adsabs/AstroCLIMB huggingface dataset:
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Four example images from our image library at 228 GHz (top) along with their inverse Fourier transforms (IFTs) following decompositions into logarithmic spirals (bottom). All images have R high = 40, with magnetic field states and spins as written at the top left of each column. In each column, the value of I max used to set the color scale is the maximum intensity in the GRRT image. The logarithmic spiral decompositions with m ≤ 20 do an excellent job at recovering even detailed image structure. In the retrograde images, some streams flip handedness as a function of radius, forming “S”-shaped patterns, some of which are marked with blue arrows.
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Tangential velocity (top) and angle of the magnetic field in the midplane (bottom) in the midplane of our GRMHD simulations, averaged over both azimuth and time. Quantities are computed in Boyer–Lindquist coordinates in the lab frame. Both plotted quantities change sign as a function of radius if and only if the system is retrograde (dashed lines), reflecting a transition in the dynamics of the accretion flow.
Paper: White Dwarf—Red Giant Star Binaries as Type Ia Supernova Progenitors: With and without Magnetic Confinement
Authors: Iminhaji Ablimit, Philipp Podsiadlowski, Rosanne Di Stefano, Saul A. Rappaport, James Wicker
Figure caption: Hertzsprung–Russell diagram for red giant donors with different masses in nonmagnetized CO WD binaries. Red circles indicate the location where the WDs starts to accrete matter, and red stars the location when SNe Ia occur.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: Left: bolometric infrared brightness temperature as a function of subobserver longitude with varying semimajor axis (colors, darker lines correspond to smaller separations) and interior assumptions (linestyles, solid lines correspond to fixed-flux cases while dashed lines correspond to hot-interior cases) for simulations with a surface gravity of 4 m s−2 (top) and 10 m s−2 (bottom). Right: phase-curve offset (top) and normalized phase-curve amplitude (bottom) as a function of semimajor axis for cases with a fixed flux (solid lines) and hot interior (dashed lines) with a surface gravity of 4 m s−2 (blue) and 10 m s−2 (orange). We find that the effect of interior assumptions on the phase-resolved emission is larger for higher-gravity planets.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: Temperature maps with overlaid wind streamlines at 28 mbar for cases with a surface gravity of 4 m s−2 and varying semimajor axis a = 0.0125−0.04 au, along with the local percent difference in temperature between the fixed-flux and hot-interior cases. Streamline width scales with wind speed, and all panels in the two leftmost columns and in the rightmost column, respectively, share a color scale. Local near-photospheric temperature differences of up to ∼10% occur in all simulations, with the largest differences occurring in midlatitudes on the nightside.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: As in Figure 1, but from simulations with no additional deep frictional drag applied and g = 4 m s−2. Similar to our results including a deep frictional drag, we find that there is a significant difference in the temperature structure between the fixed-flux and hot-interior cases. Notably, we find that the maximum local differences in temperature between the two interior assumptions can be larger in the cases without a deep frictional drag than in our main suite of GCMs.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: As in Figure 4, but showing temperature maps with overlaid wind streamlines at 57 mbar for cases with a surface gravity of 10 m s−2 and varying semimajor axis, along with the local percent difference in temperature between the fixed-flux and hot-interior cases. Maximum local near-photospheric temperature differences are larger than in the lower-gravity case due to the higher photosphere pressure, and similarly peak in midlatitudes on the nightside.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: As in Figure 1, but from simulations with no additional deep frictional drag applied and g = 10 m s−2. Similar to our results for g = 4 m s−2 shown in Figure 7, we find that differences between the fixed-flux and hot-interior assumptions are still significant when not including an additional deep frictional drag.
