adsabs/AstroCLIMB huggingface dataset:
Paper: An Efficient Tidal Dissipation Mechanism via Stellar Magnetic Fields
Authors: Craig D. Duguid, Nils B. de Vries, Daniel Lecoanet, Adrian J. Barker
Figure caption: Time series for each stellar model M ⋆ ∈ {1.2, 1.3, 1.4, 1.5, 1.6} M ⊙ (see legend) of the dissipation due to wave conversion parameterized by the modified tidal quality factor ﹩Q^{\prime} ﹩ (﹩1/Q^{\prime} ﹩ is proportional to the dissipation). Each ﹩Q^{\prime} ﹩ curve is partitioned into a region where we expect wave conversion to operate (solid) and where the criterion is not satisfied (dotted). Note that this partitioning assumes the core dynamo-generated field is in equipartition. If the field strength is above equipartition, then the period where wave conversion can operate is extended. The vertical lines denote when the convective core vanishes for each respective model. The insert in the top panel displays the same information, but the upper curve for each respective model is for a 1.5 day tidal period (3 day orbit). Included in the top panel are observational estimates of ﹩Q^{\prime} ﹩ taken from Akinsanmi et al. (2024) and Leonardi et al. (2024; point A and L respectively) for WASP-12b where the assumed stellar masses are {1.422, 1.325} M ⊙ respectively. Note that error bars for ﹩Q^{\prime} ﹩ are within the symbol. The lower panel shows the inspiral timescale associated with each stellar model for a Jupiter-mass planet on a 1 day orbit. The same labeling as for the upper panel is adopted.
Paper: An Efficient Tidal Dissipation Mechanism via Stellar Magnetic Fields
Authors: Craig D. Duguid, Nils B. de Vries, Daniel Lecoanet, Adrian J. Barker
Figure caption: Time series for each stellar model M ⋆ ∈ {1.2, 1.3, 1.4, 1.5, 1.6}M ⊙ (see legend) of: the estimated convective core dynamo field strength B eq using equipartition arguments and the threshold for wave conversion B crit as computed by Equation (2). The thinner branch of B crit denotes the value of Equation (2) is evaluated using the global minimum of B crit rather than the local minimum in the lower 10% of the radiative zone. The vertical lines indicate when the convective core vanishes for each respective model. Note that when B eq > B crit, then we can expect conversion of IGWs to MWs and hence efficient tidal dissipation.
Paper: An Efficient Tidal Dissipation Mechanism via Stellar Magnetic Fields
Authors: Craig D. Duguid, Nils B. de Vries, Daniel Lecoanet, Adrian J. Barker
Figure caption: Radial profiles within the radiative zone of the buoyancy frequency, N(r), and the critical field strength for wave conversion, B crit(r), for our 1.3 M ⊙ stellar model. We show these quantities for three different times t ∈ {0.23, 2.14, 3.3} × 109 yr (corresponding to core hydrogen mass fractions X ≈ {0.66, 0.31, 0.02}). These correspond to prior to convective core retreat, some time after the convective core begins to shrink, leading to a localized spike in N, and some time after the convective core has vanished. The latter of these highlights the persistence of the N spike. Solid dots on the B crit lines denote the global and local minima within the lowest 10% of the radiative zone. We use the latter for our evaluation of B crit throughout this work.
Paper: An Efficient Tidal Dissipation Mechanism via Stellar Magnetic Fields
Authors: Craig D. Duguid, Nils B. de Vries, Daniel Lecoanet, Adrian J. Barker
Figure caption: Schematic of tidal dissipation due to wave conversion. Tidally excited internal gravity waves (IGWs) are launched from the boundary between the convective envelope and radiative zone and travel toward the center of the star. If a convective core dynamo produces a field strong enough to surpass a critical threshold B crit, then the IGWs are fully converted to outwardly propagating magnetic waves (MWs). The outward MWs can then be fully dissipated as they propagate through the magnetized radiative zone.
