adsabs/AstroCLIMB huggingface dataset:
Paper: A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned 
Authors: Emma M. Louden, Songhu Wang, Joshua N. Winn, Erik A. Petigura, Howard Isaacson, Luke Handley, Samuel W. Yee, Corey Beard, Joseph M. Akana Murphy, Gregory Laughlin
Figure caption: Comparison between the properties of the control stars (navy) and the planet hosts (magenta) of both the 2021 (crosses) and 2022 (dots) data. The precision of the measurements is 60 K in T eff, 0.10 dex in ﹩\mathrm{log}g﹩, 0.04 dex in [Fe/H], and 1.0 km s−1 in ﹩v\sin i﹩. The ages are determined by isoclassify using the MIST isochrones and have a typical precision of 30%.
Paper: A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned 
Authors: Emma M. Louden, Songhu Wang, Joshua N. Winn, Erik A. Petigura, Howard Isaacson, Luke Handley, Samuel W. Yee, Corey Beard, Joseph M. Akana Murphy, Gregory Laughlin
Figure caption: Planetary geometry. The angle Ψ is the full stellar obliquity. The angle i 0 is the inclination between the planet’s orbital axis and the observer’s line of sight. This is near 90° for transiting planets. i is the star’s inclination.
Paper: A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned 
Authors: Emma M. Louden, Songhu Wang, Joshua N. Winn, Erik A. Petigura, Howard Isaacson, Luke Handley, Samuel W. Yee, Corey Beard, Joseph M. Akana Murphy, Gregory Laughlin
Figure caption: Target list created using rejection sampling. The striation is caused by using TESS exoFOP temperatures that are assigned. The stars span a temperature range of 6100–7100 K.
Paper: A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned 
Authors: Emma M. Louden, Songhu Wang, Joshua N. Winn, Erik A. Petigura, Howard Isaacson, Luke Handley, Samuel W. Yee, Corey Beard, Joseph M. Akana Murphy, Gregory Laughlin
Figure caption: Observational sample in the context of TESS Objects of Interest (TOIs). The planet-hosting and control stars sample are compared to the TOI catalog. The striation is caused by using TESS exoFOP temperatures that are assigned. The stars span a temperature range of 6100–7100 K.
Paper: A Larger Sample Confirms Small Planets around Hot Stars Are Misaligned 
Authors: Emma M. Louden, Songhu Wang, Joshua N. Winn, Erik A. Petigura, Howard Isaacson, Luke Handley, Samuel W. Yee, Corey Beard, Joseph M. Akana Murphy, Gregory Laughlin
Figure caption: Comparison of the 2021 and 2022 samples in effective temperature, Gaia G magnitude, and stellar radius. The striations result from the exoFOP catalog used to make the observational target list.
Paper: A Novel Model for the MeV Emission Line in GRB 221009A
Authors: Yu-Jia Wei, 煜佳 魏, Jia Ren, 佳 任, Hao-Ning He, 昊宁 贺, Yuan-Pei Yang, 元培 杨, Da-Ming Wei, 大明 韦, Zi-Gao Dai, 子高 戴, B. Theodore Zhang, 兵 张
Figure caption: Panel (a): the value of M  i  contributing to the emission line at each time interval with T = 3000 K (the blue points), T = 9000 K (the orange points), and T = 2 × 104 K (the red points). The coefficient in the caption means the scaling of M  i . The other parameters we used are d = 8.6 × 1011 cm and θ  j  = 0.02 rad. Panel (b): the lower limit of M  i,tot for T = 104 K with different γ for d = 8.6 × 1011 cm (the orange triangles) corresponding to Δt gap = 33 s and d = 2.5 × 1012 cm (the red triangles) corresponding to Δt gap = 97 s. We also show the results with d = 1015 cm (the blue triangles) due to the uncertainty of the beginning time.
