adsabs/AstroCLIMB huggingface dataset:
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Full multiwavelength Sgr A* light curves on 2024 April 6. From bottom to top the green curve shows the average of the SMA upper (230 GHz) and lower (210 GHz) sidebands. The superposed yellow to red curves show the observed flux densities in JWST/MIRI Channels 1–4, respectively. The blue curve shows the Chandra 2–8 keV light curve (corrected for background and pileup) with 300 s binning, and the horizontal dark blue line shows the median of the entire Chandra observation. The purple curve shows the NuSTAR 3–30 keV light curve with 300 s binning. The dark purple overlay is the average during the observation period. Each light curve has its own ordinate as labeled, and times are UTC at the solar system barycenter. No X-ray flares were detected by either Chandra or NuSTAR. The gray region highlights the MIR flare interval seen by JWST.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Images and light curves of Sgr A* observed on 2024 April 6. Panel (A) at the top shows 8.1 μm residual images after subtracting a constant image shown by the gray contour lines. Each image shows ~20 minutes of averaged data before (left), during (middle), and after (right) the flare. North is up, and east is to the left. Panels (B) show light curves of Sgr A* at 1.3 mm (top left and right duplicated) and the four MIRI spectral channels with wavelengths as labeled. Flux densities are as observed, i.e., calibrated but with no extinction correction. t = 0 marks the beginning of the flare as we define it, and all times have been corrected to the barycentric reference frame. Panel (C) shows normalized light curves of the four MIRI bands to demonstrate the change in spectral index.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Observed light curves with model fit. Points show the observed data, and solid lines show the predictions of the simple model described in the text. (A) 220 GHz data. (B) MIR data. The four yellow to red lines show the best-fit model predictions for each channel as labeled. The black dashed line shows the modeled Doppler boosting and deboosting due to the orbital motion of the emission region. The dotted line shows the modeled Gaussian injection curve of power-law electrons. The flare phases described in the text are indicated at the bottom.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Comparison of Sgr A* and reference-pixel light curves. Panels show the median-subtracted light curves of the Sgr A* pixel (color) and reference pixels (gray) in Channels 1, 2, 3, and 4 (panels (A), (B), (C), and (D), respectively). The black lines show the best linear fit to each reference-pixel trend. Table A1 gives the line slopes. Times are shown in UTC at the solar system barycenter on the lower abscissa and relative to the adopted t = 0 on the upper abscissa.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: MIR images of the Galactic center with JWST. The color insets show JWST 5.3 μm (A), 8.1 μm (B), 12.5 μm (C), and 19.3 μm (D) observations. The JWST/MIRI images are superposed on the ﹩L^{\prime} ﹩ (NIR 3.8 μm) stellar-background image from the Keck Observatory (J. L. Hora et al. 2014). The image scale is labeled in arcseconds with Sgr A* at the origin. North is up, east to the left.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Median images of the Galactic center in Channels 1, 2, 3, and 4. The location of Sgr A* is marked with the square box, and the locations of the reference pixels used to estimate the noise in the image are marked by white dots. Axis labels are in pixel number with pixel angular sizes given in the text. The flux-density scale is in units of MJy sr−1.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Evolution of the spectral index during the flare. Panel (A) shows the normalized MIR light curves, and panel (B) shows the change in the best-fit spectral index. The colors indicate the spectral index with blue colors Δα ≈ 0.0, and red colors Δα ≈ −0.4.
Paper: MUSEQuBES: Unveiling Cosmic Web Filaments at z ≈ 3.6 through Dual Absorption and Emission Line Analysis
Authors: Eshita Banerjee, Sowgat Muzahid, Joop Schaye, Sebastiano Cantalupo, Sean D. Johnson
Figure caption: The optimally extracted Lyα SB maps of the seven LAEs (G7) within the MUSE FOV centered on the quasar Q1317–0507 (marked by the “+” sign). The pixels within the 3D segmentation map for each LAE are combined and projected onto the image, with the gray contours representing the 5 and 25σ from the mean flux levels of the continuum-bright objects. A Gaussian smoothing function with σ = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 ( ≡ 1 pixel) has been applied to enhance the visual clarity of the SB map. The histogram in the top panel displays the redshift distribution of the LAEs. The object IDs are indicated beside each LAE as well as in the histogram plot.