Paper: Interior Heating of Rocky Exoplanets from Stellar Flares with Application to TRAPPIST-1
Authors: Alexander Grayver, Dan J. Bower, Joachim Saur, Caroline Dorn, Brett M. Morris
Figure caption: Interior heating of the TRAPPIST-1 planets 1b–1g due to flare-associated CMEs. (a)–(c) Electrical conductivity profiles (note in case of the homogeneous conductivity models, profiles for different planets overlap). (d)–(f) Mean profiles of the time-averaged Joule heating assuming no intrinsic planetary magnetic field. (g)–(i) Same as (d)–(f), but with an Earth-like magnetic field. Shaded areas bound one standard deviation. For the constant conductivity models, 0.01 S m−1 is characteristic of peridotite at upper mantle conditions (Yoshino & Katsura 2013) and 1 S m−1 roughly corresponds to a 5% partial silicate melt at 1600 K.
Paper: Interior Heating of Rocky Exoplanets from Stellar Flares with Application to TRAPPIST-1
Authors: Alexander Grayver, Dan J. Bower, Joachim Saur, Caroline Dorn, Brett M. Morris
Figure caption: (a) Normalized probability distributions of the average volumetric heating rate generated in each TRAPPIST-1 planet by flare-associated ICMEs, for the 1D radial conductivity model and no planetary magnetic field. Colored dotted lines correspond to geometric mean values and the thick dashed line delineates 20 TW, which is Earth’s present-day radiogenic heat production. (b) Average volumetric heat produced by all flares within a specified energy interval for a planet without an intrinsic magnetic field. Markers denote the center of the interval. (c)–(d) Same as (a)–(b), but for a constant 0.01 S m−1 conductivity model. (e)–(h) Same as (a)–(d), but with an Earth-like magnetic field.
Paper: Interior Heating of Rocky Exoplanets from Stellar Flares with Application to TRAPPIST-1
Authors: Alexander Grayver, Dan J. Bower, Joachim Saur, Caroline Dorn, Brett M. Morris
Figure caption: (a) Magnetic field strength at each planet as a function of flare energy. The shaded range represents three standard deviations interval in the field decay rate ﹩\gamma \in { \mathcal N }(1.6,0.1)﹩ (see Table 2). (b) Realization of an external magnetic field profile at the TRAPPIST-1d planet for an ICME event with the energy 1032 erg (dashed line, left axis) and heat dissipated within the TRAPPIST-1d planet assuming a homogeneous 100 Ωm conductivity (solid line, right axis).
Paper: Interior Heating of Rocky Exoplanets from Stellar Flares with Application to TRAPPIST-1
Authors: Alexander Grayver, Dan J. Bower, Joachim Saur, Caroline Dorn, Brett M. Morris
Figure caption: Relation between the magnitude of the interplanetary magnetic field (IMF) and magnetic disturbance index (circles) as well as a linear fit (black solid line) and the corresponding uncertainty range (dashed lines). The regression line slope and intercept coefficients are −5.1 and −59.4, respectively. Data provided from the OMNI database.
Paper: Interior Heating of Rocky Exoplanets from Stellar Flares with Application to TRAPPIST-1
Authors: Alexander Grayver, Dan J. Bower, Joachim Saur, Caroline Dorn, Brett M. Morris
Figure caption: The effect of an ICME impact on a planet. Top row shows an ICME interacting only with the exosphere (considered by previous studies), in which the interior is treated as an insulator. Bottom row shows that planetary interiors are conductive and therefore the magnetic energy carried by an ICME induces currents in the interior, resulting in ohmic dissipation and heating. Influence of an intrinsic magnetosphere around a planet is not depicted here, but is discussed in the main text.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: Temperature maps with overlaid wind streamlines plotted on isobars for the fixed-flux and hot-interior cases with a = 0.0125 au and g = 4 m s−2, along with the difference in temperature between the two cases (fixed-flux temperature minus hot-interior temperature). Streamline width scales with wind speed, but each panel has a separate streamline scale in order to discern qualitative differences in flow patterns. All panels in the two leftmost columns and in the rightmost column, respectively, share a color scale. The dot at the center of each map displays the substellar point. Due to the difference in interior assumptions, there are significant differences in the domain-wide temperature at 10 bars. Local temperature differences between the two simulations persist even to low pressures of ∼1 mbar.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: Meridional–mean temperature profiles at the antistellar point, west limb, substellar point, and east limb in cases without (solid lines) and with (dashed lines) a hot interior. Both panels show results from simulations with a = 0.0125 au, and the top panel shows the case of a surface gravity g = 4 m s−2 while the bottom panel shows g = 10 m s−2. Temperature differences between the two cases are largest at pressures ≳1 bar due to the hotter 100 bar temperature in the hot-interior case. However, meridional–mean temperature differences between the two cases persist to the top of the simulation domain.
