adsabs/AstroCLIMB huggingface dataset:
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Left: the EP/FXT spectrum in the 0.3–10 keV band by stacking the first six observations in the plateau phase (total exposure ∼35 ks). The photon index for the stacked EP/FXT spectrum is 1.8 ± 0.1 if fitted by an absorbed power law, consistent with that of EP/WXT. Note that the X-ray spectrum is relatively flat and consistent with nonthermal emission. Right: X-ray light curves of EP241021a observed by EP/WXT, EP/FXT, and XMM-Newton. The EP/FXT fluxes in the upper panel were obtained with the photon index tied during fitting. The lower panel shows the distribution of the photon index for the power-law component that was allowed to vary in the individual spectral fittings and is consistent with the value Γ = 1.8 within the errors. More details of modeling the light-curve evolution can be found in Appendix B.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Optical (r-band) light curve of EP241021a. The photometric data are taken from our own observations (Section 2.3) and those reported in GCN Circulars and M. Busmann et al. (2025). Note that the flux excess observed by SVOM/VT (at Δt ≈ 18.6 days) is due to the use of a broader r-band filter and hence should be treated with caution. For comparison, we present the r light curves of EP240414a (J. N. D. van Dalen et al. 2025) and EP250108a (W. X. Li et al. 2025)—the two EFXTs that are associated with SNe Ic-BL—as well as jetted TDEs Sw J2058 (S. B. Cenko et al. 2012) and AT 2022cmc (I. Andreoni et al. 2022). The peculiar EFXT EP240408a with an intermediate timescale but without an optical counterpart (down to 26 mag) is also plotted for comparison, assuming it is at z = 0.5 (B. O’Connor et al. 2025; W. Zhang et al. 2025). The lower panel shows the r − z color evolution of EP241021a as a function of time. It is clear that the color is persistently red up to at least ∼30 rest-frame days since discovery.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Left: the EP/WXT light curve of the count rate in the 0.5–4 keV band, in which an intense flare lasting ∼91.9 s was observed. Right: the WXT X-ray spectrum during the flare period, which can be described by an absorbed single power-law model with photon index ﹩{\rm{\Gamma }}=1.{8}_{-0.54}^{+0.57}﹩.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Multiwavelength images of EP241021a. (a) The image of EP241021a detected in one of the WXT CMOS detectors. (b) The image of EP241021a taken by one of the follow-up FXT observations. The white circle represents the center of the X-ray source localized by FXT, with a radius of 1﹩^{\prime} ﹩, while the yellow circle shows the localization of WXT with an error circle of 3﹩^{\prime} ﹩. (c) The GTC r-band image observed on 2024 December 7, in which the optical counterpart was found within the FXT error circle (radius ∼10″; dashed white circle). The radio position obtained by VLBA is marked by the small red circle, which can localize the optical counterpart with a positional uncertainty of ∼1 mas.
Paper: EP241021a: A Months-duration X-Ray Transient with Luminous Optical and Radio Emission
Authors: Xinwen Shu, Lei Yang, Haonan Yang, Fan Xu, Jin-Hong Chen, Rob A. J. Eyles-Ferris, Lixin Dai, Yunwei Yu, Rong-Feng Shen, Luming Sun, Hucheng Ding, WeiKang Zheng, Ning Jiang, Wenxiong Li, Ning-Chen Sun, Dong Xu, Zhumao Zhang, Chichuan Jin, Arne Rau, Tinggui Wang, Xue-feng Wu, Weimin Yuan, Bing Zhang, Kirpal Nandra, Alexei V. Filippenko, Frédérick Poidevin, Roberto Soria, Amit Kumar, David S. Aguado, Fangxia An, Tao An, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pietro Baldini, Thomas G. Brink, Pathompong Butpan, Zhiming Cai, Alberto J. Castro-Tirado, Huaqing Cheng, Weiwei Cui, Joseph Farah, Shaoyu Fu, Johan P.U. Fynbo, Xing Gao, Dawei Han, Xuhui Han, D. Andrew Howell, Jingwei Hu, Shuaiqing Jiang, Brajesh Kumar, Weihua Lei, Dongyue Li, Chengkui Li, Huaqiu Liu, Xing Liu, Yuan Liu, Xiaowei Liu, Alicia López-Oramas, David López Fernández-Nespral, Justyn R. Maund, Curtis McCully, Zexi Niu, Megan Newsome, Paul O'Brien, Haiwu Pan, Yu Pan, Estefania Padilla Gonzalez, Ismael Pérez-Fournon, Walter Silima, Hui Sun, Shengli Sun, Xiaojin Sun, Giacomo Terreran, Samaporn Tinyanont, Junxian Wang, Yanan Wang, Yun Wang, Klaas Wiersema, Yunfei Xu, Yongquan Xue, Yi Yang, Fabao Zhang, Juan Zhang, Pinpin Zhang, Wenda Zhang, Yonghe Zhang, Haisheng Zhao, Zipei Zhu, Liping Xin, Zhuheng Yao, Bertrand Cordier, Jianyan Wei, Yulei Qiu, Frédéric Daigne
Figure caption: Keck spectrum of EP241021a taken on 2024 October 30 and the power-law model that can describe the continuum likely dominated by the transient. Wavelengths were converted into the rest frame according to the redshift z = 0.7478, which was obtained from the labeled narrow emission lines. We show in the inset the single Gaussian models that fit the Hβ and [O III] emission lines.
