adsabs/AstroCLIMB huggingface dataset:
Paper: The Discovery of a 41 s Radio Pulsar PSR J0311+1402 with ASKAP
Authors: Yuanming Wang, 远明 王, Pavan A. Uttarkar, Ryan M. Shannon, Yu Wing Joshua Lee, Dougal Dobie, Ziteng Wang, Keith W. Bannister, Manisha Caleb, Adam T. Deller, Marcin Glowacki, Joscha N. Jahns-Schindler, Tara Murphy, Reshma Anna-Thomas, N. D. R. Bhat, Xinping Deng, Vivek Gupta, Akhil Jaini, Clancy W. James, John Tuthill
Figure caption: Radio lightcurve of PSR J0311+1402 extracted from 2 s images from the first two MeerKAT observations. The orange points represent the flux density measured at the UHF band, while the gray points represent the flux density measured at the L band. The bottom panel displays the spectral indices (with errors) calculated from the UHF- and L-band data during the MeerKAT epoch 2 observation.
Paper: Moving Plasma Structures and Possible Driving Mechanisms of Solar Microflares Observed with High-resolution Coronal Imaging
Authors: Qingmei Wang, Yi Bi, Hongfei Liang, JiaYan Yang, Liufan Gong
Figure caption: (a)–(d) SDO/AIA 171 Å images at peak times of Flare 1, Flare 2, Flare 3, and Flare 4, with the regions outlined (1–4). (e)–(h) Profiles of the average DEM temperature within the numbered contours shown on the left panels (a)–(d). The yellow curves represent the mean values over a 20 minute period, while the black curve shows the values at the peak time of each flare.
Paper: The Discovery of a 41 s Radio Pulsar PSR J0311+1402 with ASKAP
Authors: Yuanming Wang, 远明 王, Pavan A. Uttarkar, Ryan M. Shannon, Yu Wing Joshua Lee, Dougal Dobie, Ziteng Wang, Keith W. Bannister, Manisha Caleb, Adam T. Deller, Marcin Glowacki, Joscha N. Jahns-Schindler, Tara Murphy, Reshma Anna-Thomas, N. D. R. Bhat, Xinping Deng, Vivek Gupta, Akhil Jaini, Clancy W. James, John Tuthill
Figure caption: Filter bank plots for PSR J0311+1402 with the CRACO data. Left: the dedispersed tied-array beam filter bank with a time resolution of 110 ms in the whole 2 minute discovery observation. Right: the dedispersed data with a time resolution of 27.6 ms for the brightest pulse.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Summary of the main retrieval results from our best setup. Left panel: histograms of the final samples for the radius and mixing ratios of CH4, H2O, and NH3 from the best setup. Right panel: pressure–temperature profile from the best setup (black) and for the baseline retrieval with constant NH3 (purple); both corner plots are in Appendix D, Figures 7 and 8. The chemical profiles, with a 1σ region, of water (blue), ammonia (green), and methane (red) are shown with a dashed line for the best setup and with solid lines for the baseline setup. The navy and green dashed lines show water and ammonia condensation curves for solar metallicity from K. Lodders & B. Fegley (2002). The black solid line is the radiative contribution function for the best setup.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Top panel: MIRI fixed-slit LRS spectrum of WD 661 b (black) and best-fit model from TauREx (blue). The black rectangle in the upper left corner shows the λ = [11, 24] μm range. The red lines are the λ ∈ {12.8, 15, 18, 21} μm photometric points from MIRI. They are not included in the retrieval, just plotted over the best fit. The navy line at the same places corresponds to the best fit, binned to the resolution of these photometric points. The bottom left panel displays the residuals between the LRS data and the best fit, for which the root mean standard deviation is 1.247. The bottom right panel shows the histograms of these residuals.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Extracted spectra from exposure 1 (red) and exposure 2 (blue). We show a zoom-in of the spectra for better visibility.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: LRS spectrum using the default wavelength calibration (black) and best fit from TauRex (red). A wavelength discrepancy (Δλ ∼ 10 nm) is clearly visible.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Left panel: mean image of the first exposure after the ramp fitting. Middle panel: plot of the green line shown in the left panel. We clearly see the right-to-left gradient and the target’s signal. Right panel: line-by-line median for each of the two exposures and associated second-order polynomial fit.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Corner plot for our best setup.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Spectra extracted from every integration after our “background rescaling” step. The compatibility of the integrations constrains the variability of the planet over the 4 hr period in which they were taken.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Corner plot for our baseline setup.