Paper: Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick
Authors: Tatsuya Akiba, Selah McIntyre, Ann-Marie Madigan
Figure caption: Evolution of tidal disruption rates and apsidal alignment for the M disk = 20 M ⊕ simulation. Top: the cumulative mass accreted by the white dwarf from tidal disruption events over time. The axis on the right shows the fraction of the debris disk that is tidally disrupted. Center: eccentricity evolution of a small sample of planetesimals that become tidally disrupted. The quantity, 1 − e, is plotted on the y-axis using a logarithmic scale. The time at which tidal disruption is detected is denoted by an open black circle. Bottom: the evolution of the magnitude of the mean eccentricity vector. The green shaded region indicates the noise floor above which apsidal alignment is statistically significant at the 3σ level.
Paper: Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick
Authors: Tatsuya Akiba, Selah McIntyre, Ann-Marie Madigan
Figure caption: A comparison of the planetesimals’ orbital angular momenta and apsidal alignment as a function of the semimajor axis at t = 0 postkick ranging from α = 3° to 90°. Top: the z-component of angular momentum normalized by the circular angular momentum, ﹩{j}_{\mathrm{circ}}=\sqrt{{{GM}}_{* }a}﹩. Orbits above the dashed line are prograde and those below are retrograde. Orbits are more eccentric closer to the dashed line and are circular when ∣j  z /j circ∣ = 1. The planetesimal orbits are color-coded by the y-component of the eccentricity vector. Bottom: the magnitude of the mean eccentricity vector, 〈 e 〉. The green, shaded region indicates the noise floor above which alignment is statistically significant at the 3σ level. Retrograde orbits and apsidal alignment both emerge as the kick tends toward an in-plane direction.
Paper: Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick
Authors: Tatsuya Akiba, Selah McIntyre, Ann-Marie Madigan
Figure caption: A histogram of kick angles with respect to the orbital angular momentum axis. α = 0° or 180° indicates an out-of-plane kick where the kick is parallel or antiparallel to the angular momentum vector, whereas α = 90° means that the kick is in the planetesimal disk plane. The analytic expectation assuming an isotropic distribution is shown with the blue, solid line, and the numerical results of sampling 2500 times are shown in purple bars. The most likely natal kick direction is in the planetesimal disk plane.
Paper: Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick
Authors: Tatsuya Akiba, Selah McIntyre, Ann-Marie Madigan
Figure caption: Snapshots of planetesimal orbits for the M disk = 20 M ⊕ simulation at (left:) t = 0 prekick, (center:) t = 0 postkick, and (right:) t = 100 Myr. Initially, every planetesimal has a circular, prograde orbit. The kick forms an eccentric debris disk, which coherently precesses while maintaining apsidal alignment.
Paper: The Kinematic and Chemical Properties of the Close-in Planet Host Star 8 UMi
Authors: Huiling Chen, Yang Huang, Wei Zhu, Timothy C. Beers, Renjing Xie, Yutao Zhou, Sharon Xuesong Wang, Wei Wang, Sofya Alexeeva, Qikang Feng, Haozhu Fu, Haining Li, Lile Wang, Huawei Zhang
Figure caption: Left panels: [Fe/H] estimates as a function of reduced equivalent width (upper subpanel) and excitation potential (lower subpanel). The open circles represent the lines filtered by the sigma-clipping process of ISPEC with a 0.90 weight scale. Right panels: synthetic spectrum-fitting examples (red solid line) of 8 UMi in the abundance-determination process. The black dots show the observed spectrum. The upper two subpanels show portions of the CH and CN bands with 1σ errors (blue dashed–dotted line). The lower two subpanels show the fitting examples for the Mg 5711 Å and Y 5402 Å lines, with abundance variations for 0.10 and 0.05 dex, respectively.
