adsabs/AstroCLIMB huggingface dataset:
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Panels (a) and (b) show EP/WXT images of EP J182730.0−095633 from 2024 September 3 to 4 (ObsIDs are 06800000068 and 06800000067, respectively). Panel (c) presents EP/FXTA image obtained with FF mode on 2024 September 6. Panel (d) displays ATCA (5.5 GHz) images on 2024 September 12. The restoring beam (19﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2, 5﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5) is indicated as a gray elliptical shape in the lower left corner. Panels (e) and (f) show NIR (H-band) images obtained from GROND on 2024 September 8 and 19, respectively. The potential NIR counterpart is denoted by the white arrow in panel (e). The white, green, and cyan circles represent the positional errors of WXT, FXT, and XRT, respectively.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Long-term evolution of the multiwavelength properties of EP J182730.0–095633. Top to bottom: the evolutions of the unabsorbed flux in the 0.5–10 keV band, the photon index (Γ), the hydrogen column density (NH), the observed magnitude in the optical/infrared bands, and the radio peak flux density of ATCA and MeerKAT. The X-ray flux during the decaying phase is fitted by either a broken power-law model (gray solid curve) or a broken exponential model (black dashed curve). See Section 3.2.1 for more details. The results of a few optical/infrared observations after the X-ray outburst, where only upper limits have been obtained, are not shown for clearer data visualization. In addition, primarily due to the low signal-to-noise ratio of the data, the X-ray absorbing column density NH in some observations cannot be well constrained within physically reasonable ranges and are fixed at 3.1 × 1022 cm−2; hence, they are not shown in this figure (see text and Table B1 for more details).
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Posterior distributions of the model parameters for the ionization cone. Lower panels show the marginalized two-dimensional posterior probability distributions determined via MCMC of the four model parameters for the ionization cone, i.e., the inclination i, the position angle PA, the unobscured solid angle fraction ﹩{\mathrm{log}}\,_{10}(1-{f}_{\mathrm{obsc}})﹩, and the UV-luminous lifetime of the quasar ﹩{\mathrm{log}}\,_{10}({t}_{{\rm{QSO}}}/{\rm{yr}})﹩. Light and dark gray histograms in the top diagonal panels show the one-dimensional prior and posterior distributions, respectively.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Biconical model for a quasar’s ionization cone. Left to right: panels show the model for the ionization cone with varying parameters, i.e., the opening angle of the obscuring medium ψ, which corresponds to the solid angle obscured fraction fobsc, the inclination of the cone i, the position angle PA, and the timescale of the quasar’s UV-luminous radiation tQSO. All other parameters are kept fixed to the values as indicated above each panel. The top panels show the illuminated area around the central quasar, while the bottom panels illustrate the expected mean transmitted flux profile for a highly idealized sample of 1000 galaxies, which are all aligned and equally distributed along one axis of the sky, ysky, while xsky = 0.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Flux transmission along individual galaxy sightlines. The panels show the continuum-normalized, transmitted flux (black) around the systemic redshift of the quasar at d∥ = 0 pMpc with spectral uncertainties (gray) along the 12 background galaxy sightlines, which are used to model the quasar’s ionization cone. The red lines show the expected transmission profile from the best fit of the quasar’s ionization cone extracted at each galaxy’s location on the sky (see Section 4).
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Joint spectral fitting of EP/FXT (module B, 0.5–10 keV) and NuSTAR (4–79 keV) with an absorbed cutoff power-law model. Note that the residual feature at ∼2 keV is due to a calibration issue.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Power density spectra of the EP/FXTA data (left panel; ObsID 06800000091) and NuSTAR data (right panel; ObsID 91001334002), with the bottom of each panel showing the power ratio between the data and best-fitting bending power-law model.
