adsabs/AstroCLIMB huggingface dataset:
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: For NGC 3081 (top panels) and NGC 5506 (bottom panels), the left column presents the normalized [Ne II]12.814μm flux distribution, the center column presents the [Ne V]14.322μm flux distribution (line maps have been normalized by the maximum flux value for each respective map), and the right column presents the spatial distribution of the observed [Ne II]12.814μm/[Ne V]14.322μm flux ratio. To address differences in the PSF, the [Ne II]12.814μm emission map has been convolved with the FWHM of the PSF of the [Ne V]14.322μm line prior to computing the flux ratio map. The dotted black lines indicate the edges of the ionization bicone, PA = 165°, ΩOut = 30° and PA = 22°, ΩOut = 80° for NGC 3081 and NGC 5506, respectively.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Thermal mapping for NGC 3081 (left panel) and NGC 5506 (right panel) generated from the H2 0–0 S(1)/S(5) line ratio. To address differences in PSF, the S(5) emission maps have been convolved with the FWHM of the broader PSF of the S(1) line prior to computing excitation maps. Black and white contours outline the [Ne V]14.322μm and [Fe II]5.34μm emission, respectively. The dotted black lines indicate the edges of the ionization bicone, PA = 165°, ΩOut = 30° and PA = 22°, ΩOut = 80° for NGC 3081 and NGC 5506, respectively. For NGC 3081, the [Fe II]5.34μm intensity contours range from 10−7.25 to 10−6.25 Jy (in 0.5 dex steps) and the [Ne V]14.322μm intensity contours range from 10−5.0 to 10−4.0 Jy (in 0.5 dex steps). For NGC 5506, the [Fe II]5.34μm intensity contours range from 10−5.75 to 10−5.0 Jy (in 0.25 dex steps) and the [Ne V]14.322μm intensity contours range from from 10−4.8 to 10−3.8 Jy (in 0.5 dex steps).
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: The top-left panel depicts the NGC 3081 H2 0–0 S(5) normalized line flux and apertures utilized for analysis. The bottom panel depicts the integrated spectra for the associated apertures. The top-right panel presents the estimated population levels for each of the associated eight MIR rotational H2 emission lines and the LTE best fit for each aperture of interest.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: The top-left panel depicts the NGC 5506 H2 0–0 S(5) normalized line flux and apertures utilized for analysis. The bottom panel depicts the integrated spectra for the associated apertures. Integrated spectra for the rotational disk regions are not displayed as the continuum level is significantly lower than in other apertures. The top-right panel depicts the estimated population levels for each of the associated eight MIR rotational H2 emission lines and the LTE best fit for each aperture of interest.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Radial LTE analysis for the ionization bicone of NGC 3081. The left panel presents the wide-slit aperture encompassing the [Ne V]14.322μm emission. The black outline highlights an example integration aperture for the LTE modeling. The top-right panel presents the best value of the thermal scaling parameter β as a function of radial distance. The bottom-right panel presents the LTE model best-fit log[﹩{N}_{{{\rm{H}}}_{2}}﹩/cm−2] as a function of radial distance from the nucleus. Shaded gray regions indicate the standard error of the LTE fit parameters.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Emission-line fits for the H2 0–0 S(1) through S(5) two-component Gaussian fits for the entrained aperture in NGC 5506 are displayed in the left panels. The red line indicates the Gaussian fit to the rotational component and the blue line highlights the fit for the nonrotational component. The right panel presents the NGC 5506 estimated population levels for the seven detected MIR rotational H2 emission lines (we report S(8) as an upper limit) and the LTE best fit for the individual rotational and nonrotational fit components within the entrained aperture.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Comparison of the synthetic multiband light curves (F · d2, with F being the flux at reference distance d) for different orbital inclinations (θinc) and viewing angles relative to the initial AGN disk plane (αLoS). Time is measured from the first pericenter passage (t0 ≈ 0.73 days). Each column corresponds to an orbital inclination of θinc = 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, 45°, 90°, and 135°, from left to right. Each row is for a certain energy band: 1–10 eV (top), 80–120 eV (middle), and 0.2–0.4 keV (bottom), corresponding to the UV/optical, EUV, and soft X-ray bands, respectively. In each panel, different viewing angles (αLoS) are color-coded, as indicated in the top panel of each column.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Synthetic light curves exhibiting a two-phase structure: a precursor flare, associated with the process of debris tearing through the AGN accretion disk, followed by a major flare powered by the fallback of debris. Time is measured from the first pericenter passage (t0 ≈ 0.73 days). The onset of the fallback phase, marking the transition between the two flares, is indicated by a red vertical line in each panel. All panels present a face-on view of the system. Each row corresponds to a different orbital inclination angle, θinc = 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, 45°, 90°, and 135°, from top to bottom. The left column displays the bolometric luminosity (F · d2, where F is the flux at an arbitrary reference distance d), while the right column shows its band-integrated components in three energy ranges: 2–7 eV (green), 7–12 eV (gray), and 40–50 eV (purple), corresponding to the NUV/optical, FUV, and EUV bands, respectively.