Paper: MUSEQuBES: Unveiling Cosmic Web Filaments at z ≈ 3.6 through Dual Absorption and Emission Line Analysis
Authors: Eshita Banerjee, Sowgat Muzahid, Joop Schaye, Sebastiano Cantalupo, Sean D. Johnson
Figure caption: Velocity plot of the G7 system, showing several Lyman-series lines (arranged in descending order of wavelength from bottom to top) along with metal lines detected in the system. The observed spectrum is shown in blue, with the best-fitting model curve from VPFIT in red. Fits for contaminating transitions are displayed in green. The black, orange, and red ticks mark the positions of individual H I, C IV, and Si IV components, respectively. For visual clarity, the normalized fluxes of each line are shifted vertically. The positions of the seven LAEs are marked by red stars at the bottom, and their respective IDs are written on top, with Δv = 0 corresponding to their median redshift of z = 3.577. The total column densities measured within the three pink shaded regions (S1, S2, and S3) are used to construct photoionization models.
Paper: MUSEQuBES: Unveiling Cosmic Web Filaments at z ≈ 3.6 through Dual Absorption and Emission Line Analysis
Authors: Eshita Banerjee, Sowgat Muzahid, Joop Schaye, Sebastiano Cantalupo, Sean D. Johnson
Figure caption: Top: the SB profile of the extended filament-like structure as well as the associated LAEs of the G7 system. The contour indicates the SB ﹩=1{0}^{-19}\,{\rm{erg}}\,{{\rm{s}}}^{-1}\,{{\rm{cm}}}^{-2}\,{{\rm{arcsec}}}^{-2}﹩. Bottom: the SNR map of the extended emission and the associated LAEs, plotted on top of a single wavelength layer associated to the extended emission. The white contours correspond to the SNR of 2. In both panels, the positions of the seven LAEs are highlighted by the squares, while the quasar position is marked by an “x” symbol. The maximum projected length of this structure is ≈260 pkpc. Refer to the text for the details about white dashed and dotted lines.
Paper: MUSEQuBES: Unveiling Cosmic Web Filaments at z ≈ 3.6 through Dual Absorption and Emission Line Analysis
Authors: Eshita Banerjee, Sowgat Muzahid, Joop Schaye, Sebastiano Cantalupo, Sean D. Johnson
Figure caption: Measured column densities of different transitions associated with S1, S2, and S3 (top to bottom) are shown in red, with upper limits indicated by downward arrows. Blue squares represent the predicted column densities based on the median values of the model parameters from their respective posterior PDFs. The median values of metallicity and nH along with their 16th–84th percentile ranges are displayed at the top. The bottom panel shows the residuals (﹩{\rm{\Delta }}\equiv {{\rm{log}}}_{10}\,N-{{\rm{log}}}_{10}\,{N}_{{\rm{model}}}﹩).
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Posterior of the MCMC chain. Columns left to right show the starting angular position of the emitting region (Ω0), the width of the Gaussian electron-injection pulse (σ), the time of the maximum electron-injection rate (﹩{t}_{{\rm{\max }}}﹩), the magnetic field strength (B), the total number of injected electrons (﹩\mathrm{log}({N}_{{\rm{e}}})﹩), the flux density of the constant 220 GHz component (ϕ in units of mJy), and the orbit radius of the emitting region in units of the Schwarzschild radius (﹩{R}_{{\rm{flare}}}/{R}_{{\rm{S}}}﹩). Histograms above or to the right of each column show the probability distribution for the corresponding parameter, and each parameter's median value and uncertainty (16% and 84% range) are shown above its histogram plot.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Light curves of reference pixels compared with the Sgr A* pixel. Gray curves in each panel (Channels 1, 2, 3, and 4 in panels (A), (B), (C), and (D), respectively) show the reference-pixel light curves after removing the linear slope but without subtracting each pixel's median value. Colored lines show the same for the Sgr A* pixel.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Distribution of model magnetic field values as β and Ti/Te are varied. The green line shows all parameter combinations that result in a 45 G magnetic field, while the red cross indicates EHT's magnetic field value for their chosen parameters of β = 1 and Ti/Te = 3.
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Background-subtracted, de-trended light curves extracted from 2D detector frames compared to data cube-extracted light curves. The colored light curves are the light curves used in the analysis of this Letter. The black lines are the corresponding lines extracted from the 2D integral field unit detector, extracted from the detector slice corresponding to the Sgr A* spaxel in the 3D cube. Both light curves have been normalized using Equation (C8).