Paper: The Light Echo of a High-redshift Quasar Mapped with Lyα Tomography
Authors: Anna-Christina Eilers, Minghao Yue, Jorryt Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, Rongmon Bordoloi, Gabriel Brammer, Yi Kang, Daichi Kashino, Ruari Mackenzie, Rohan P. Naidu, Benjamín Navarrete
Figure caption: Map of the quasar’s ionized bubble. The central quasar is indicated by the yellow star, and all galaxy sightlines are shown as blue dashed lines. The underlying colormap indicates the level of the expected Lyα flux transmission, while the overplotted black contours illustrate the best-fit ionization cone. The thin white parabolas show isochrones, i.e., outlines of the quasar’s light echo at different times, while the thick white line indicates the best fit to our data of ﹩{\mathrm{log}}\,_{10}({t}_{{\rm{QSO}}}/{\rm{yr}})=5.{7}_{-0.3}^{+0.1}﹩. Thus, all shaded regions are not illuminated by the quasar, and only the congruence of the ionization cone and illuminated parabola due to the quasar’s light echo is illuminated.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Quasi-simultaneous X-ray vs. radio and NIR luminosities for LMXBs, including EP J182730.0–095633. Left: the radio–X-ray (LRadio–LX) fundamental plane for XRBs, adopted from A. Bahramian & A. Rushton (2022). The results of EP J182730.0−095633 are represented by red symbols, assuming various distance values. Right: the position of EP J182730.0–095633 on the NIR–X-ray (LNIR(JHK)–LX) correlation for XRBs (D. M. Russell et al. 2006). The data are taken on September 7 (the results barely change for those of September 8 and 9) and corrected for absorption using extinction values of AH = 2.8 ± 0.1 mag. For brevity, only the results of the H band are displayed here as a representative, with similar results for the other two bands.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Left panel: the rms spectrum calculated using the same data set as Figure 2 (EP/FXT+NuSTAR on 2024 September 11). The blue circles are from EP-FXT, and green circles are from NuSTAR. Right panel: the relation between the low-frequency break (νb) of the PSD and the centroid frequency of the QPO signal (νqpo), with the results of EP J182730.0–095633 denoted as blue circles. Here we use the PSDs from September 7–10 (FXT), September 11 (NuSTAR), September 11–12 (FXT), and September 13–17 (FXT), where the QPO significance exceeds 3σ. The black dashed line is the empirical W–K relation between the two variables for type C LFQPOs. νqpo are 38.2  ±  0.2 mHz, 38.3  ±  0.3 mHz, 36.4  ±  0.4 mHz, and 34.4  ±  0.4 mHz for the four PSDs, respectively, while νb are 55  ±  6 mHz, 43  ±  2 mHz, 60  ±  5 mHz, and 36  ±  4 mHz.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: PSDs of EP/FXT and NICER during the outburst. The centroid frequency of the most prominent QPO holds steady at ∼0.04 Hz. For the EP/FXTA (TM mode) data, we combined them to improve the signal-to-noise ratio. The absence of the QPO signal in the final FXT data set (from September 20 to 24) is likely attributed to the extremely low count rate of the source during this period.
Paper: Einstein Probe Discovery of EP J182730.0−095633: A New Black Hole X-Ray Binary Candidate in Faint Outburst?
