the 95% (2σ) credible interval of the marginalized posterior probability. The contours in the other panels contain 0.5σ, 1σ, 1.5σ, and 2σ marginalized posterior probability from inside to outside.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Stellar limb-darkening curves (I  λ (μ)/I  λ (μ = 1)) at different wavelengths derived from the MPS-ATLAS spectral library (N. Kostogryz et al. 2023) for the selected stars with different fundamental parameters. The MPS-ATLAS limb darkening has been rebinned to a spectral grid with R ≈ 40. The x-axis shows μ, which is the cosine of the angle of between line of sight and the stellar surface normal. The y-axis is the limb darkening normalized to the stellar disk center. The three columns display limb darkening of stars with different metallicities: M/H = −1.0 (left column), M/H = 0.0 (middle column), and M/H = 0.5 (right column). The rows illustrate limb darkening of stars with different effective temperatures, ranging from 3500 to 6200 K (from top to bottom). The colors represent wavelengths from 0.5 to 10 μm, as indicated by the logarithmic color bar. Limb darkening is wavelength dependent, occurs over the entire radius of the star, and is highly dependent on the stellar metallicity and temperature.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Centrally transiting planets (b = 0) wavelength-dependent offset from modeled transit depth. The left column shows offsets for stars with a constant effective temperature T eff = 3500 K and varying metallicity M/H = [–1.0, 0.0, 0.5]. The figures in the right column show these offsets for stars with a constant solar metallicity M/H = 0.0 and varying effective temperatures T eff = [3500, 4500, 5800, 6200] K. The thick black lines at zero offset correspond to the true transit depth. As in Figure 1, the wavelengths are scaled logarithmically. For both columns, each panel is for a different limb-darkening law: quadratic law (top), power law (middle), and Kipping–Sing three-parameter law (bottom). The quadratic law introduces up to 13 ppm offsets from the modeled transit depth in the visible.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: High impact parameter (b = 0.7) wavelength-dependent offset from modeled transit depth. See Figure 2 for a detailed description of the figure layout. Note the increased offset, up to 130 ppm for the quadratic law, compared with Figure 2.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Top: offsets from true transit depth induced by different limb-darkening laws compared to a simulated spectrum of a super-Earth from P. Niraula et al. (2022). Bottom: the same spectrum of a super-Earth from P. Niraula et al. (2022) compared to the spectrum that would be retrieved using different limb-darkening laws for the case of a b = 0.7 transit (see the text for more details). JWST instrument coverage is also included in black, alongside HST and Spitzer instruments in gray. The quadratic limb-darkening law results in a downward slope toward shorter wavelengths.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: The difference between the true impact parameter values and those obtained from fitting light curves (b Fit) vs. true impact parameters (b True). For both limb-darkening laws used to fit these impact parameters, the difference between the true and fit impact parameter values peaks for central transits.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: The same as Figure 4 but for a simulated spectrum of a warm Jupiter from P. Niraula et al. (2022). The quadratic limb-darkening law leads to a downward slope in transit depth toward shorter wavelengths and a sharp increase at λ ≈ 0.7 μm.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offset from true transit depth over wavelength for planets transiting at the highest impact parameter b = 0.9. See Figure 2 for a detailed description of the figure layout.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth for a planet transiting at b = 0.1, for both true impact parameters and those obtained from light-curve fitting.
Paper: FAST H I 21 cm Study of Blueberry Galaxies
Authors: Yogesh Chandola, Chao-Wei Tsai, D. J. Saikia, Guodong Li, Di Li, Yin-Zhe Ma
Figure caption: 21 cm emission spectra of blueberry galaxies with H I detections. The X-axes show the velocity relative to optical systemic velocity (cz) at the heliocentric frame in km s−1. The Y-axes show the flux density in mJy. Blue shades mark the 3σ noise levels. Red vertical dashed lines mark the zero relative velocity corresponding to the optical redshift of the blueberry galaxies. Green vertical dashed lines mark the H I velocity (V H I ) relative to the optical systemic velocity. In the upper panel, the blue dashed vertical line marks the optical systemic velocity of the neighboring spiral galaxy relative to the optical velocity of blueberry galaxy J1026+0426.