Paper: MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements
Authors: Maël Voyer, Quentin Changeat, Pierre-Olivier Lagage, Pascal Tremblin, Rens Waters, Manuel Güdel, Thomas Henning, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alain Coulais, Leen Decin, Adrian M. Glauser, John Pye, Alistair Glasse, René Gastaud, Sarah Kendrew, Polychronis Patapis, Daniel Rouan, Ewine F. van Dishoeck, Göran Östlin, Tom P. Ray, Gillian Wright
Figure caption: Molecular absorption created by water (blue), ammonia (green), and methane (red).
Paper: Resolving the Super-Earth/Gas Giant Connection in Stellar Mass and Metallicity
Authors: Marta L. Bryan, Eve J. Lee
Figure caption: Fraction of disks expected to create inner (inside 100 days) super-Earths (black) compared to the fraction of disks with enough mass to create both the outer giant and inner super-Earths, bounded by thrice as much (lower edge of the red zone) and twice as much (upper edge of the red zone) as required to create a single giant at 2000 days. See text for more discussion on our definition. The span of the horizontal lines for each black circle illustrates the range of stellar masses used for each bin in the calculation of the disk fraction. We use the methodology of Y. Chachan & E. J. Lee (2023) and we choose turbulent αt = 10−3, ﹩{\dot{M}}_{\star ,\odot }=1{0}^{-8}{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩, and fragmentation velocity of 10 m s−1 as a representative illustration (we obtain qualitatively similar results at higher fragmentation velocities).
Paper: Resolving the Super-Earth/Gas Giant Connection in Stellar Mass and Metallicity
Authors: Marta L. Bryan, Eve J. Lee
Figure caption: Comparison of gas giant (0.5–20 MJup 1–10 au) frequencies from this Letter’s sample P(GG∣SE), the R21 sample P(GG), and the W20 sample P(GG). Top left: comparison of low, middle, and high-metallicity occurrence rates for early M dwarfs. Top right: same comparison for K dwarfs. Bottom left: same comparison for G stars. Bottom right: same comparison for F stars. For all panels, frequencies from this Letter are shown in red, R21 in gray, and W20 in blue. We find a transition from no correlation between super-Earths and gas giants for M stars of any metallicity to a positive correlation in the highest metallicity bin. This transition occurs with K dwarfs.
Paper: Resolving the Super-Earth/Gas Giant Connection in Stellar Mass and Metallicity
Authors: Marta L. Bryan, Eve J. Lee
Figure caption: Top left: M dwarf mass distribution from the R21 sample. Top right: M dwarf mass distributions from this Letter. Bottom left: M dwarf metallicity distribution from the R21 sample. Bottom right: M dwarf metallicity distribution from this Letter’s sample. For all panels, black histograms correspond to systems without gas giants, and red ones correspond to those with gas giants. Gas giants considered are 0.5–20 MJup and <10 au. All systems in this Letter’s sample host inner super-Earths.
Paper: Resolving the Super-Earth/Gas Giant Connection in Stellar Mass and Metallicity
Authors: Marta L. Bryan, Eve J. Lee
Figure caption: Top: occurrence rate of gas giants in metal-rich M dwarf systems. Bottom: same in metal-poor systems. Frequencies from this Letter are in maroon, and those from R21 are in black. While metal-rich M dwarfs have a higher frequency of gas giants for both samples, there is no significant difference in occurrence rates between the samples. We find no significant correlation between super-Earths and gas giants around M dwarf host stars.
Paper: Resolving the Super-Earth/Gas Giant Connection in Stellar Mass and Metallicity
Authors: Marta L. Bryan, Eve J. Lee
Figure caption: Left: average completeness map for the R21 sample. Right: average completeness map for this Letter’s sample. Detected gas giants in each sample are overplotted in teal.
Paper: Inhomogeneous Dust Biases Photometric Redshifts and Stellar Masses for LSST
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: Left panel: SEDs from the NIHAO-SKIRT catalog for one of the simulated galaxies. We include the SEDs of the galaxy observed from 10 different orientations ranging from face-on to edge-on (color gradient). We also include an SED excluding dust (black dashed). The SEDs are modeled at z = 0.4 and their emission lines are masked. For reference, we plot the LSST broadband throughput curves (dotted). Right panel: synthetic LSST magnitudes constructed from the NIHAO-SKIRT SEDs observed from the 10 different orientations. The magnitudes include LSST-like observational uncertainties.