Paper: Detection of Young Massive White Dwarfs in Core-collapsed Globular Cluster NGC 362
Authors: R. K. S. Yadav, Arvind K. Dattatrey, Annapurni Subramaniam, Geeta Rangwal, Ravi S. Singh
Figure caption: (a) The FUV image of 1.75﹩^{\prime} \times 1.75^{\prime} ﹩ for the cluster NGC 362 in the F148 filter. Directions are shown in the figure. The 17 FUV bright WDs are shown with the star ID numbers. Panel (b) shows the (mF275W-mF336W) vs. mF275W, while panels (c) and (d) show the (F148W-F606W) vs. F148W and (F169M-F606W) vs. F169M CMDs. Magenta color in panels (c) and (d) represents the WDs. The open magenta squares represent the WDs without contamination from neighboring stars.
Paper: Detection of Young Massive White Dwarfs in Core-collapsed Globular Cluster NGC 362
Authors: R. K. S. Yadav, Arvind K. Dattatrey, Annapurni Subramaniam, Geeta Rangwal, Ravi S. Singh
Figure caption: The SEDs of the 14 single-component and three two-component (WD 15, WD 16, and WD 17) WDs. The blue points represent the synthetic flux from the model used to fit the observed SED. The Teff values of the hot (A) and cool (B) components are displayed for the two-component WDs. The UVIT and HST data points are represented in cyan and red, while the model data are represented with blue points. The D. Koester (2010), F. Castelli & R. L. Kurucz (2003), and combined spectra are shown by gray, cyan, and black curves, respectively. ΔF/F is the fractional residual.
Paper: Detection of Young Massive White Dwarfs in Core-collapsed Globular Cluster NGC 362
Authors: R. K. S. Yadav, Arvind K. Dattatrey, Annapurni Subramaniam, Geeta Rangwal, Ravi S. Singh
Figure caption: The H-R diagram of hot and cool components of the WDs. The red points represent the WDs, while the blue points represent the cool components (MS stars). The WD cooling curves for different masses are shown in different colors (defined in the legend). The black curve represents the isochrone taken from S. L. Hidalgo et al. (2018) and A. Pietrinferni et al. (2021).
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: (a, b) Time-integrated swirl distributions Fsw(x, y) at TR1 (z = 3.6 Mm) and TR2 (z = 20.4 Mm) for ﹩{n}_{{\rm{\min }}}=2﹩, ﹩{n}_{{\rm{\max }}}=6﹩. Color indicates normalized swirl counts. (c, d) Temporal evolution of xy-integrated Poynting flux in minisquares L0 and U1, respectively. Blue and orange hatched areas show periods with counterclockwise and clockwise swirls. (e) Mean Poynting flux during swirl (﹩\overline{{S}_{z}}| {\rm{sw}}﹩, solid) and nonswirl (﹩\overline{{S}_{z}}| {\rm{ns}}﹩, dashed) periods at TR1 (blue) and TR2 (orange). (f) Upper (Rupper, solid) and lower (Rlower, dashed) limits of swirl contribution ratio to total Poynting flux at TR1 (blue) and TR2 (orange).
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: (a) Three-dimensional magnetic field lines at t = 17,500 s with vertical velocity (vz) maps at z = 0 Mm and z = 24 Mm. (b) Vertical velocity (vz) at z = 0 Mm in color, with streamlines of horizontal velocity (vx, vy). Green contour marks a magnetic flux concentration (MC), defined by ∣Bz∣ ≥ 500 G. (c) Swirling strength (λsw) at z = 1.8 Mm in color. Green patch: Bz ≥ 500 G at z = 0 Mm. Rectangle indicates panel (b) region.
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: Solid line: the occurrence frequency distribution of swirl-driven coronal heating energy (dN/dE), normalized by simulation time (Ptot = 6600 s) and area (L⊥Lz=14 × 24 Mm2). Dashed line: fitted power law. Orange dots with error bars: estimated heating energies from quiet Sun coronal observation (V. Upendran et al. 2022).
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: (a) Time-integrated swirl distribution Gsw in the corona (3.6 Mm ≤ z ≤ 20.4 Mm) for ﹩{n}_{{\rm{\min }}}=2﹩, ﹩{n}_{{\rm{\max }}}=6﹩. (b) Maximum temperatures of swirl-driven heating events within minisquare A0 in panel (a), shown at event midpoints. Swirl periods are marked with blue (counterclockwise) and orange (clockwise) hatches.