Paper: A Novel Model for the MeV Emission Line in GRB 221009A
Authors: Yu-Jia Wei, 煜佳 魏, Jia Ren, 佳 任, Hao-Ning He, 昊宁 贺, Yuan-Pei Yang, 元培 杨, Da-Ming Wei, 大明 韦, Zi-Gao Dai, 子高 戴, B. Theodore Zhang, 兵 张
Figure caption: Panel (a): a schematic model for scattering the photons from the progenitor. The region that generates the emission line can have almost isotropic seed photons from the reflection of the cold cloud shell since the clouds might be destroyed by the jet only within a small solid angle ∼θ 2/2. Panel (b): the specific energy density for the radiation of the W-R star (red line) and Compton reflection (blue line) at d sc = 1015 cm with ΔΩ = 1 sr. The temperature of the incident photons is T = 1.5 × 104 K.
Paper: A Novel Model for the MeV Emission Line in GRB 221009A
Authors: Yu-Jia Wei, 煜佳 魏, Jia Ren, 佳 任, Hao-Ning He, 昊宁 贺, Yuan-Pei Yang, 元培 杨, Da-Ming Wei, 大明 韦, Zi-Gao Dai, 子高 戴, B. Theodore Zhang, 兵 张
Figure caption: A schematic picture of the generation of the MeV emission line. The mass-dominated jet head (the jet without heavy nuclei) could not carry heavy nuclei due to its high temperature, which corresponds to effective photodisintegration and spallation. Once the jet becomes Poynting-dominated, it can entrain heavy nuclei. After the jet with heavy nuclei breaks through the photosphere and hydrogen-like heavy ions are generated by β decay and/or recombination, the emission line can be generated at R emit. Around this point, the jet head reaches the dissipation radius R diss, generating the prompt emission. When the jet with heavy nuclei arrives at R diss, it can not generate the emission line due to band broadening and/or spallation, leading to the disappearance of the emission line in the end.
Paper: A Novel Model for the MeV Emission Line in GRB 221009A
Authors: Yu-Jia Wei, 煜佳 魏, Jia Ren, 佳 任, Hao-Ning He, 昊宁 贺, Yuan-Pei Yang, 元培 杨, Da-Ming Wei, 大明 韦, Zi-Gao Dai, 子高 戴, B. Theodore Zhang, 兵 张
Figure caption: The parameter space in the γ–T plane with the color indicating the isotropic luminosity with θ  j  = 0.01 rad and N  i  = 1042 counts. Blank areas indicate that this part of the parameter space can not generate emission lines. We use d = 1012 cm (1014 cm) in the left (right) panels, which mainly affects the size of the parameter space but not the luminosity. We use Z = 10, 20, 30, and 40 in Figures 4(a)–(h), which affects both the parameter space and the luminosity.
Paper: NICER Discovery that SRGA J144459.2–604207 Is an Accreting Millisecond X-Ray Pulsar
Authors: Mason Ng, Paul S. Ray, Andrea Sanna, Tod E. Strohmayer, Alessandro Papitto, Giulia Illiano, Arianna C. Albayati, Diego Altamirano, Tuğba Boztepe, Tolga Güver, Deepto Chakrabarty, Zaven Arzoumanian, D. J. K. Buisson, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Jeremy Hare, Gaurava K. Jaisawal, Christian Malacaria, Michael T. Wolff
Figure caption: Evolution of the second blackbody component during the type I X-ray burst from time-resolved spectroscopy. (a) bolometric (0.1–100.0 keV) unabsorbed flux in units of 10−8 erg s−1 cm−2; (b) blackbody temperature, kT (keV); (c) blackbody normalization, normbb scaled by ﹩{({R}_{\mathrm{km}}/{D}_{10})}^{2};﹩ (d) reduced χ 2 for the fit. The cooling blackbody, the key signature of the thermonuclear nature of the burst, is evident. The offset, t  i , corresponds to MJD 60362.35047 (TT units at NICER).