Paper: A Rotational Disruption Crisis for Zodiacal Dust
Authors: Kedron Silsbee, Brandon S. Hensley, Jamey R. Szalay, Petr Pokorný, Jeong-Gyu Kim
Figure caption: Mass distribution observed by Ulysses for α-meteoroids near the equatorial plane in green (E. Grün et al. 1997) and β-meteoroids observed throughout the mission in purple (A. Wehry & I. Mann 1999). The distribution of α-meteoroids also has a minor contribution from interstellar grains in the lowest mass range (E. Grün et al. 1997). The top axis shows the mass converted to radius assuming “old cometary” grains (M. Wilck & I. Mann 1996). All α-meteoroid masses shown here would be rotationally disrupted on very short timescales with the current assumptions on rotational disruption physics.
Paper: A Rotational Disruption Crisis for Zodiacal Dust
Authors: Kedron Silsbee, Brandon S. Hensley, Jamey R. Szalay, Petr Pokorný, Jeong-Gyu Kim
Figure caption: Several relevant timescales for grain dynamics. Red dotted curve: timescale for Larmor precession (τB). Blue dashed curve: timescales for precession of grain angular momentum about direction of radiation anisotropy assuming that the grain is spinning at the breakup speed (τk; see text). Black dashed–dotted curve: dynamical time for grain on a circular orbit at 1 au (ignoring radiation pressure effects). Green solid curves: timescale for rotational disruption (see Equation (18)). The upper curve is for our fiducial ﹩{S}_{{\rm{\max }}}=5\times 1{0}^{9}﹩ dyn cm−2, corresponding to meteoritic iron (A. A. Ahles et al. 2021), while the lower curve is for ﹩{S}_{{\rm{\max }}}=5\times 1{0}^{7}﹩ dyn cm−2, corresponding to reinforced concrete (N. Arioglu et al. 2006).
Paper: A Rotational Disruption Crisis for Zodiacal Dust
Authors: Kedron Silsbee, Brandon S. Hensley, Jamey R. Szalay, Petr Pokorný, Jeong-Gyu Kim
Figure caption: β-meteoroid fluxes observed by multiple spacecraft and detection methods (N. E. Raouafi et al. 2023). Pioneer 8 and 9 (O. E. Berg & E. Grün 1973), Ulysses (A. Wehry & I. Mann 1999), as well electric-field-based observations from STEREO (A. Zaslavsky et al. 2012), SolO (A. Zaslavsky et al. 2021), and PSP (J. R. Szalay et al. 2020, 2021b; I. Mann & A. Czechowski 2021). The purple shaded region shows the estimated β-meteoroid fluxes from rotational disruption, significantly larger than the observed values.
Paper: A Rotational Disruption Crisis for Zodiacal Dust
Authors: Kedron Silsbee, Brandon S. Hensley, Jamey R. Szalay, Petr Pokorný, Jeong-Gyu Kim
Figure caption: Disruption timescale given by Equation (18) as a function of grain size and heliocentric distance. The black curve corresponds to the location in this space where the disruption time is equal to the dynamical time (see Equation (19)). The white space on the left side of the figure corresponds to the region in which ωeq < ωcrit, so the grain is not disrupted.
Paper: A Rotational Disruption Crisis for Zodiacal Dust
Authors: Kedron Silsbee, Brandon S. Hensley, Jamey R. Szalay, Petr Pokorný, Jeong-Gyu Kim
Figure caption: Comparison of the timescales for grain removal by collisions (assuming two different grain size distributions: lunar and interplanetary (IP; see E. Grun et al. 1985), Poynting–Robertson drag, and rotational disruption. The two plots are made for different orbital radii as labeled on the panels.