Paper: The Kinematic and Chemical Properties of the Close-in Planet Host Star 8 UMi
Authors: Huiling Chen, Yang Huang, Wei Zhu, Timothy C. Beers, Renjing Xie, Yutao Zhou, Sharon Xuesong Wang, Wei Wang, Sofya Alexeeva, Qikang Feng, Haozhu Fu, Haining Li, Lile Wang, Huawei Zhang
Figure caption: Left panel: theoretical isochrones of 1.40, 1.70, and 2.35 Gyr (from left to right) and [M/H] = −0.05 in the ﹩{({B}_{{\rm{P}}}-{R}_{{\rm{P}}})}_{0}﹩–M G diagram. The red star with error bars represents 8 UMi. Right panel: the posterior probability density distribution of age calculated by our Bayesian method (see Section 3.1). The red dashed lines of 1.60, 1.90, and 3.05 Gyr represent the 16%, 50%, and 84% cumulative probability levels.
Paper: CLEANing Cygnus A Deep and Fast with R2D2
Authors: Arwa Dabbech, Amir Aghabiglou, Chung San Chu, Yves Wiaux
Figure caption: Cygnus A: reconstructions of uSARA (top) and AIRI (bottom), both displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Their associated residual dirty images are provided in linear scale in panels (a), with standard deviation values 7.2 × 10−4, and 7.4 × 10−4, respectively. Reconstructions are overlaid by zooms on key regions of the radio galaxy: the inner core of Cygnus A in panels (b), the east hotspots in panels (c), and the west hotspots in panels (d), all displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Reconstructions are available in FITS format in the data set Dabbech et al. (2024).
Paper: CLEANing Cygnus A Deep and Fast with R2D2
Authors: Arwa Dabbech, Amir Aghabiglou, Chung San Chu, Yves Wiaux
Figure caption: Cygnus A: reconstructions of MS-CLEAN (negative pixels set to zero for visualization purposes; top) and R2D2 (bottom), both displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Their associated residual dirty images are provided in linear scale in panels (a), with standard deviation values 10.4 × 10−4, and 11.7 × 10−4, respectively. Reconstructions are overlaid by zooms on key regions of the radio galaxy: the inner core of Cygnus A in panels (b), the east hotspots in panels (c), and the west hotspots in panels (d), all displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Reconstructions are available in FITS format in the data set Dabbech et al. (2024).
Paper: CLEANing Cygnus A Deep and Fast with R2D2
Authors: Arwa Dabbech, Amir Aghabiglou, Chung San Chu, Yves Wiaux
Figure caption: Cygnus A: reconstructions of Hö-CLEAN (top) and CS-CLEAN (bottom), displayed in ﹩{\mathrm{log}}_{10}﹩ scale (negative pixels set to zero for visualization purposes). Their associated residual dirty images are provided in linear scale in panels (a), with standard deviation values 359 × 10−4, and 8.6 × 10−4, respectively. Reconstructions are overlaid by zooms on key regions of the radio galaxy: the inner core of Cygnus A in panels (b), the east hotspots in panels (c), and the west hotspots in panels (d), all displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Reconstructions are available in FITS format in the data set Dabbech et al. (2024).
Paper: CLEANing Cygnus A Deep and Fast with R2D2
Authors: Arwa Dabbech, Amir Aghabiglou, Chung San Chu, Yves Wiaux
Figure caption: Cygnus A: reconstructions of R2D2-Net (also the first iteration of R3D3; top), and R3D3 (bottom), both displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Their associated residual dirty images are provided in linear scale in panels (a), with standard deviation values 13.4 × 10−4, and 9.7 × 10−4, respectively. Reconstructions are overlaid by zooms on key regions of the radio galaxy: the inner core of Cygnus A in panels (b), the east hotspots in panels (c), and the west hotspots in panels (d), all displayed in ﹩{\mathrm{log}}_{10}﹩ scale. Reconstructions are available in FITS format in the data set Dabbech et al. (2024).