Paper: First Mid-infrared Detection and Modeling of a Flare from Sgr A*
Authors: Sebastiano D. von Fellenberg, Tamojeet Roychowdhury, Joseph M. Michail, Zach Sumners, Grace Sanger-Johnson, Giovanni G. Fazio, Daryl Haggard, Joseph L. Hora, Alexander Philippov, Bart Ripperda, Howard A. Smith, S. P. Willner, Gunther Witzel, Shuo Zhang, Eric E. Becklin, Geoffrey C. Bower, Sunil Chandra, Tuan Do, Macarena Garcia Marin, Mark A. Gurwell, Nicole M. Ford, Kazuhiro Hada, Sera Markoff, Mark R. Morris, Joey Neilsen, Nadeen B. Sabha, Braden Seefeldt-Gail
Figure caption: Posteriors of the electron magnetization σe (left) and proton magnetization σp (right) of the flare. The thick vertical lines indicate the median values, and the dashed lines mark the quartiles.
Paper: Stellar Contamination Correction Using Back-to-back Transits of TRAPPIST-1 b and c
Authors: Alexander D. Rathcke, Lars A. Buchhave, Julien de Wit, Benjamin V. Rackham, Prune C. August, Hannah Diamond-Lowe, João M. MendonÇa, Aaron Bello-Arufe, Mercedes López-Morales, Daniel Kitzmann, Kevin Heng
Figure caption: Comparison of uncorrected transit spectra and stellar contamination factors derived from out-of-transit stellar spectra. The transit spectrum of planet c is shown along with stellar contamination models calculated from the mean stellar spectrum just before the transit of c (S3). The green line shows the model that assumes the entirety of the cooler spectral component is present outside of the transit chord. The purple line shows the best-fit stellar contamination model, allowing for a mixture of cool and warm spectral components throughout the stellar disk and a slight overdensity of the cool component outside the transit chord. Both contamination models have been multiplied by a flat planetary transit spectrum that yields the best fit to the data. The inset panel shows the X2 value for models with varying levels of coverage of the cool component within the transit chord (f1,chord). Rather than the cool component being a monolithic unocculted feature, the relatively muted features in the transit spectrum point to the component spectra being relatively well mixed across the stellar surface, with the cool component being slightly underrepresented in the transit chord. While this technique cannot probe the spatial distribution of features beyond their full-disk and transit-chord covering fractions, we present illustrative examples of stellar photospheres with spot distributions that reflect these models, with the transit chord of c highlighted (produced with spotter; L. J. Garcia & B. V. Rackham 2023).
Paper: Stellar Contamination Correction Using Back-to-back Transits of TRAPPIST-1 b and c
Authors: Alexander D. Rathcke, Lars A. Buchhave, Julien de Wit, Benjamin V. Rackham, Prune C. August, Hannah Diamond-Lowe, João M. MendonÇa, Aaron Bello-Arufe, Mercedes López-Morales, Daniel Kitzmann, Kevin Heng
Figure caption: Transit spectra of TRAPPIST-1 b and TRAPPIST-1 c and the impact of the correction process. Top left panel: transit spectra for TRAPPIST-1 b (blue) and TRAPPIST-1 c (orange), shown both at native pixel resolution (faded points) and binned into 0.1 μm intervals (solid points). Bottom left panel: corrected transit spectrum of TRAPPIST-1 c (purple). The corrected spectrum was computed as the ratio of the TRAPPIST-1 c transit spectrum to the TRAPPIST-1 b transit spectrum, multiplied by the weighted mean of the TRAPPIST-1 b transit depth in the 2–5 μm range. The corrected spectrum is displayed at native pixel resolution and binned into 0.1 μm intervals. Also plotted is a reference model for a 10 bar O2-dominated outgassing atmosphere (similar to that of A. P. Lincowski et al. 2018), illustrating potential atmospheric signatures and their expected amplitudes in this wavelength range. Top right panel: Allan variance plot for the 0.8–2 μm range, comparing the standard deviation of residuals before correction (orange) and after correction (purple) as a function of bin size for TRAPPIST-1 c. Dashed lines represent the expected noise reduction for uncorrelated (white) noise. Bottom right panel: similar to the panel above it but for the 2–5 μm range. The transit spectra used in this figure, provided at pixel-level resolution, are available at 10.5281/zenodo.14644472.