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: The maximum temperatures of the coronal heating events at the midpoints between the start and end times for the case with ﹩{n}_{\min }=2,\,{n}_{\max }=6﹩ are plotted within each minisquare (A0–A5) shown in Figure 4(a). Simultaneously, the swirl periods are shown as blue and orange hatched areas , indicating counterclockwise and clockwise rotation directions, respectively.
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: Time evolution of xy-averaged Poynting flux within the minisquares (L0–L7) outlined in the swirl distribution map at TR1 (Figure 2(a)) in the case of ﹩n{}_{\min }=2,\,{n}_{\max }=6﹩. Blue and orange hatched areas indicate periods when swirls are present within the box, with counterclockwise and clockwise rotation angles, respectively.
Paper: A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation
Authors: Hidetaka Kuniyoshi, Shinsuke Imada, Takaaki Yokoyama
Figure caption: Same as Figure 6 but showing xy-averaged Poynting flux within the minisquares (U0–U7) at TR2 (Figure 2(b)).
Paper: From Photospheric Footpoint Motion to Plasmoid Ejection: A Two-stage Reconnection Process in a Small-scale Chromospheric Jet
Authors: Zehao Tang, Yuandeng Shen, Dongxu Liu, Surui Yao, Chengrui Zhou, Xiaobo Li
Figure caption: Evolutionary images of the development of the reconnection current sheet. Panels (a)–(e) are zoomed-in versions of NVST Hα observations, whose FOV is represented by the white box in Figure 1(m). Their contrasts are adjusted to better visualize the development of the reconnection current sheet. Red arrows in panels (b)–(d) symbolize the propagating process of a plasmoid.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: From top to bottom, we show how the the continuum NAI (top panel; P. Curone et al. 2025), stellar accretion rates (second panel from top), normalized stellar accretion rates (to the square of the stellar mass; third panel), and NIR excess (A. Garufi et al. 2018; bottom panel) depend on the range of tilt amplitudes we infer from our model. The outcomes of Spearman rank, Kendall τ, and permutation correlation tests are shown in terms of correlation statistic and p-value. We exclude cases where inclination is unfavorable owing to the appearance of the back side of the disk.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the tilt amplitudes inferred using 12CO and 13CO isotopologues. The black dashed line shows 1:1 agreement. Points are colored by the global inclination of the disk. The disks for which the back side is visible in the line profiles are circled in red.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Slice of our model density profile used for radiative transfer calculations of scattered light. The red line shows the radius beyond which we directly use the inferred inclination and position angle profile from the residual LOS velocity map. Inside of this we make an arbitrary cubic spline extrapolation. The cyan dashed line traces the midplane. We use a flaring exponent of 1.03 and a midplane density profile ∝r−1.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: The relationship between inclination and PA tilt amplitude, with points being colored by overall inclination of the system. The points circled in red are those for which the back side of the disk is visible in the 12CO line profiles.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: The extrapolation of the warp file we infer for MWC 758 into the inner disk, as required by our radiative transfer model. The two inner points were chosen arbitrarily to extrapolate the warp profile with a cubic spline.
Paper: exoALMA. XVIII. Interpreting Large-scale Kinematic Structures as Moderate Warping
Authors: Andrew J. Winter, Myriam Benisty, Andrés F. Izquierdo, Giuseppe Lodato, Richard Teague, Carolin N. Kimmig, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Cassandra Hall, Caitlyn Hardiman, Thomas Hilder, John D. Ilee, Misato Fukagawa, Cristiano Longarini, François Ménard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Same as Figure 7, but with the averaged logarithmic warp amplitude for the sample of exoALMA disks on the x-axis. Results of statistical correlation tests are shown as in Figure 7.
Paper: From Photospheric Footpoint Motion to Plasmoid Ejection: A Two-stage Reconnection Process in a Small-scale Chromospheric Jet
Authors: Zehao Tang, Yuandeng Shen, Dongxu Liu, Surui Yao, Chengrui Zhou, Xiaobo Li
Figure caption: A cartoon interpretation of the present event. Panel (a) shows the magnetic skeleton at the cool jet stage, in which blue areas represent cold (Hα) reconnection outflow. Panel (b) displays the lengthening of the reconnection current sheet and the correspondingly formed plasmoid, where red areas represent hot (EUV) reconnection outflow. Panel (c) illustrates the upward-propagating process of the plasmoid as well as its collision with the upper cusp and the in-between secondary current sheet. Panel (d) represents the merging process of the plasmoid with the upper cusp and resulting blob. Note that this cartoon incorporates certain features not directly observed in our observation.
Paper: From Photospheric Footpoint Motion to Plasmoid Ejection: A Two-stage Reconnection Process in a Small-scale Chromospheric Jet
Authors: Zehao Tang, Yuandeng Shen, Dongxu Liu, Surui Yao, Chengrui Zhou, Xiaobo Li
Figure caption: DEM analysis before and after the blob ejection. Panels ((a) and (c)) and ((b) and (d)) represent density and averaged temperature maps, respectively. Key observational features, such as jet, jet base, and blob, are annotated in the corresponding panels.