Paper: The Effect of Interior Heat Flux on the Atmospheric Circulation of Hot and Ultra-hot Jupiters
Authors: Thaddeus D. Komacek, Peter Gao, Daniel P. Thorngren, Erin M. May, Xianyu Tan
Figure caption: Horizontal wind speed on isobars for the fixed-flux and hot-interior cases with a = 0.0125 au, along with the difference in wind speed between the two cases (fixed-flux wind speed minus hot-interior wind speed). For the fixed-flux and hot-interior columns, each row shares a color scale for wind speed. However, each plot in the difference column has a different color scale for the difference in wind speed. The fixed-flux case has a stronger equatorial jet than the hot-interior case, and local differences in wind speed on the order of kilometers per second occur at pressures ≤1 bar, with maximum local wind speed differences increasing with decreasing pressure.
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Overview of data used in this study. The large white squares are the 2.′2 × 2.′2 FoVs of the two NIRCam modules. The left one is centered on the cluster BCG (color composite of all six observed NIRCam filters) and the right one (F200W shown only) is offset by approximately ﹩3^{\prime} ﹩ (or ∼1 Mpc at cluster redshift). The location of the selected compact star clusters studied in this work is marked with the green dashed contour. The JWST/MIRI coverage (red) is indicated for completeness, although MIRI data are not used in this study. The red inset shows an example selection of globular cluster (green circles) close to the BCG.
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Left: one-dimensional light profiles of the extracted compact star clusters (purple; stacked in each filter) and the PSF (gray) in all six NIRCam filters. This shows the unresolved nature of the extracted sources. Right: simulation to assess the maximum upper limit in size of an unresolved source given the PSF in the NIRCam/F150W filter (black). We simulated sources with half-light radii of 20, 50, 100, and 200 pc (blue, orange, green, and red lines) at z = 0.39 and a peak flux of 20 nJy, consistent with observations of the F150W stack (see left panel). We convolved those profiles with the PSF (which is shown as the thick black line) and include realistic noise from the real observations. We find that we would be able to resolve source larger than 50 pc. Hence, the selected compact star clusters must have sizes less than 50 pc. The lower panel shows the residual (source−PSF profile).
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Example model images and their simulated reconstructions using ngEHT and potential space-based extensions. Models are 345 GHz images corresponding to a MAD a • = 0.3 R high = 10 snapshot, a MAD a • = −0.3 R high = 10 snapshot, and a SANE a • = −0.9 R high = 40 snapshot respectively. Perfect resolution images are shown in the left columns, images blurred with a Gaussian kernel are shown in the central columns, and simulated reconstructions are shown in the right columns, demonstrating that future arrays will be capable of observing these features. The ngEHT would be capable of observing the flip in sign of ∠β 2 that occurs as a function of radius for retrogrades, while space-based extensions may be necessary to resolve the turnaround of individual streams.
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Probability of there existing an observable flip in the sign of ∠β 2 as a function of radius (a sign flip in its imaginary component) in our 228 GHz images. Images have first been convolved with a Gaussian with a FWHM of 20 μas. For a flip to be detectable, we demand that its ∣β 2∣ > 10−2 and its intensity is no less than a factor of 103 less than the annulus with the peak intensity. This metric preferentially selects for retrograde MADs. SANEs are more likely to fail the ∣β 2∣ > 10−2 condition due to their higher Faraday rotation depths. Some prograde SANEs are erroneously selected by this metric because their overall ∠β 2 ≈ 0, but such models could be ruled out with additional polarimetric information (Event Horizon Telescope Collaboration et al. 2021b).