Paper: FAST H I 21 cm Study of Blueberry Galaxies
Authors: Yogesh Chandola, Chao-Wei Tsai, D. J. Saikia, Guodong Li, Di Li, Yin-Zhe Ma
Figure caption: Spectra of blueberry galaxies with H I nondetections. The symbols mean the same as in Figure 1.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a planet transiting at b = 0.9, for all 12 stars.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a centrally transiting planet, for all 12 model stars.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a planet transiting at b = 0.3, for all 12 stars.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a planet transiting at b = 0.5, for all 12 stars.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a planet transiting at b = 0.7, for all 12 stars.
Paper: Reliable Transmission Spectrum Extraction with a Three-parameter Limb-darkening Law
Authors: Rosa E. Keers, Alexander I. Shapiro, Nadiia M. Kostogryz, Ana Glidden, Prajwal Niraula, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh, Valeriy Vasilyev, Julien de Wit
Figure caption: Offsets from true transit depth, for a planet transiting at b = 0.1, for all 12 stars.
Paper: FAST H I 21 cm Study of Blueberry Galaxies
Authors: Yogesh Chandola, Chao-Wei Tsai, D. J. Saikia, Guodong Li, Di Li, Yin-Zhe Ma
Figure caption: (a): f H I  vs. M *. BBs observed with the FAST are shown with blue-colored circles. Gray-colored circles represent GPs with H I study by N. Kanekar et al. (2021). Filled and empty circles represent detections and nondetections, respectively. Median values of log f H I  for respective median log M * values for main-sequence galaxies from B. Catinella et al. (2018) are shown with black connected dots. Similarly, gray connected error bars mark the median log f H I  values at low and high stellar mass bins for GPs, respectively. The error bars represent the median absolute deviation (MAD) values of log f H I  at low and high stellar mass bins. For BB J1132+0809, we show the two f H I  values, one with the consideration that there is no neighboring galaxy (higher f H I ) and the other in the case that the neighboring blue galaxy is at a similar redshift (lower f H I ), connected with the dashed blue vertical line. (b): f H I  vs. sSFR. Symbols mean the same as in panel (a). Median values of log f H I  for respective median log sSFR values for main-sequence galaxies from B. Catinella et al. (2018) are shown with black connected dots. Dashed gray diagonal lines mark the H I depletion timescale (τ H I ). (c): τ H I  vs. M *. The dashed horizontal black line marks the median τ H I  for main-sequence galaxies from A. Saintonge et al. (2016) and B. Catinella et al. (2018). Dashed horizontal magenta, cyan, and orange colored lines mark the median τ H I  for mid-infrared bright BCDs in the Arecibo sample, all mid-infrared bright BCDs and other non-mid-infrared bright dwarf irregulars or BCDs, respectively, from Y. Chandola et al. (2024). The gray dashed horizontal line marks the median τ H I  value for GPs from N. Kanekar et al. (2021). For BB J1132+0809, we show two values of τ H I , connected with the blue dashed vertical line for the two cases mentioned earlier. (d): τ H I  vs. sSFR. Dashed gray diagonal lines mark the H I gas fraction. Other symbols mean the same as in panel (c).
Paper: FAST H I 21 cm Study of Blueberry Galaxies
Authors: Yogesh Chandola, Chao-Wei Tsai, D. J. Saikia, Guodong Li, Di Li, Yin-Zhe Ma
Figure caption: Top panel: M H I  vs. O32 ≡ O[III]λ5007/O[II]λ3727 ratio. Middle panel: f H I  vs. O32 ≡ O[III]λ5007/O[II]λ3727 ratio. Bottom panel: τ H I  vs. O32 ≡ O[III]λ5007/O[II]λ3727 ratio. The symbols mean the same as in Figure 3.
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: (a) Trajectory of PSP in the solar corotating frame. Black dots are plotted every 8 hr, and the green dot indicates the entering direction of PSP. (b) Trace magnetic PSD of the selected interval. (c) RTN components and magnitude of the magnetic field. The selected interval is highlighted with the vertical pink area. (d) Trace wavelet scalogram of the magnetic field from the selected interval. (e) Radial solar wind Vr and Alfvén speed VA. (f) Cross-helicity σc (left; blue) and plasma β = 2μ0P/B2 (right; black). (g) Proton density np (left; black) and Carrington longitude (right; orange). (h) Advection time τadv = (R − R⊙)/Vr (left; red) and helioradial distance R of the spacecraft (right; black).
