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: The radio SEDs over four epochs that have quasi-simultaneous observations at different frequencies. For nondetections, the corresponding 5σ upper limits on flux density are shown. The colored lines represent the best fit to each SED from our MCMC modeling, which are the model realizations on a basis of 200 random samples from the MCMC chains.
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: The optical spectrum observed by GTC and Keck on Δt = 2, 8, and 9 days since the discovery of EP241021a . While the GTC spectra have lower resolution and lower S/N than the Keck spectrum, the narrow emission lines of [O III] λ5007, [O III] λ4959, and [O II] λ3727 are detected, confirming the Keck redshift of z = 0.7478.
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: Parameters derived for EP241021a by using the three-jet model. The contour curves represent the 1σ−2σ−3σ confidence levels. The best-fit parameter values, along with their 1σ uncertainties, are indicated above the panels of their respective posterior distributions.
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: X-ray light curve in the 0.5–4 keV range within ∼1–50 rest-frame days since discovery. The data are taken from EP/WXT, EP/FXT, and XMM-Newton observations. Our best-fit model with three power laws is shown as gray curves, representing random samples from the MCMC chains. Right: marginalized posterior distributions for each model parameter are shown on the diagonal, where dashed lines indicate the median and 68% confidence interval.
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: EP241021a and the observed L–T–E relation for 210 GRBs (F. Xu et al. 2021; C. Deng et al. 2023). Long GRBs and short GRBs are marked with blue circles and purple squares, respectively. EP241021a is an outlier of this relation, indicating that its plateau originates from a different mechanism compared to the typical GRB plateau.
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: The same as Figure B1 but for the model with three piecewise power laws.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: Left: color map of the current density in the z-direction at t = 3 tA for the simulation with χ = 0.5. The bright green lines indicate isocontours of the out-of-plane component of the vector potential Az. Several strong X-points are marked with an “×” and serve as origins for the normal and tangential unit vectors ﹩\hat{{\boldsymbol{n}}}﹩ (red arrows) and ﹩\hat{{\boldsymbol{t}}}﹩ (blue arrows), respectively. Right: the left column shows the average profiles of the magnetic field components parallel (blue lines) and perpendicular (gray lines) to the current sheet, plotted along the n-direction, for χ = 0.1 (top row), χ = 0.5 (middle row), and χ = 0.9 (bottom row). The right column displays the average profiles of the various contributions to Ohm’s law, including the total electric field (black lines), the positron pressure gradient contribution (purple lines), the electron pressure gradient contribution (red lines), and the electron–positron electromotive contribution (orange lines), also along the n-direction. As before, each row corresponds to a different value of χ.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: Upper row: snapshots of the (normalized) total number density n/〈n〉rms at time t = 3 tA for (a) χ = 0.1, (b) χ = 0.5, and (c) χ = 0.9 (c). Lower row: (d) shows the evolution of the rms of the out-of-plane component of the current density for different concentration ratios; (e) shows the power spectrum of the magnetic field when turbulence is fully developed at t = 3 tA, with the corresponding slopes; and (f) shows the same as (e), but for the electric field. The power spectra are normalized to the rms of the in-plane magnetic field. The thin solid lines mark the spectral slope breaks in the inertial range.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: PDFs of the modulus of the electric field ∣E∣ at the time t = 3 tA, as computed by the aggregation of the various components (∣EOhm∣, black line) or by the total electric field of the simulation (﹩| {{\boldsymbol{E}}}_{{\rm{sim}}}| ﹩, red line). The different panels refer to χ = 0.1 (left), χ = 0.5 (middle), and χ = 0.9 (right).
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: Top panel: PDFs of the various contributions to the electric field in the z-direction, as given in Equation (4), for χ = 0.5 and at t = 3 tA. Bottom panel: power spectra of the dominant contributions reported in the top panel. Marked with the gray vertical line is the typical proton scale.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: PDFs of the reconnection rates (symbols) for χ = 0.1 (blue), χ = 0.5 (red), and χ = 0.9 (green), with the corresponding linear fits shown as solid lines in matching colors. The dashed vertical lines indicate the median reconnection rates for each distribution, while the inset shows the evolution of the number of X-points (#XP) for each configuration.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: Consistency study showing the particle kinetic energy distributions expressed as a function of the Lorentz factor for electrons (left panel), positrons (middle panel), and protons (right panel). The simulations refer to the case with χ = 0.5 and show the different setups listed in Equation (A1) at t = tA.
Paper: Turbulence and Magnetic Reconnection in Relativistic Multispecies Plasmas
Authors: Mario Imbrogno, Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla, Benoît Cerutti, Sergio Servidio
Figure caption: The same as Figure 3 but for χ = 0.1 (left) and χ = 0.9 (right). Much of what is discussed for the case χ = 0.5 in Figure 3 applies also for the other concentrations.