Authors: H. Q. Cheng, Q. C. Zhao, L. Tao, H. Feng, F. Coti Zelati, H. W. Pan, A. L. Wang, Y. N. Wang, M. Y. Ge, A. Rau, A. Marino, L. Zhang, W. J. Zhang, F. Carotenuto, L. Ji, C. C. Jin, D. Y. Li, B. F. Liu, Y. Liu, E. L. Qiao, N. Rea, R. Soria, S. Wang, Z. Yan, W. Yuan, B. Zhang, G. B. Zhang, S. N. Zhang, W. D. Zhang, A. Beardmore, J. S. Bright, X. L. Chen, Z. Fan, S. Y. Fu, J. P. U. Fynbo, J. W. Hu, J. J. Jin, P. G. Jonker, A. K. H. Kong, E. Kuulkers, C. K. Li, H. L. Li, Z. K. Lin, C. X. Liu, H.-Y. Liu, J. Z. Liu, X. W. Liu, Z. Lu, C. Maitra, H. Y. Mu, C.-Y. Ng, Y. L. Qiu, S. Tinyanont, Y. Wang, S. X. Wen, S. S. Weng, Jianfeng Wu, D. Xu, Y. K. Yan, Z. Yan, Y.-P. Yang, P. Zhang, S. Zhang, Q. Zhao, Z. M. Cai, Y. Chen, Y. F. Chen, C. Z. Cui, W. W. Cui, H. B. Hu, M. H. Huang, S. M. Jia, G. Jin, Z. X. Ling, H. Q. Liu, S. L. Sun, X. J. Sun, Y. F. Xu, C. Zhang, M. Zhang, Y. H. Zhang
Figure caption: Evolutionary trend of the photon index Γ using two different data analysis strategies for EP/FXT, NICER, Swift/XRT, and NuSTAR data. The results shown as gray symbols are obtained by fixing the column density NH to the typical parameter value of 3.1 × 1022 cm−2 during the outburst. The result obtained with variable column density (same as in Figure 3) is also plotted for comparison.
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: Time evolution of (a) mean squared current density, jz, and (b) mean squared magnetic (black) and kinetic (orange for the plasma, and blue for the neutral fluid) energy. Solid and dashed lines correspond to the coupled and uncoupled cases, respectively. These values are normalized by their initial value at t = 0. Note that the initial value is the same for the uncoupled and coupled cases. The vertical dotted line is at t = 4800, indicating the representative time of the maximum turbulence activity.
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: Snapshots of the current density, jz, for (a) the uncoupled and (b) coupled case.
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: (a) Color map shows the current density, jz, for the coupled case at t = 4800, contour lines correspond to the vector potential, and a crossed mark is an X-point of magnetic reconnection. (b) Probability distribution function (PDF) of the current density, jz, for the coupled case (solid) at t = 4800. The dashed line corresponds to a Gaussian distribution.
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: Power spectral density (PSD), with respect to the wavenumber, of the magnetic (black) and kinetic (orange for the plasma, and blue for the neutral fluid) energy for (a) the uncoupled and (b) coupled case at t = 4800.
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: (a) Snapshot of the magnitude of the velocity difference between the plasma and neutral fluid at t = 4800. Counter lines correspond to the vector potential. (b) Profile of the velocity difference along the dashed line in panel (a).
Paper: Survival of 2D Turbulence in the Local Interstellar Medium
Authors: Masaru Nakanotani, Gary P. Zank
Figure caption: Snapshot of the ionization fraction, ξ, normalized by the initial ionization fraction, ξ0 = 1/3, at t = 4800.
Paper: Coexistence of Decaying and Decayless Kink Oscillations in a Bundle of Coronal Loops Triggered by an X6.3 Solar Flare
Authors: Yi Dai, Xiansheng Zheng, Xinping Zhou, Linqiao Jiang, Jie Zheng, Haiyin Qing, Zhining Qu
Figure caption: (a) Soft X-ray flux profiles of the 2024 February 22 X6.3-class solar flare recorded by GOES/XRS in the 1.0–8.0 Å (red) and 0.5–4.0 Å (blue) channels. The flux began to rise around 22:10 UT, marking flare onset, with a minor preflare enhancement (red arrow) near 22:15 UT. The main flare peaks at 22:34 UT, as indicated by the dashed lines. (b) Hard X-ray count rates observed by ASO-S/HXI in four energy bands (10–20, 20–50, 50–100, and 100–300 keV), showing a rapid increase in high-energy emission during the impulsive phase. The shaded area in both panels indicates the period when kink oscillations were observed in the coronal loops.