Paper: Evaporation of Close-in Sub-Neptunes by Cooling White Dwarfs
Authors: Elena Gallo, Andrea Caldiroli, Riccardo Spinelli, Federico Biassoni, Francesco Haardt, Mary Anne Limbach, Juliette Becker, Fred C. Adams
Figure caption: Left: evaporation efficiency (squares, left y-axis) and atmospheric mass-loss rate (circles, right y-axis) as a function of XUV irradiation (bottom x-axis) and/or WD age (top x-axis) for the case of a sub-Neptune-sized planet (8 M ⊕, 2.7 R ⊕) orbiting a 0.61 M ⊙ WD at 0.02 au. The symbol colors trace the WD cooling history (top axis), with T WD varying between 69,000 K (deepest red) and 5,000 K (deepest blue). Right: same as left but for the case of a gas giant (1.24 M J and 1.19 R J).
Paper: Evaporation of Close-in Sub-Neptunes by Cooling White Dwarfs
Authors: Elena Gallo, Andrea Caldiroli, Riccardo Spinelli, Federico Biassoni, Francesco Haardt, Mary Anne Limbach, Juliette Becker, Fred C. Adams
Figure caption: Left: expected evaporation timescales for the sub-Neptune-sized planet simulated in the left panel of Figure 1. The color bar on the right shows the fractional amount of mass lost to hydrodynamic escape as a function of the planet arrival time at 0.02 au (t start) and of the total residence time at this separation (t − t start). The dashed black lines track the locus of the points where the planet would shed 1%, 2%, ...up to 10% of its mass—in the form of a H–He envelope—via hydrodynamic escape. Right: same as left but for the gas giant case in the right panel of Figure 1.
Paper: Evaporation of Close-in Sub-Neptunes by Cooling White Dwarfs
Authors: Elena Gallo, Andrea Caldiroli, Riccardo Spinelli, Federico Biassoni, Francesco Haardt, Mary Anne Limbach, Juliette Becker, Fred C. Adams
Figure caption: Fractional contributions of the total radiative cooling rate (solid blue line) and adiabatic cooling rate (solid green line) with respect to the heating rate (solid red line), shown as a function of the XUV irradiation/WD temperature for the sub-Neptune (left) and gas giant (right). For the latter, the nonmonotonic behavior of the adiabatic cooling is responsible for the nonmonotonic trend of the evaporation efficiency shown in the right panel of Figure 1.
Paper: Tidal Disruption of Planetesimals from an Eccentric Debris Disk Following a White Dwarf Natal Kick
Authors: Tatsuya Akiba, Selah McIntyre, Ann-Marie Madigan
Figure caption: The average mass accretion rate ﹩\dot{M}﹩ from tidal disruption events as a function of the debris disk mass, M disk. The average is calculated from the first 10 Myr of each simulation. The axis on the right shows the corresponding fraction of the debris disk that is tidally disrupted in each case. For simulations with at least one tidal disruption event detection, the results are consistent with a power-law dependence ﹩\dot{M}\propto {({M}_{\mathrm{disk}})}^{2}﹩.
Paper: The Disappearance of the Blue and Luminous Progenitor of the Type IIn SN 2010jl
Authors: Zexi Niu, Ning-Chen Sun, Jifeng Liu
Figure caption: Left and middle: WFC3 images of the SN environment with four different epochs combined together. Both images have the same dimension of 1.″6 × 1.″6 and are centered on the SN position with north up and east to the left. The small circles correspond to the detected point sources for each band within 150 pc of the SN position, and they are color coded in the same way as in the right-hand panel. Right: color–magnitude diagram of the resolved stellar population in the SN vicinity (circles). PARSEC v1.2S single-star isochrones are overplotted, which correspond to the two best-fitting model stellar populations (see text). Sources that can be well fitted by model stellar populations are shown in orange while the overluminous ones are displayed in blue. In addition, we also show the SN progenitor (red star; based on synthetic magnitude from our SED decomposition in Section 3), the late-time behavior of SN 2010jl (green diamonds; which becomes fainter and redder with time), and the field cluster s2 (blue star). The error bars reflect photometric uncertainties.