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Probability of a flip in handedness of spiral features occurring between the interior and exterior regions, separated by the photon ring in our 228 GHz images. Different values of R high are shown in different colors. Probabilities computed with the Fourier method (Equation (1)) are plotted with solid lines, while probabilities computed with the gradient method (Equation (3)) are plotted with dotted lines. Requiring a few independent high-resolution observations, this metric can accurately identify retrograde systems. Note that our images have not been blurred for this analysis, since high spatial resolution of futuristic arrays is required to resolve these streams.
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: Time-averaged images for a MAD a • = 0.5 model on the left and a • = −0.5 on the right, each with R high = 1 at 228 GHz. In the lower panel, we plot ∠β 2 as a function of radius for these models, where the blue curve corresponds to the prograde and the red curve corresponds to the retrograde. In this model, time-averaging washes away the individual “S”-shaped streams, but preserves the flip in ∠β 2 as a function of radius in the retrograde.
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: An example model from our library (SANE, a • = −0.7, R high = 40) at the four frequencies included in our library, as indicated at the top of each panel. Total flux density and image-averaged optical depth are written at the bottom left. At 86 GHz, the image becomes larger and more optically thick than 228 GHz. At 690 GHz, the spiral features probed in this work grow fainter relative to the photon ring and more difficult to observe.
Paper: Observational Signatures of Frame Dragging in Strong Gravity
Authors: Angelo Ricarte, Daniel C. M. Palumbo, Ramesh Narayan, Freek Roelofs, Razieh Emami
Figure caption: An example image from our library (SANE, a • = +0.5, R high = 160, 228 GHz) and its “unwrapped” equivalent. Plotted in ﹩(\mathrm{ln}\rho ,\varphi )﹩ coordinates, logarithmic spirals with different pitch angles appear as diagonal lines with different slopes. Meanwhile, the circular photon ring becomes a nearly vertical line.
Paper: Interstellar Meteors Are Outliers in Material Strength
Authors: Amir Siraj, Abraham Loeb
Figure caption: IM1 and IM2 in size-abundance parameter space, expressed as number per star per differential unit of log size. The vertical error bars correspond to 95% Poisson uncertainties, while the horizontal error bars correspond to a factor of 2 in mass in each direction.
Paper: White Dwarf—Red Giant Star Binaries as Type Ia Supernova Progenitors: With and without Magnetic Confinement
Authors: Iminhaji Ablimit, Philipp Podsiadlowski, Rosanne Di Stefano, Saul A. Rappaport, James Wicker
Figure caption: Another example for the detailed evolution of CO WD+RG binaries using the MESA code: evolution of mass transfer, wind mass loss, WD/donor mass, orbital period, and radius of the donors are shown as a function of time. The right and left panels are for a nonmagnetized and highly magnetized WD (B = 2.5 × 107 G) with magnetic confinement, respectively. The initial masses of the WD and RG donors are 1.2 and 1.1 M ⊙,and the initial orbital period is 120 days for both cases.
Paper: White Dwarf—Red Giant Star Binaries as Type Ia Supernova Progenitors: With and without Magnetic Confinement
Authors: Iminhaji Ablimit, Philipp Podsiadlowski, Rosanne Di Stefano, Saul A. Rappaport, James Wicker
Figure caption: Initial parameter space for producing SNe Ia: the initial orbital period (P orb,i )—initial red giant donor mass (M RG,i ) plane for WD+RG systems. The initial WD masses are 1.0 and 1.2 M ⊙. The panels show the results for WDs with no or intermediate-strength magnetic fields (upper panel), and high magnetic fields (lower panel), respectively. Blue stars show the cases that produce SNe Ia. The solid blue lines show the parameter regions within which SNe Ia are produced. The cyan triangles in the upper regions in the figure indicate the occurrence of a common envelope, and the black crosses in the lower regions show where nova outbursts occur. The red triangles and black squares on the sides show regions with inefficient mass transfer.