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Time evolution of angular momentum and inflow rate for the stellar debris and the AGN disk, for models with orbital inclinations θinc = 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, 45°, 90°, and 135° from (a)–(d). The top three rows show the angular momentum, normalized by the disk’s initial angular momentum (Ldisk,init). From top to bottom are the z-component (Lz), y-component (Ly), and ﹩L=\sqrt{{L}_{x}^{2}+{L}_{y}^{2}+{L}_{z}^{2}}﹩ with Lx denoting the x-component. Angular-momentum components of the stellar debris (red, left axis) and the disk (blue, right axis) are shown, with a dynamically adjusted and a fixed plotting range, respectively. The bottom row shows the inflow rate as a function of time, with the total inflow rate (﹩{\dot{M}}_{{\rm{total}}}﹩), stellar debris contribution (﹩{\dot{M}}_{{\rm{debris}}}﹩), and disk contribution (﹩{\dot{M}}_{{\rm{disk}}}﹩) plotted in black, red, and blue, respectively.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Time evolution of the radial surface density profiles for models with stellar orbital inclinations of 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, 45°, 90°, and 135°. The plot range is limited to the inner region (R < 103Rg). The total surface density, AGN disk contribution, and stellar debris contribution are shown by the solid gray, solid black, and dashed–dotted black lines, respectively. The pericenter distance as well as the impact radius (Rp) is indicated by dashed red vertical lines. The corresponding time for each panel is labeled in the upper-left corner.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Comparison of the column density distributions of the inner disk under Newtonian gravity (left panels) and Schwarzschild metric (right panels), color-coded on a logarithmic scale. Panel (a) shows the case of θinc = 45°, viewed face-on relative to the initial AGN disk plane, and panel (b) shows the case of θinc = 90°, viewed from an arbitrary inclined angle to better reveal the formation of a tilted inner disk. For each case, the bottom row displays the projected column density in the y–z plane, providing an edge-on view of the inner disk structure. The time since the start of the simulation is marked in each panel, and a scale bar of 103Rg is shown for reference.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Face-on views of the evolution of the log-scaled column density of the inner region (R < 103Rg) of the disk for models with θinc = 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, 45°, 90°, and 135°. The 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 45° models develop a central cavity and prominent spiral arms, while the 90° and 135° models form a gradually tilting inner disk. The time since the start of the simulation for each snapshot is labeled on the top right of each row.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Edge-on views illustrating the debris under Newtonian gravity (blue) and Schwarzschild metric (red) at t = 1.98 days, 4.9 days, 16.6 days and 34 days. Panels (a) and (b) correspond to stellar orbital inclinations θinc = 45° and θinc = 90°, respectively, relative to the AGN disk plane. In the Schwarzschild metric, relativistic apsidal precession causes the debris to leave the disk earlier, resulting in a shorter duration of debris–disk interaction than Newtonian cases.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Snapshots of the central cavity for model R45. In each panel, the red curve outlines the cavity edge, the gray dot indicates the central SMBH, and the gray arrow denotes the direction of the cavity’s major axis. The time since the beginning of the simulation is labeled in each panel. A scale bar of 200Rg is shown in the bottom left of the plot.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Hα line width vs. luminosity for solar and stellar flares. (a) Flares on young solar-type stars, marked by flare type: WLFs with red circles, non-WLFs with blue triangles, and flares without TESS data with black crosses. Values are from the peak time of line broadening. (b) Time evolution for EK3 (green squares), EK4 (orange circles), and V3 (black crosses). Each colored line shows a power-law fit for the event. (c) Time evolution of an M4.2-class solar flare from the Sun-as-a-star analysis by K. Namekata et al. (2022a). The dashed line shows a power-law fit for the event. (d) Comparison of solar and stellar data. The symbols are the same as panels (a) and (c). All data are fitted with a single power-law relation as indicated with the dashed line.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: The flare catalog. Each panel displays a typical preflare-subtracted Hα line spectrum for the superflare events EK1-12 and V1-3, as labeled in each panel. The black solid lines correspond to the observed spectrum, highlighting the most prominent time for each flare. The gray thick lines represent the Gaussian fits to the observed spectra. For events exhibiting significant blue/redshifts at velocities exceeding 50 km s−1, the fitted Gaussians are shown in blue (EK6) or red (EK12), respectively. EK7 is fitted with two Gaussian components as described by K. Namekata et al. (2024a). For EK2 and EK9, where postflare blueshifted absorption components appear, these spectra are plotted in blue. The velocity and FWHM from fitting the Gaussian to the flare Hα central wavelength radiation are indicated in the top right of each panel. Additionally, as an indicator of broadening, a Gaussian with a standard deviation of 2.5 Å (FWHM of 5.9 Å), which is comparable with a typical Hα line width with our spectrograph (see Section 3.2.3), is plotted in shaded gray.