Paper: Coexistence of Decaying and Decayless Kink Oscillations in a Bundle of Coronal Loops Triggered by an X6.3 Solar Flare
Authors: Yi Dai, Xiansheng Zheng, Xinping Zhou, Linqiao Jiang, Jie Zheng, Haiyin Qing, Zhining Qu
Figure caption: Panels (a1) and (a2) show the SDO/AIA 131 Å intensity images at 22:20:06 UT and 22:23:42 UT, respectively. White boxes indicate the two subregions used for subsequent differential emission measure (DEM) analysis: DEM1 (S1) and DEM2 (S2). Panels (b1) and (b2) display the corresponding emission-weighted temperature maps, and panels (c2) and (c3) present the total emission measure (EM) maps (in units of 1028 cm−5). The upper right plot shows the DEM distribution for region S1, peaking at T ≈ 3.0 MK with EM ≈ 3.1 × 1026 cm−5; the lower right plot shows the DEM distribution for region S2, peaking at T ≈ 2.9 MK with EM ≈ 0.6 × 1026 cm−5.
Paper: Coexistence of Decaying and Decayless Kink Oscillations in a Bundle of Coronal Loops Triggered by an X6.3 Solar Flare
Authors: Yi Dai, Xiansheng Zheng, Xinping Zhou, Linqiao Jiang, Jie Zheng, Haiyin Qing, Zhining Qu
Figure caption: TD plots of five selected slices (S1–S5) derived from AIA 171 Å images, illustrating transverse oscillations of coronal loops triggered by the 2024 February 22 X6.3 flare. The zero-point in each plot corresponds to the loop footpoints as defined in Figure 2(g). Each slice exhibits distinct oscillation amplitudes, periods, and decaying characteristics, influenced by local magnetic and plasma conditions.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Parameter space of BHOB triples before the second SN. Blue contours show the density of triples with inner binaries that survive the second SN and form stable NSBH binaries. Red contours represent systems successfully forming stable NSBH triples. Scatter points highlight systems that will lead to tertiary-driven NSBH mergers, with the color indicating their residual eccentricity e20 at a dominant GW frequency fGW = 20 Hz (L. Wen 2003). The parameter window for surviving NSBH triples (red) can be understood as a result of several constraining limits, marked with hatched and dotted regions: diagonally hatched and dotted regions indicate regions where the natal kick tends to disrupt the inner binary, the natal kick tends to disrupt the outer binary, and the SN mass loss disrupts the outer binary, respectively (see Equations (7)–(9)). Below a1 ≈ 10 R⊙, inner binaries would undergo a stellar merger at the ZAMS (horizontally hatched) and may only be occupied by systems surviving a CE phase. The square hatched region indicates the region of dynamical instability of the triple. The black dashed line shows jGW = jGR for a fiducial triple with m1 = 10 M⊙, m2 = 1.5 M⊙, m3 = 1 M⊙, and e2 = 0.67.
Paper: Orbital Eccentricity and Spin–Orbit Misalignment Are Evidence that Neutron Star–Black Hole Mergers Form through Triple Star Evolution
Authors: Jakob Stegmann, Jakub Klencki
Figure caption: Distributions of the inner semimajor axis (left panel) and semimajor axis ratio (right panel) of triples studied in this work. Gray patches indicate the distributions of Ntot = 107 stellar triples at ZAMS (initial conditions), black lines show all triples that survive the first SN and form a BHOB in the inner binary, blue lines show all inner binaries that survive the second SN and form an NSBH (regardless of whether the outer binary remained stable or not), and blue and turquoise patches highlight the subset of NSBHs that underwent some sort of MT and a CE evolution, respectively. Red lines show all stable triples that develop an NSBH in the inner binary, red patches show those that eventually lead to an NSBH merger, and gold solid and dashed lines highlight the subset of those that retain residual eccentricity upon merging (e20 > 0.1) and coalesce with large BH spin–orbit misalignment (﹩\cos {\theta }_{{\rm{BH}}}\lt 0﹩), respectively.