Paper: NICER Discovery that SRGA J144459.2–604207 Is an Accreting Millisecond X-Ray Pulsar
Authors: Mason Ng, Paul S. Ray, Andrea Sanna, Tod E. Strohmayer, Alessandro Papitto, Giulia Illiano, Arianna C. Albayati, Diego Altamirano, Tuğba Boztepe, Tolga Güver, Deepto Chakrabarty, Zaven Arzoumanian, D. J. K. Buisson, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Jeremy Hare, Gaurava K. Jaisawal, Christian Malacaria, Michael T. Wolff
Figure caption: (a) SRGA J144459.2−604207 monitoring 2–10 keV light curve by MAXI/GSC (Mihara et al. 2024). The shaded gray region corresponds to the NICER observation interval. (b) NICER 0.3–12.0 keV light curve with 4 s bins. The burst emission was removed, but instead the midpoint of the burst interval (including the preburst) is shown with the red arrow. (c) The pulse arrival time delay as a function of the orbital phase, with the best-fit orbit shown with the dashed lines, and the pulse timing residuals shown in squares (with scale on the right y-axis). (d) Folded 1.0–10.0 keV pulse profile with the NICER observations. The profile also shows a significant second harmonic. There are 20 pulse phase bins and two cycles are plotted for clarity.
Paper: NICER Discovery that SRGA J144459.2–604207 Is an Accreting Millisecond X-Ray Pulsar
Authors: Mason Ng, Paul S. Ray, Andrea Sanna, Tod E. Strohmayer, Alessandro Papitto, Giulia Illiano, Arianna C. Albayati, Diego Altamirano, Tuğba Boztepe, Tolga Güver, Deepto Chakrabarty, Zaven Arzoumanian, D. J. K. Buisson, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Jeremy Hare, Gaurava K. Jaisawal, Christian Malacaria, Michael T. Wolff
Figure caption: Phenomenological fit to the light curve of the type I X-ray burst in the NICER ObsID 6204190102 with a simple FRED model and a model with a FRED component and a plateau. (a) Light curve of the type I X-ray burst, with 0.5 s bins, with the FRED + plateau model shown in the solid red line; (b) residuals from fitting the burst light curve to a simple FRED model; (c) residuals from a FRED + plateau model. While the fit with the FRED model is formally acceptable (χ 2/dof = 1.08;  318 dof), the fit with the hybrid FRED and plateau model is significantly better at the 1.4 × 10−11 level, and the systematic residuals around the plateau are minimized. The elapsed time of 0 corresponds to MJD 60362.35007 (TT units at NICER).
Paper: NICER Discovery that SRGA J144459.2–604207 Is an Accreting Millisecond X-Ray Pulsar
Authors: Mason Ng, Paul S. Ray, Andrea Sanna, Tod E. Strohmayer, Alessandro Papitto, Giulia Illiano, Arianna C. Albayati, Diego Altamirano, Tuğba Boztepe, Tolga Güver, Deepto Chakrabarty, Zaven Arzoumanian, D. J. K. Buisson, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Jeremy Hare, Gaurava K. Jaisawal, Christian Malacaria, Michael T. Wolff
Figure caption: Top: donor mass (M  d , M ⊙) as a function of the binary inclination, i, for M ns = 1.4 M ⊙; ﹩1-\cos \,i﹩ is the a priori cumulative distribution function of observed binary inclinations. Bottom: donor radius (R  d , R ⊙) as a function of the donor mass for SRGA J144459.2−604207 (black solid line), zero-age main-sequence stars (orange solid line; Tout et al. 1996), and hot (red) and cold (blue) WDs of varying compositions (Deloye & Bildsten 2003). The most viable donor for SRGA J144459.2−604207 is a main-sequence star (which may be slightly bloated).
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption: Integrated 12CO intensity images and flux–intensity relations of two single-exponential molecular clouds. See Table 1 for detailed parameters of the two molecular clouds. For added clarity on exponential properties, plots in logarithmic scale are also displayed, where the constant c in Equation (1) has been subtracted.