Paper: Decay of Turbulent Upper-hybrid Waves in Weakly Magnetized Solar Wind Plasmas
Authors: F. J. Polanco-Rodríguez, C. Krafft, P. Savoini
Figure caption: (a)–(c): Dispersion of the spectral magnetic energies ∣Bxk∣2, ∣Byk∣2, and ∣Bzk∣2 in the map (sign(kx)kλD, ω/ωp), filtered around ωp, at ωpt = 13,500, in a magnetized plasma with ωc/ωp = 0.07; the dispersion curves of ﹩{ \mathcal O }﹩- and ﹩{ \mathcal X }﹩-modes (black lines) and ﹩{ \mathcal Z }﹩-mode (white lines) calculated with the magnetoionic theory are superimposed for parallel (solid lines) and perpendicular (dashed lines) wave propagation (see also the inset of Figure 3(i)). (d)–(f): Corresponding energy spectra of ∣Bxk∣2, ∣Byk∣2, and ∣Bzk∣2 around frequency ωp, in the map (kxλD, kyλD). The boundary curve k*(θ) is represented in panels (d) and (e) by a black dashed contour; note that a small part of the ﹩{ \mathcal O }﹩-mode energy is visible on its right and left borders. (a)–(f) : arbitrary units and logarithmic scales. The colorbar is the same for panels (a)–(c) and for panels (d)–(f). (g) Spectrum of ﹩| {B}_{{ \mathcal L }{ \mathcal Z }{\boldsymbol{k}}}{| }^{2}=| {B}_{x{\boldsymbol{k}}}{| }^{2}+| {B}_{y{\boldsymbol{k}}}{| }^{2}﹩, filtered around ωp, at ωpt = 13,500, for ωc/ωp = 0.07, up to large k. (h) Evolution with time of the spectral magnetic energy ﹩{W}_{{ \mathcal L }{ \mathcal Z }}^{M}﹩, for different values of ωc/ωp (see legend), normalized by the initial beam energy, in logarithmic scales. (i) Variations with time of the electromagnetic energies carried by the ﹩{ \mathcal Z }﹩-, ﹩{ \mathcal O }﹩- and ﹩{ \mathcal X }﹩-mode waves (with ω ≲ ωp and ω ≳ ωp, respectively) near ωp (see legend), normalized by the initial beam energy, in logarithmic scales, for ωc/ωp = 0.07. (a)–(g) and (i): The lengths of simulation boxes are ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{D}^{2},﹩ with grid numbers Nx = 4096 and Ny = 2048; (h): ﹩{L}_{x}\times {L}_{y}=1448\times 1448{\lambda }_{D}^{2},﹩ Nx = Ny = 1024. The frequency resolution in (a)–(c) is δω ≃ 2 · 10−3ωp. The first set of physical parameters is used (see above).
Paper: Decay of Turbulent Upper-hybrid Waves in Weakly Magnetized Solar Wind Plasmas
Authors: F. J. Polanco-Rodríguez, C. Krafft, P. Savoini
Figure caption: (a)–(c): Spectra at small k-scales of ﹩{ \mathcal L }{ \mathcal Z }﹩ wave energy ﹩| {B}_{{ \mathcal L }{ \mathcal Z }{\boldsymbol{k}}}{| }^{2}=| {B}_{x{\boldsymbol{k}}}{| }^{2}+| {B}_{y{\boldsymbol{k}}}{| }^{2}﹩, filtered around ωp, for ωpt = 5800, 7200, and 14,000, in a plasma with ωc/ωp = 0.07. The boundary curve k = k*(θ) at ω = ωmin and the isocontours ﹩k=k{{\prime} }_{* }(\theta ,\omega ,t)﹩ at frequency ω and time t are represented by black solid and dashed lines, respectively; the latter are calculated by solving the equation ﹩{\omega }_{{ \mathcal L }{ \mathcal Z }}(k,\theta )=\omega ﹩, and are represented for ω/ωp = 0.996, 0.998, and 0.9995 in panels (a), (b), and (c), respectively. (d)–(f): Spectra of ﹩| {B}_{{ \mathcal L }{ \mathcal Z }{\boldsymbol{k}}}{| }^{2}﹩ radiated at ωp, for ωpt = 14000, in plasmas with ωc/ωp = 0.02, 0.07,  and 0.14; the dashed line represents the curve k = k*(θ) calculated in all cases by solving the equation ﹩{\omega }_{{ \mathcal L }{ \mathcal Z }}(k,\theta )={\omega }_{\min }﹩. (g) Spectral electric energy ∣Ek∣2, radiated at ωp, at ωpt = 9300, for Te = 20eV, Te/Ti = 3, ωc/ωp = 0.02, vb ≃ 0.08c, and nb/n0 = 5 · 10−4. (h): Magnetic energy ﹩| {B}_{{ \mathcal L }{ \mathcal Z }{\boldsymbol{k}}}{| }^{2}﹩ corresponding to (g). (a)–(h): Arbitrary units and logarithmic scales. The first set of physical parameters is used for (a)–(f) and the second one for (g)–(h) (see above). In panels (a)–(c), the lengths of the simulation boxes are ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{D}^{2},﹩ with Nx = 4096 and Ny = 2048; in panels (d)–(h), they are ﹩{L}_{x}\times {L}_{y}=1448\times 1448{\lambda }_{D}^{2},﹩ with Nx = Ny = 1024.