Paper: The Kinematic and Chemical Properties of the Close-in Planet Host Star 8 UMi
Authors: Huiling Chen, Yang Huang, Wei Zhu, Timothy C. Beers, Renjing Xie, Yutao Zhou, Sharon Xuesong Wang, Wei Wang, Sofya Alexeeva, Qikang Feng, Haozhu Fu, Haining Li, Lile Wang, Huawei Zhang
Figure caption: Left panel: Toomre diagram for 8 UMi (red star). Overplotted background is the distribution of field red clump stars from Huang et al. (2020), color coded by median age with the color bar shown on the right side. The bin size is 5 and 5 km s−1 in the X-axis and Y-axis, respectively. The two dashed circles delineate constant total space velocities with respect to the local standard of rest of V tot = 85 and 180  km s−1, respectively, as commonly used to define a sample of thick-disk stars. The blue contours represent the 10%, 50%, 84%, and 99% of the thin-disk population selected from the field red clump stars, based on the criteria taken from Chen et al. (2021). The red rectangle (V from 5 to 15 km s−1 and ﹩\sqrt{{U}^{2}+{W}^{2}}﹩ from 5 to 20 km s−1) selects stars with similar 3D space velocities to 8 UMi. Right panel: the age distribution of the red clump stars selected by the red rectangle shown in the left panel. Lines of 1.50, 3.50, and 6.50 Gyr mark the 16%, 50%, and 84% cumulative probabilities, respectively.
Paper: The Kinematic and Chemical Properties of the Close-in Planet Host Star 8 UMi
Authors: Huiling Chen, Yang Huang, Wei Zhu, Timothy C. Beers, Renjing Xie, Yutao Zhou, Sharon Xuesong Wang, Wei Wang, Sofya Alexeeva, Qikang Feng, Haozhu Fu, Haining Li, Lile Wang, Huawei Zhang
Figure caption: Left panel: density map for age estimates based on [C/N], using red clump stars taken from Huang et al. (2020). The yellow horizontal region marks the measurement of [C/N] for 8 UMi. The age of 8 UMi is calculated from the probability distribution of the crossed region; the red star indicates the final derived age for 8 UMi. Right panel: the age–[Y/Mg] relation using nearby 72 nearby stars (black dots) taken from Nissen et al. (2020). The blue solid line and dashed lines are the least-squares linear fit and 1σ error for the sample stars. Two binaries and two Na-rich stars are excluded in the fitting (labeled by orange rectangles in the figure; see Section 4.4 of Nissen et al. 2020 for details). The yellow horizontal region marks the measurement of [Y/Mg] for 8 UMi. The red star represents 8 UMi, with age given by the linear relation and errors from the uncertainty of the linear relation and measurement errors of [Y/Mg].
Paper: The Kinematic and Chemical Properties of the Close-in Planet Host Star 8 UMi
Authors: Huiling Chen, Yang Huang, Wei Zhu, Timothy C. Beers, Renjing Xie, Yutao Zhou, Sharon Xuesong Wang, Wei Wang, Sofya Alexeeva, Qikang Feng, Haozhu Fu, Haining Li, Lile Wang, Huawei Zhang
Figure caption: The synthetic line-fitting results (red solid line) of CH, CN, Mg, and Y in the observed solar spectrum (black dots). The solar atmospheric parameters are set to T eff = 5777 K, log g = 4.44, [Fe/H] = 0.00, and v mic = 1.00 km s−1. The upper two panels show the CH and CN band with the observed solar spectrum taken by SOPHIE under HR mode, with abundance variations of 0.10 and 1.00 dex, respectively. Since molecular lines differ between dwarf and giant stars, the CN band is not well reproduced in the solar spectrum. The lower two panels show the fitting of Mg 5711 Å and Y 5402 Å lines with abundance variations of 0.10 and 0.05 dex, respectively.