Paper: White Dwarf—Red Giant Star Binaries as Type Ia Supernova Progenitors: With and without Magnetic Confinement
Authors: Iminhaji Ablimit, Philipp Podsiadlowski, Rosanne Di Stefano, Saul A. Rappaport, James Wicker
Figure caption: Detailed evolution of CO WD+RG binaries as a function of time using the MESA code. The left panels show the case of a nonmagnetic WD and the right panels the case of a magnetized WD (with B = 2.5 × 107 G). All other initial parameters are the same: the initial masses of the WDs and donor stars are 1.2 M ⊙ and 0.8 M ⊙, respectively, with an initial orbital period of 10 days. The evolution of mass transfer, WD/donor mass, orbital period, and the radius of the donors are shown. Wind mass loss is very low (<5 × 10−13 M ⊙/yr) and is not shown for clarity. RLOF M_dot and Polar M_dot in the figures are ﹩{\dot{M}}_{\mathrm{RL}}﹩ and ﹩{\dot{M}}_{{\rm{p}}}﹩ in the text, respectively.
Paper: Can 1D Radiative-equilibrium Models of Faculae Be Used for Calculating Contamination of Transmission Spectra?
Authors: Veronika Witzke, Alexander I. Shapiro, Nadiia M. Kostogryz, Robert Cameron, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh
Figure caption: Relative facular contrast from 3D simulations (as given in Equation (1)) and from 1D models (as discussed in Section 3) for facular regions with different magnetic flux density values (left to right columns) and viewing angles (top to bottom rows). The top row shows the relative contrast for the disk-integrated flux, the middle row for the disk center, and the bottom row for the limb (μ = 0.1).
Paper: White Dwarf—Red Giant Star Binaries as Type Ia Supernova Progenitors: With and without Magnetic Confinement
Authors: Iminhaji Ablimit, Philipp Podsiadlowski, Rosanne Di Stefano, Saul A. Rappaport, James Wicker
Figure caption: Example of the evolution of an RG star in the Hertzsprung–Russell diagram for the CO WD+RG binaries without and with magnetic confinement.
Paper: Can 1D Radiative-equilibrium Models of Faculae Be Used for Calculating Contamination of Transmission Spectra?
Authors: Veronika Witzke, Alexander I. Shapiro, Nadiia M. Kostogryz, Robert Cameron, Benjamin V. Rackham, Sara Seager, Sami K. Solanki, Yvonne C. Unruh
Figure caption: Disk-integrated relative facular contrast from 3D simulations (as given in Equation (1)) and normalized (see the text for details) relative contrasts from 1D models for different ΔT. The gray shaded area corresponds to the standard deviation of the scatter in contrasts due to temporal fluctuations in the 3D simulations. Different values of magnetic flux density (100 G in the top row and 300 G in the bottom row) and different wavelength intervals (left to right columns) are shown.
Paper: A Temperature Trend for Clouds and Hazes in Exoplanet Atmospheres
Authors: Raissa Estrela, Mark R. Swain, Gael M. Roudier
Figure caption: (Top) Spectral modulation indices of the TEC (light pink), DisEQ (magenta), and Indeterminate (orange) targets from the Roudier et al. (2021) catalog give the cloudiness level of each target. The solid blue line shows the best-fit for the “partial cloud/haze” targets (within gray region), a second-order polynomial to the data that can be used as a forecast of spectral modulation to future missions. The dashed blue line shows a fourth-order polynomial that highlights an increase in reduced hazy/cloudy atmospheres for the lower temperatures planets that are in the habitable zone. The blue shaded region indicates the zone of the targets with cloud-/haze-free atmospheres. (Bottom) Residual of the spectral modulation index subtracted from the model.
Paper: A Temperature Trend for Clouds and Hazes in Exoplanet Atmospheres
Authors: Raissa Estrela, Mark R. Swain, Gael M. Roudier
Figure caption: Amplitude of the spectral modulation in TEC (light pink), DisEQ (magenta), and Indeterminate (orange) targets in terms of scale height.