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption: Integrated 12CO intensity images and segmented flux–intensity relations of three double-exponential clouds. The red contour delineates the edge of the second exponential component (integrated from T break to peak). See Table 1 for detailed parameters of molecular clouds and see Equation (2) for the definition of the piecewise function. For added clarity on exponential properties, plots in logarithmic scale are also displayed, where the constant c in Equation (2) has been subtracted from the first segment, and to maintain the continuity of the plots, a shift in logarithmic scale (by multiplying a factor) is applied to the first segment.
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption: Distribution of the peak intensity, the angular area, α, α 1, α 2, T break, and ﹩{F}_{\exp 2}/{F}_{\mathrm{total}}﹩ of single- and double-exponential molecular clouds. For comparison, the distribution of the steepness (α 3) of the third segment of triple-exponential 12CO flux–intensity relations is also plotted in panel (d).
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption: Relationships between parameters of the flux–intensity relation and cloud properties. 〈T〉 is the mean brightness temperature of 12CO across all voxels. F total is the total flux of 12CO emission, and ﹩{F}_{\exp 2}﹩ is the flux of the second exponential component.
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption: Correlation between the flux of the second exponential component, ﹩{F}_{\exp 2}﹩, and the total observed flux for 12CO (blue; 10,367 clouds), 13CO (green; 4602 clouds), and C18O (red; 66 clouds). Envelopes of line emission are defined using data cubes and the DBSCAN algorithm.
Paper: On the Flux–Intensity Relation of Molecular Clouds
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Chen Wang, Yiping Ao, Xuepeng Chen, Min Wang
Figure caption:  T break contours on integrated intensity images of 13CO. The T break contour is exactly the same as that in Figure 2, and see Figure 2 also for 12CO images and flux–intensity relations of these three clouds.
Paper: Connecting Solar Wind Velocity Spikes Measured by Solar Orbiter and Coronal Brightenings Observed by SDO
Authors: Chuanpeng Hou, Alexis P. Rouillard, Jiansen He, Bahaeddine Gannouni, Victor Réville, Philippe Louarn, Andrey Fedorov, Lubomír Přech, Christopher J. Owen, Daniel Verscharen, Raffaella D'Amicis, Luca Sorriso-Valvo, Naïs Fargette, Jesse Coburn, Vincent Génot, Jim M. Raines, Roberto Bruno, Stefano Livi, Benoit Lavraud, Nicolas André, Gabriel Fruit, Rungployphan Kieokaew, Illya Plotnikov, Emmanuel Penou, Alain Barthe, Dhiren Kataria, Matthieu Berthomier, Frederic Allegrini, Vito Fortunato, Gennaro Mele, Timothy Horbury
Figure caption: (a) The radial component of the magnetic field measured by Solar Orbiter. (b) The radial solar wind speed measured by Solar Orbiter. The red curves identified visually mark the patches of spikes. The green shaded interval indicates when the solar footpoints of the solar wind are concentrated and remain within the visible disk from Earth. (c) The correlation coefficient between the N component of the magnetic field and the solar wind velocity in the RTN coordinate system. (d) ﹩\tfrac{{O}^{7+}}{{O}^{6+}}﹩ measured by Solar Orbiter/SWA-HIS. (e) The radial magnetic field during the interval marked with a green shaded area. (f) The radial solar wind speed during the same interval. (g) Wavelet transform power 2D-spectrum of the radial solar wind speed in (f). The black crossed area marks the parameter space outside the confidence level of 95%. (h) The global average of the power spectrum (black solid line) with a peak at a period of 7.5 hr.