Paper: Expected Impact of Glints from Space Debris in the LSST
Authors: J. Anthony Tyson, Adam Snyder, Daniel Polin, Meredith L. Rawls, Željko Ivezić
Figure caption: Effect of defocus of small LEO objects (10 cm radius debris) due to the large LSST primary mirror. Top: the simulated surface-brightness cross section of a faint stationary 1 ms glint in a 30 s LSST exposure in blue, an in-focus star of the same net flux (22.7 mag) with PSF size of 0.″73 in green, and the same glint simulated with the added effect of moving across the focal plane in orange, assuming a 500 km altitude orbit. Bottom left: the simulated surface-brightness profile of the faint stationary 1 ms glint in a 30 s LSST exposure. Bottom center: the same glint simulated with the added effect of moving across the focal plane. Bottom right: the in-focus star with PSF size of 0.″73. In this simulation, 1 ADU = 1 electron. The actual LSST matched-filter source-detection process, the PSF convolved with these images, produces the same conclusion. This simulated glint debris assumes an albedo of 0.1; the peak brightness scales linearly with albedo.
Paper: Exploring the Impact of the Aging Effect on Inferred Properties of Solar Coronal Mass Ejections
Authors: F. Regnault, N. Al-Haddad, N. Lugaz, C. J. Farrugia, B. Zhuang, W. Yu, A. Strugarek
Figure caption: Comparison of the CME properties deduced from the temporal profile (in red) and from the spatial profile (in black). From top to bottom, we show the size of the CME in astronomical units, the expansion speed in kilometers per second, and the DiP. All the parameters are a function of heliocentric distance. In the first panel, the purple curve corresponds to a power-law fit. Blue bars show the absolute difference between the parameter deduced from the temporal and spatial profiles relative to the parameter deduced with the spatial profile. For sake of comparison, all the y-axes are set to the same scale.
Paper: Exploring the Impact of the Aging Effect on Inferred Properties of Solar Coronal Mass Ejections
Authors: F. Regnault, N. Al-Haddad, N. Lugaz, C. J. Farrugia, B. Zhuang, W. Yu, A. Strugarek
Figure caption: Synthetic temporal profile (left) and spatial profile of the simulated CME in RTN coordinates. The green and blue areas correspond to the sheath and the ME, respectively. From top to bottom, we show the magnetic field strength and its components in nT, the speed in kilometers per second, and the density in cubic centimeters inverse.
Paper: Exploring the Impact of the Aging Effect on Inferred Properties of Solar Coronal Mass Ejections
Authors: F. Regnault, N. Al-Haddad, N. Lugaz, C. J. Farrugia, B. Zhuang, W. Yu, A. Strugarek
Figure caption: Three-dimensional visualization when the CME reaches 90 R ⊙. The gray color map encodes the magnitude of the speed in the meridional plane. Blue lines are the magnetic field lines plotted from a radial line starting at 57 R ⊙ and ending at 78 R ⊙. The yellow sphere corresponds to the position of the Sun, with a radius of 1 R ⊙. The green circle corresponds to 90 R ⊙.
Paper: Exploring the Impact of the Aging Effect on Inferred Properties of Solar Coronal Mass Ejections
Authors: F. Regnault, N. Al-Haddad, N. Lugaz, C. J. Farrugia, B. Zhuang, W. Yu, A. Strugarek
Figure caption: Left panels: comparison of the temporal and spatial profiles when the CME is at 50, 100, 150 and 200 R ⊙. These profiles are normalized; see main text for more details. The right panel shows the difference between the temporal and spatial profiles as a function of distance. Details are in Section 3.1.