Paper: A Multiwavelength Investigation of Spiral Structures in z > 1 Galaxies with JWST
Authors: Boris S. Kalita, Si-Yue Yu, John D. Silverman, Emanuele Daddi, Luis C. Ho, Andreas L. Faisst, Miroslava Dessauges-Zavadsky, Annagrazia Puglisi, Simon Birrer, Daichi Kashino, Xuheng Ding, Jeyhan S. Kartaltepe, Zhaoxuan Liu, Darshan Kakkad, Francesco Valentino, Olivier Ilbert, Georgios Magdis, Arianna S. Long, Shuowen Jin, Anton M. Koekemoer, Richard Massey
Figure caption: Image compilation of the sample: (top panels) the RGB images (F150W, F277W, F444W) of the 8 galaxies used in this work are 100 × 100 pixels or 3″ × 3″. The COSMOS2015 (C. Laigle et al. 2016) IDs are provided for each galaxy, with the final two in red denoting the possible presence of an interacting companion. All are within a redshift range of 1.43 ≤ z ≤ 1.74 and have stellar masses of 1010.5−11.4 M⊙. The corresponding F444W (middle panels, with 5σ contours) and F150W (PSF-matched to F444W, bottom panels, with lower 3σ contours to account for the lower image depth) residual images after subtraction of a bulge and disk model highlight the presence of spiral arms.
Paper: Production, Transport, and Destruction of Dust in the Kuiper Belt: The Effects of Refractory and Volatile Grain Compositions
Authors: Thomas Corbett, Alex Doner, Mihály Horányi, Pontus Brandt, Will Grundy, Carey M. Lisse, Joel Parker, Lowell Peltier, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne J. Verbiscer
Figure caption: Left: equilibrium number density profiles of silicate and ice grains near the ecliptic and above the SDC mass threshold as a function of heliocentric distance using the SBDB (top), CFEPS (middle), and OSSOS (bottom) KBO databases/models. The combined modeled number density (black) of silicate (red) and ice (blue) grains is fitted to SDC data with 1σ error bars (black) for heliocentric distances greater than 10 au. Right: corresponding χ2 maps of silicate and ice mass production rates for each KBO database/model with best-fit production rates (white crosses). Regions of confidence corresponding to a significance level of α = 0.68 and α = 0.99, or 1σ and 3σ, respectively, are encircled in white lines. The 1σ production rate ranges can be found in Table 1.
Paper: Production, Transport, and Destruction of Dust in the Kuiper Belt: The Effects of Refractory and Volatile Grain Compositions
Authors: Thomas Corbett, Alex Doner, Mihály Horányi, Pontus Brandt, Will Grundy, Carey M. Lisse, Joel Parker, Lowell Peltier, Andrew R. Poppe, Kelsi N. Singer, S. Alan Stern, Anne J. Verbiscer
Figure caption: Equilibrium number density profiles of well-mixed (top) and differentiated (bottom) grains near the ecliptic and above the SDC mass threshold as a function of heliocentric distance using the SBDB KBO database. Each histogram is labeled with its corresponding ice mass fraction. The same number of grains is produced for each case, matching the best-fit silicate production rate for the SBDB KBO database in Table 1.
Paper: Hot Jupiters Are Asynchronous Rotators
Authors: Marek Wazny, Kristen Menou
Figure caption: Zonally averaged zonal wind speeds of planet Kepler7b generated by the GCM. Wind speeds are shown in m s−1 where the red line separates regions of opposite wind directions. Wind speeds are solved on pressure levels seen on the left vertical axis, and the converted radial coordinates (averaged) via Equation (1) are seen on the right vertical axis.
Paper: Hot Jupiters Are Asynchronous Rotators
Authors: Marek Wazny, Kristen Menou
Figure caption: Top: numerically evaluated Log10 drag timescale (s) averaged radially. Bottom: numerically integrated current in G s−1 using Equation (6) with a zero boundary term and red lines separating positive and negative regions. Both panels are for planet Kepler7b, assuming a magnetic field strength of 10 G.
Paper: Hot Jupiters Are Asynchronous Rotators
Authors: Marek Wazny, Kristen Menou
Figure caption: Asynchronicity ratio, Log10(Δω/ωsync), for planets HD189733b, HD209458b, and Kepler7b. Values are calculated given an equilibrium temperature and magnetic field strength. Red lines correspond to the isolines Δω/ωsync = 1, while yellow lines show the equilibrium temperature for each planet.
Paper: Hot Jupiters Are Asynchronous Rotators
Authors: Marek Wazny, Kristen Menou
Figure caption: Left: magnetic torque (dyne cm) of planet Kepler7b radially evaluating Equation (9) for the approximate drag time in Equations (7) (bottom) and (8) (top). Right: magnetic torque of planet Kepler7b zonally integrated for the approximate (bottom) and integrated (top) drag times. Red lines separate regions of positive and negative contributions.