Paper: The Kinematic Age of 3I/ATLAS and Its Implications for Early Planet Formation
Authors: Aster G. Taylor, Darryl Z. Seligman
Figure caption: Inferred Interstellar Object Prior. An approximate interstellar object local age distribution, assuming that the weight for each interstellar object is equal. The 1σ uncertainty is shown as a shadowed region. We also show the expected local age distributions assuming that interstellar objects are not destroyed (Γ = 0) and are uniformly destroyed at a rate Γ = 0.123 Gyr−1.
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: The cutout image and the photo-z analysis of STUDIES-COSMOS-450-019. The left upper and lower panels show 1﹩{}^{{\prime} }﹩ cutout images of the SCUBA-2 450 μm and 850 μm maps, respectively, with orange contours starting at 1σ with a step of 1σ. The green squares mark the position and size of the JWST cutout image shown in the middle panel. The middle panel presents a 6″ RGB (F444W − F277W − F150W) composite image generated from NIRCam data, with white ALMA contours, starting at 3σ with a step of 1σ. The blue and red dashed lines represent the apertures of photometry for photo-z analysis of the foreground lens and background source, respectively. The right panels display the results of the photo-z analysis, including SED fitting and the redshift probability distributions. Vertical lines mark the spectroscopic redshifts obtained from previous studies. The aperture used for flux measurement is indicated in the middle panel.
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: An example of the result from lens modeling for STUDIES-COSMOS-450-019. From left to right: the observed NIRCam F444W image centered on the foreground lens, the reconstructed model image with the applied mask, and the residual between the model and the observed image. All images have the same size, orientation, and display flux in logarithmic scale.
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: The sky positions of all 18 strongly lensed faint DSFG candidates identified by this work. The two yellow dashed circles show the footprint of STUDIES. The blue dot and green diamond represent the strongly lensed DSFGs found in previous studies (P. van Dokkum et al. 2024; J. Pearson et al. 2024), which are also identified by our method.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Apparent flux cancellation event in the NIRIS data, captured between 2018 July 29T17:31:10 and 2018 July 29T17:39:05. (a) The NIRIS FOV shortly before the event, including a feature spanning 2﹩\mathop{.}\limits{^{\prime\prime} }﹩822 horizontally and 2﹩\mathop{.}\limits{^{\prime\prime} }﹩158 vertically (red rectangle). (b) A blowup of this rectangle in a sequence of images, with LOS magnetic field values saturated at ±100 G. (c) AIA 304 Å sequence of images coaligned with the NIRIS FOV in (a). The chromospheric brightening associated with the apparent cancellation is indicated by red circles.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Time series of (a) the negative- (blue curve) and positive- (red curve) polarity magnetic flux in the 222 Hinode SOT/NFI magnetograms tested and (b) the virial magnetic energy (Equation (3); red curve), the surface-integral potential energy of this work (Equation (1); black curve), and 12 volume energies obtained nominally by means of a full-fledged potential field extrapolation (green diamonds). For the virial and surface-integral energies, applicable uncertainties are also included. Each virial energy is the mean of 100 random realizations of the vector position r, with uncertainties realized as the standard deviation of each set of estimates.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Variations of (a) the potential magnetic energy and (b) the flux of both polarities for the event of Figure 5. The flux decrease for both polarities (dark red in (b)) signifies the energy-loss rate (dark red in (a)) and subsequent lower limit of energy released during the event.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: (a) LOS Hinode SOT/NFI magnetogram of NOAA AR 10930 acquired at about midday on 2006 December 11. (b) The respective surface density of the potential magnetic energy, as obtained by the integrand of Equation (1). Minor tick-mark separation in both images is 5″. Integrating these densities over the FOV, we obtain a potential energy of ∼(3.24 ± 0.07) × 1032 erg.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Scaling between Ep and Φ for 100,000 randomly chosen sub-FOV magnetogram areas for NIRIS (light red dots) and HMI (light blue dots). The scaling for the full FOVs is also shown (red squares for NIRIS; blue squares for HMI). Curves correspond to the least-squares power-law best fits (red for NIRIS; blue for HMI).
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Random selection of 100,000 subparts of the FOV from 222 SOT/NFI magnetograms and the correlation between their unsigned magnetic flux and respective potential magnetic energies (light red dots). A power-law best fit (curve) is also shown. Further shown are the respective calculations for all 222 frames and their full FOV (green squares).
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: The first NIRIS magnetogram in our time series with four indicated features, namely, the main network feature and features 1–3. Each of these subfields has equal dimensions of 11﹩\mathop{.}\limits{^{\prime\prime} }﹩039 (short side) by 27﹩\mathop{.}\limits{^{\prime\prime} }﹩971 (long side).
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Specific energy-loss rates when both polarity fluxes decrease for the NIRIS magnetograms (red histogram) and the HMI magnetograms (blue histogram). Dashed lines denote averages of energy-loss rates (∼7.2 × 1025 erg s−1 for the NIRIS data; ∼2 × 1025 erg s−1 for the HMI data).
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Histogram of surface density values of the potential energy as shown in Figure 8. The green shaded part of the histogram corresponds to nominal positive values, whereas the red shaded one corresponds to spurious negative values.