Paper: Self-consistent Multidimensional Penrose Process Driven by Magnetic Reconnection
Authors: Filippo Camilloni, Luciano Rezzolla
Figure caption: Top panel: rate of energy extraction per unit of enthalpy density, ﹩{\dot{E}}_{{\rm{rec}}}/{w}_{0}﹩, at the ergobelt of a maximally filling torus as a function of the magnetization σ0 and BH angular velocity ﹩{\omega }_{{}_{{\rm{BH}}}}﹩ (the top horizontal axis uses instead a scale in a/M). The red solid line marks the critical magnetization σ0,crit below which no PP is possible (gray shaded area). Bottom panel: the same as in the top but when the energy-extraction rate is normalized to the BZ power ﹩{\dot{E}}_{{\rm{rec}}}/{\dot{E}}_{{}_{{\rm{BZ}}}}﹩.
Paper: Self-consistent Multidimensional Penrose Process Driven by Magnetic Reconnection
Authors: Filippo Camilloni, Luciano Rezzolla
Figure caption: The same as Figure 2 but for θ = π/2 and illustrating the (r, a) dependence. For each BH spin, the torus cusp is located between rmb (black line) and rms (red line). Maximally filled tori penetrate the ergosphere (r0 = 2 M on the equator) for a/M ≳ 0.83. Tori with the cusp at the largest possible position (rcusp = rms or ℓ0 = ℓms) require larger BH spins, a/M ≳ 0.94. By increasing the BH spin rms → rmb → r+, the ergobelt area grows and comparatively smaller magnetizations are needed for a plasmoid-mediated PP.
Paper: Self-consistent Multidimensional Penrose Process Driven by Magnetic Reconnection
Authors: Filippo Camilloni, Luciano Rezzolla
Figure caption: Polar sections of tori with ℓ0 ≃ ℓmb (light blue shading) entering the ergosphere r0 (green dashed line), with BH spin increasing from left to right. The torus surface inside the ergosphere, dubbed the ergobelt (red solid line), is suitable for reconnection to drive a PP. The color map reports values of the magnetization σ0 necessary for the pair-production of plasmoids with ﹩{\varepsilon }_{+}^{\infty }\gt 0﹩ and ﹩{\varepsilon }_{-}^{\infty }\lt 0﹩ at different positions in the torus, with the yellow solid line marking σ0 = 10.
Paper: Self-consistent Multidimensional Penrose Process Driven by Magnetic Reconnection
Authors: Filippo Camilloni, Luciano Rezzolla
Figure caption: Shown with gray contours are the isolevels of the rest-mass density of a torus with a toroidal magnetic field entering the BH ergosphere (green region). Reconnection and plasmoid production can take place on the surface of the torus; if this happens in the ergoregion, i.e., on the “ergobelt” (red region), then a PP can be activated from plasmoids with a negative energy-at-infinity.
Paper: Formation of the Dark Matter–Deficient S0 Galaxy NGC 4111 under the Tidal Interactions
Authors: Mei Ai, Ming Zhu, Nai-ping Yu, Jin-long Xu, Xiao-lan Liu, Yingjie Jing, Qian Jiao, Yao Liu, Chuan-peng Zhang, Jie Wang, Peng Jiang
Figure caption: Comparison between the FAST observational data and the best-fitting model data demonstrated by the H I major axis P–V diagram. Left panel: the P–V diagram extracted from the FAST data cube in the direction of the PA derived from our simulation; the red plus indicates the center of the disk. The radius of the H I disk is labeled. Middle panel: the P–V diagram extracted from the model data cube in the same direction as the left panel. Right panel: the difference between observed and model data, which evaluates the performance of our simulation. The contour levels for the left and middle panels are 0.6, 2.6, 5.4, 8.6, 10.7, and 12.9 mJy beam−1. The negative contours for the right panel are −5.4, −2.9, −1.4, and −0.7 mJy beam−1, and the positive contours are the same as the left and middle panels.