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: Left: solar wind and Alfvén speed profile. Right: transmission coefficient of Alfvén waves as a function of launch frequency.
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: Illustration of the spherical polarization of the Alfvén wave burst. (a) Components RTN and the magnitude of the magnetic field. The selected interval is highlighted by the vertical pink area, while the Alfvén wave burst event is indicated by the red dashed lines. (b) Trace wavelet scalogram of the magnetic field for the selected interval. (c1)–(c3) Hodograms of Br − Bt, Br − Bn, and Bt − Bn for the Alfvén wave burst event. (d1)–(d3) Hodograms of Vr − Vt, Vr − Vn, and Vt − Vn from SPAN-i moments.
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: (a) Heliocentric distance of PSP as of 2024 July 1. The time range considered in this study is highlighted with the black lines and pink shaded area. (b1)–(e1) Trajectory of PSP (black line) in the Carrington corotating frame. The black dots are plotted every 8 hr, and the green dot indicates the entering direction of PSP. (b2)–(e2) PSD of the selected interval. (b3)–(e3) Wavelet scalogram of the trace magnetic field power spectrum of the selected interval. The elements in (b), (c), and (d) are identical to Figures 1 (a), (b), and (d).
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: (a) Scatter plot of 1/fmid as a function of heliocentric distance R. The window limit is the 1/fmid value estimated from a Kolmogorov f−5/3 spectrum. The error bars indicate one standard deviation in logarithmic scale. (b) Intervals with ∣σc∣ > 0.75 are selected. The two known in situ coronal holes from E10 and E12 are highlighted. (c) 1/fmid is plotted as a function of tadv = (R − R⊙)/Vr. (d) Intervals with ∣σc∣ > 0.75 are selected.
Paper: Dominance of 2 Minute Oscillations near the Alfvén Surface
Authors: Zesen Huang, 泽森 黄, Marco Velli, Chen Shi, 辰 时, Yingjie Zhu, 英杰 朱, B. D. G. Chandran, Trevor Bowen, Victor Réville, Jia Huang, 佳 黄, Chuanpeng Hou, 传鹏 侯, Nikos Sioulas, Mingzhe Liu, 明哲 刘, Marc Pulupa, Sheng Huang, 胜 黄, Stuart D. Bale
Figure caption: Illustration of the saturation 1/fmid with a 4 hr window. Orange: Kolmogorov P(f) = f−5/3 spectrum. Dotted–dashed: compensated spectrum P(f) · f in linear scale on twin axis. Gray area: frequency range where >50% of the points are out of the CoI. Green area: frequency range that contains 50% of the fluctuation energy (from 25% to 75%).
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: The magnetic configuration, including the FR, the image of the FR, and dipole 1 to model the unchanged background field and dipole 2 to model the NEF. Prior to the magnetic emergence (S = 0), the FR remained undisturbed, positioning itself just above dipole 1.
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: (a) Equilibrium surface from two views shows variations in yh, the equilibrium heights, as functions of both S and xd with yd = 2.5, possessing two topological structures, i.e., the hole (H) and the fold (F). (b) Equilibrium curves of yh vs. S with yd = 2.5 and xd = 5. The green dot marks the FR’s initial position before new flux emerges, while red dots indicate the critical states where the catastrophe occurs. (c) Distributions of S* in the space (xd, yd) with colors for S* values. Regions filled with triangles indicate the combinations of parameters that yield a catastrophe followed by a plausible eruption, regions filled with downward-pointing triangles indicate cases of the catastrophe followed by the failed eruption, and regions filled with crosses are for the case without a catastrophe. The dashed line corresponds to C(xd, yd) = 0.
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: Six cases of the FR evolution. Columns, from left to right, illustrate the evolution in xh with respect to S, the evolution in yh, and the magnetic structure at the critical state. Each row illustrates a distinct case. Green dots on the curve and crosses in the magnetic structure represent initial positions of the FR, while red ones mark critical positions. In cases 5 and 6 (fifth and sixth rows), new equilibrium locations exist for the FR with the same S at the critical point, so the FR might jump to the new location as indicated by the blue dots and crosses. The new magnetic structures after the catastrophe are plotted as cyan curves in the right panels for cases 5 and 6.