Paper: Connecting Solar Wind Velocity Spikes Measured by Solar Orbiter and Coronal Brightenings Observed by SDO
Authors: Chuanpeng Hou, Alexis P. Rouillard, Jiansen He, Bahaeddine Gannouni, Victor Réville, Philippe Louarn, Andrey Fedorov, Lubomír Přech, Christopher J. Owen, Daniel Verscharen, Raffaella D'Amicis, Luca Sorriso-Valvo, Naïs Fargette, Jesse Coburn, Vincent Génot, Jim M. Raines, Roberto Bruno, Stefano Livi, Benoit Lavraud, Nicolas André, Gabriel Fruit, Rungployphan Kieokaew, Illya Plotnikov, Emmanuel Penou, Alain Barthe, Dhiren Kataria, Matthieu Berthomier, Frederic Allegrini, Vito Fortunato, Gennaro Mele, Timothy Horbury
Figure caption: (a) The time series of the number of identified CBs. (b) The wavelet transform power 2D-spectrum of the time series in (a). The black crossed area marks the parameter space outside the confidence level of 95%. (c) The time average power spectrum, fast Fourier transform (fft) power, red noise spectrum, and 95% confidence level. (d)–(f) The same format as (a)–(c) but for the time series of total magnetic flux on the solar surface.
Paper: Connecting Solar Wind Velocity Spikes Measured by Solar Orbiter and Coronal Brightenings Observed by SDO
Authors: Chuanpeng Hou, Alexis P. Rouillard, Jiansen He, Bahaeddine Gannouni, Victor Réville, Philippe Louarn, Andrey Fedorov, Lubomír Přech, Christopher J. Owen, Daniel Verscharen, Raffaella D'Amicis, Luca Sorriso-Valvo, Naïs Fargette, Jesse Coburn, Vincent Génot, Jim M. Raines, Roberto Bruno, Stefano Livi, Benoit Lavraud, Nicolas André, Gabriel Fruit, Rungployphan Kieokaew, Illya Plotnikov, Emmanuel Penou, Alain Barthe, Dhiren Kataria, Matthieu Berthomier, Frederic Allegrini, Vito Fortunato, Gennaro Mele, Timothy Horbury
Figure caption: Our scenario about the formation of velocity spikes. The closed magnetic loop caused by flux emergence, cancellation, or shearing motions reconnects with surrounding open field lines. During the reconnection processes, the accumulated magnetic energy is released to heat the surrounding plasma, and the increasing brightness becomes visible as a CB. Waves and jets are triggered as seeds of the switchbacks and velocity spikes measured by Solar Orbiter.
Paper: Connecting Solar Wind Velocity Spikes Measured by Solar Orbiter and Coronal Brightenings Observed by SDO
Authors: Chuanpeng Hou, Alexis P. Rouillard, Jiansen He, Bahaeddine Gannouni, Victor Réville, Philippe Louarn, Andrey Fedorov, Lubomír Přech, Christopher J. Owen, Daniel Verscharen, Raffaella D'Amicis, Luca Sorriso-Valvo, Naïs Fargette, Jesse Coburn, Vincent Génot, Jim M. Raines, Roberto Bruno, Stefano Livi, Benoit Lavraud, Nicolas André, Gabriel Fruit, Rungployphan Kieokaew, Illya Plotnikov, Emmanuel Penou, Alain Barthe, Dhiren Kataria, Matthieu Berthomier, Frederic Allegrini, Vito Fortunato, Gennaro Mele, Timothy Horbury
Figure caption: (a) Animation of the proposed scenario that connects CBs with the in situ measurements by Solar Orbiter. (b)–(d) The same format as Figures 3(a)–(c) but for the time series of the number of CBs connecting with Solar Orbiter.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: A time sequence of the highest-resolution simulation (SMR5-SP99) with BH spin a = 0.99. We show square slices of the xz-plane (side-on view) of six quantities. The rows show the comoving plasma magnetization σ co, the plasma beta β, the dimensionless temperature Θ, the Lorentz factor Γ, the radial magnetic field component times the square of the radial distance B  r  r 2 (to account for the scaling of the monopolar field), and the radial 4-velocity u  r . The six columns show for three different times t = (45, 111, 270) r g/c (all taken in the same phase of rotation), on the left a zoomed-out view and on the right a zoomed-in view. The zoomed-out views cover a larger distance for later times, as shown by the values on the axes at the bottom of the figures. In the panels, the black circle is the BH, the white dashed line is the ergosphere, and the white dotted line is the inner light surface. In the second row, the white dashed–dotted lines show the envelope of the event horizon current sheet inclination if it would radially propagate at the speed of light. In the fourth row, the black arrowed lines represent the 3-velocity streamlines. In the fifth row, the black arrowed lines represent magnetic field lines.