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Relationship between Hα flare energy and FWHM duration. (a) Red triangles indicate events with red asymmetry. Blue squares show events with blueshifted absorption or emission (filament/prominence eruptions). Black circles are events with line broadening but no asymmetry. Black crosses show no asymmetry or broadening. (b) Orange circles are WLF events. Green squares are non-WLF events. Black crosses are events without simultaneous TESS observations.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK12 on 2024 April 19. The initial bump observed around 0–30 minutes falls below the detection threshold (ΔEW > 0.1) and is therefore not considered significant. Consequently, the subsequent bump at around 100–200 minutes is treated as the primary superflare. Note that after approximately t = 260 minutes, the weather conditions began to be worse, and around t = 420 minutes, a slight bump is visible. However, this coincides with another period of poor data quality, and thus we conservatively excluded it as a flare candidate. These exclusions, however, do not significantly affect the estimated flare/CME occurrence rate.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Time evolution of the filament eruption from flare event EK9. (a) Zoom-in view of the dynamic Hα spectrum. The dotted line is the Hα line center wavelength. (b) Absorption velocity over time (blue squares). The green line shows an exponential fit and the magenta line shows the freefall velocity evolution.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event V3 on 2023 March 31.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event EK11 on 2024 March 29.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event V1 on 2021 April 24.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Same as Figure 1, but for the flare event V2 on 2022 July 25.
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Mass and kinetic energy of solar and stellar filament/prominence eruptions and CMEs as a function of bolometric WLF energy or GOES X-ray energy. The dark green symbols (circle and downward-pointing triangles) and red/blue squares show stellar prominence and filament eruptions on EK Dra, respectively. Black crosses represent solar CME data (S. Yashiro & N. Gopalswamy 2009; J. J. Drake et al. 2013), and lime green pluses show solar filament/prominence eruptions (see, K. Namekata et al. 2022c; Y. Kotani et al. 2023). The large error bars on the two lime green data points in panel (a) are taken from the original sources by R. Jain & B. Sorathia (1987) and D. J. Christian et al. (2015), whereas error estimates for the other data points were not provided in the publications (M. Ohyama & K. Shibata 1999; Y. Liu & H. Kurokawa 2004; K. Namekata et al. 2022c; Y. Kotani et al. 2023); therefore, these two error bars do not necessarily represent the typical uncertainties. Note also that the data in panels (a) and (b) are not in a one-to-one correspondence. The cyan dashed and magenta dotted lines are observational fits for solar CMEs: ﹩{M}_{{\rm{CME}}}\propto {E}_{{\rm{bol}}}^{0.59}﹩ and ﹩{E}_{{\rm{kin}}}\propto {E}_{{\rm{bol}}}^{1.05}﹩ (cyan; J. J. Drake et al. 2013), and ﹩{M}_{{\rm{CME}}}\propto {E}_{{\rm{bol}}}^{0.7}﹩ (magenta; A. N. Aarnio et al. 2012). Gray lines in the right panel indicate Ekin = Ebol, Ebol/10, and Ebol/100. GOES X-ray energy/flux is converted to bolometric energy using Ebol = 100, EGOES (A. G. Emslie et al. 2012) and Ebol, [erg] = 1035, FGOES, [W, m−2] (K. Shibata et al. 2013). Bolometric energy is assumed to be approximately equal to bolometric WLF energy (M. Kretzschmar et al. 2010; M. Kretzschmar 2011; R. A. Osten & S. J. Wolk 2015).
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Filament/prominence eruption velocity vs. flare energy, shown as GOES flux (bottom axis) or bolometric WLF energy (top axis). The dark green symbols (circle and downward-pointing triangles) and red/blue squares show stellar prominence and filament eruptions on EK Dra, respectively. Solar filament eruption data (lime green pluses) are from D. Seki et al. (2021), and data for M dwarfs, RS CVn, and young stellar objects (black circles) are from the list in K. Namekata et al. (2024a). The cyan solid line shows a power-law fit to all solar and stellar data. The black dashed line represents a power law with index 1/6, tracing the upper limit of the data (T. Takahashi et al. 2016).
Paper: Do Young Suns Produce Frequent, Massive CMEs? Results from Five-year Dedicated Optical Observations of EK Draconis and V889 Hercules
Authors: Kosuke Namekata, Hiroyuki Maehara, Yuta Notsu, Satoshi Honda, Kai Ikuta, Daisaku Nogami, Kazunari Shibata
Figure caption: Detection probability of blueshifted absorption as a function of initial velocity of erupted filament. The assumptions we made are described in Section 5.6. The crosses and circles indicate the probabilities that the events can be observed in absorption for more than 5 and 10 minutes, respectively.