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: The time evolution of the current sheet inclination angle χ on the event horizon (top panel) and the total event horizon magnetic flux Φ∣B∣ of ∣B  r ∣ normalized to its initial value (bottom panel) for BH spins a = (0.5, 0.8, 0.9, 0.99). Next to the simulations with χ 0 = 30° for all spins, we also included the simulations with χ 0 = 20° and χ 0 = 0° with spin a = 0.99, where the latter is not shown in the top panel as there is no alignment angle evolution. Colored solid lines are measured from the simulations, and the matching colored dashed lines are exponential fits. The top panel shows that the inclination angle decreases at an exponential rate, with timescale dependent on the BH spin, where higher spin results in faster alignment. The simulation with χ 0 = 20° aligns at an equal rate to the χ 0 = 30° case, making the alignment timescale independent of χ 0. The bottom panel shows that for all spins and all χ 0, the magnetic flux decays on a similar exponential timescale τ Φ ∼ 2 · 102 r g/c.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: A time sequence identical to Figure 1 of the xy-plane (top-down view). Everything is the same as in Figure 1 except that the panels in the y-direction are off-center from y = 0 to better illustrate the spherical structure of the magnetosphere in the equatorial plane.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Exponential alignment timescales τ  χ  for all considered dimensionless BH spins a = (0.5, 0.8, 0.9, 0.99) as a function of the BH angular velocity ΩH. The fit (dashed line) shows that the alignment timescale is inversely proportional to the square of the BH angular velocity.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: The period P, alignment timescale τ  χ , and decay timescale τ Φ as a function of BH angular velocity ΩH. The colored thick lines are associated with the left vertical axis showing the dimensionless timescales. The colored shaded regions are associated with the right vertical axis showing the timescales in milliseconds restricted by the possible BH masses 2.0 ≲ M/M ⊙ ≲ 4.8 formed from NS–NS mergers.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: An example of the general shape of an emitting striped wind current sheet described by its inclination angle ﹩\tilde{\chi }﹩ (dashed lines) for a fixed azimuth with a shrinking envelope (dashed–dotted line) described by the current sheet inclination angle χ. A fixed observer at χ obs (dotted line) may receive emission in the form of timed pulses (red crosses) if ﹩\tilde{\chi }﹩ matches with χ obs. The current sheet inclination angle ﹩\chi ^{\prime} ﹩ (black dots) measured by the maximum current density along the θ-direction at r = 5r g at a fixed azimuth ϕ 0 (from simulation SMR5-SP99) shows variability with respect to the general striped wind motion due to the local corrugated motion of the current sheet and goes slightly out of phase due to ΩF not being exactly ΩH/2.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: A snapshot of the xz-plane in a side-on view of the highest-resolution simulation, SMR5-SP99, showing an SMR structure. The wedge-shaped SMR structure has a half-opening angle of 45° around the equatorial region and is displayed by grid lines representing the computational blocks. The computational blocks contain 20, 8, and 20 computational cells in, respectively, the r, θ, and ϕ coordinate directions. The color scale shows the plasma beta, which, inside the current sheet β, is higher than in the surrounding region. The current sheet moves inside the SMR wedge at all times, thereby ensuring that the highest resolution is imposed on the current sheet.
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Time evolution of the measured electromagnetic radial energy flux ﹩{\dot{E}}_{{\rm{EM}}}﹩ over the event horizon and the corresponding instantaneous Blandford–Znajek power scaling P BZ6 for all four simulated spins a = (0.5, 0.8, 0.9, 0.99). For all spins during the entire evolution, ﹩{\dot{E}}_{{\rm{EM}}}﹩ is in excellent agreement with P BZ6, and there is no alignment dependence on the output power.