adsabs/AstroCLIMB huggingface dataset:
Paper: Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
Authors: Ken-ichi Tadaki, Tadayuki Kodama, Yusei Koyama, Tomoko L. Suzuki, Ikki Mitsuhashi, Ryota Ikeda
Figure caption: Stellar mass vs. SFR for our ALMA sample of 10 massive SFGs at z ∼ 2.2–2.5 (magenta pentagons), the T20 sample with ALMA 870 μm data (blue circles), and all galaxies at 1.9 < z < 2.6 (gray dots) taken from the 3D-HST catalog (Skelton et al. 2014; Momcheva et al. 2016). The shaded region indicates the range of ±0.4 dex from the star formation main sequence at z ∼ 2 (Whitaker et al. 2014).
Paper: Is the M81 Fast Radio Burst Host Globular Cluster Special?
Authors: Kristen C. Dage, Arash Bahramian, Clancy W. James, Arunav Kundu, Katherine L. Rhode, Jay Strader, Enrico Vesperini, Stephen E. Zepf
Figure caption: Left: Digital Sky Survey (DSS) R band image of M81. Positions of globular clusters from NH11 considered in this work are shown by cyan circles. The cyan rectangle indicates the area around the FRB GC, plotted in the middle and right panels. Middle and right: a composite color image of the vicinity of the FRB GC (middle) and a zoom-in on the cluster (right) based on HST images in F814W (red), F606W (green), and F435W (blue).
Paper: Is the M81 Fast Radio Burst Host Globular Cluster Special?
Authors: Kristen C. Dage, Arash Bahramian, Clancy W. James, Arunav Kundu, Katherine L. Rhode, Jay Strader, Enrico Vesperini, Stephen E. Zepf
Figure caption: Scatterplot of half-light radii vs. absolute magnitude for globular clusters in the Milky Way and M81, in the context of star clusters and dwarf galaxies (e.g., see Tolstoy et al. 2009). Core-collapsed globular clusters in the Milky Way are denoted by hollow circles, and globular clusters in M81 with bright X-ray sources are denoted with black margins. The FRB GC in M81 does not appear to be exceptional in its properties compared to these other cluster populations.
Paper: Is the M81 Fast Radio Burst Host Globular Cluster Special?
Authors: Kristen C. Dage, Arash Bahramian, Clancy W. James, Arunav Kundu, Katherine L. Rhode, Jay Strader, Enrico Vesperini, Stephen E. Zepf
Figure caption: Relative encounter rates for globular clusters as they would be observed in the M81 system, normalized assuming 47 Tuc has an encounter rate of 1000.
Paper: Is the M81 Fast Radio Burst Host Globular Cluster Special?
Authors: Kristen C. Dage, Arash Bahramian, Clancy W. James, Arunav Kundu, Katherine L. Rhode, Jay Strader, Enrico Vesperini, Stephen E. Zepf
Figure caption: Original (left) and residual (right) images with the best-fitting King model subtracted. The large number of resolved giants, including near the center of the cluster, are evident.
Paper: Dwindling Surface Cooling of a Rotating Jovian Planet Leads to a Convection Zone That Grows to a Finite Depth
Authors: Bradley W. Hindman, J. R. Fuentes
Figure caption: Panel (a): radiant luminosity L as a function of time for a MESA model of a Jupiter-like planet (Marleau & Cumming 2014) that undergoes cooling for 5 Gyr (black solid line) and for an analytic model where L ∝ t −1 (dashed red line). Panel (b): depth of the convection zone of Jupiter as a function of time for the analytic models described by Equations (16) and (17) and using the parameter values that appear in Table 1. The convection zone in a nonrotating Jupiter deepens rapidly engulfing the entire interior of the planet in less than 105 yr. Conversely, the convection zone in a rotating giant planet initially grows, but asymptotes to a finite depth. For parameter values appropriate for Jupiter, the convection zone stops growing after it occupies the outer 37% of the planetary radius.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Sections of the continuum-subtracted infrared water spectra of the compact disk GK Tau (in black) and the large disk CI Tau (in gray), at the top from Spitzer-IRS (offset by 0.15 Jy) and in the middle from JWST-MIRI. A broader range of the spectrum is shown in Figure 10 in Appendix B. The CI Tau spectrum is scaled to the distance of GK Tau and corrected for the different accretion luminosity (Section 3). The subtraction of the two spectra is shown in brown at the bottom, with the single-temperature LTE model (blue area) from Figure 5 and Table 2. Vertical labels show the upper level energy E  u  in kelvins, separated into higher energy (>4000 K) in red and lower energy (<4000 K) in blue.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Overview of excess cool components in compact disks by using water spectra in large disks as reference templates for the hotter inner component, as explained in Section 3. The orange area in the top panels is the high-energy line luminosity ratio expected from using the correlation with L acc shown in Figure 3 (3σ region). The red dashed line is the median value of the line luminosity ratio at E  u  ∼ 6000–9000 K. The data point color gradient reflects the E  u  value (x-axis) of each water line. A single-temperature LTE fit to line fluxes measured in the excess cool component is shown in gray in the middle (line flux residuals) and bottom (population diagram) panels, with parameters shown in the inset.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Broader view of the excess cool component in rotational water emission in GK Tau, using CI Tau as a template for the hot component as in Figure 4. The same scaling and subtraction procedure described in Section 3 is applied here, where residuals after subtraction are shown in brown for MIRI (top three panels) and IRS (bottom panel). A two-temperature fit is shown in blue (only the T ≈ 400 K component) and cyan (the T ≈ 400 and 170 K components together), with best-fit values as reported in Appendix B. The dashed box marks the two MIRI lines discussed in the text. Other molecules are reported and labeled in different colors for reference.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Illustration of the interpretation of the results in the context of the long-proposed scenario of inner water enrichment by pebble drift (Cyr et al. 1998; Ciesla & Cuzzi 2006). The zoomed-in insets show the main processes of pebble drift, ice sublimation, and vapor diffusion as included in recent model explorations by Kalyaan et al. (2021, 2023) in the context of how ice delivery and inner disk water enrichment may be regulated by dust gaps (pebble traps) observed with ALMA.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Correlations with dust disk radius R disk for the luminosity ratio between resolved water low- and high-energy lines in MIRI (left), resolved water low-energy lines and the 14 μm HCN band in MIRI (middle), and blended water low-energy lines in Spitzer near 30 μm (taken from Figure 9 in Banzatti et al. 2023, excluding disks with large inner dust cavities).
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Single-temperature LTE fits to the high-energy lines that dominate water spectra at 12–16 μm. Best-fit parameters are reported in Table 2. Representative models of organics and OH emission are reported for reference at the bottom.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Stacked P5–P18 line profiles of CO rovibrational fundamental emission observed in the four targets from iSHELL and CRIRES spectra in Banzatti et al. (2022), Brown et al. (2012), and this work. The stellar RV is marked with a dashed line, and the gaps on the blue side of each line are due to telluric lines at the time of observation.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: ALMA images for the sample ordered by disk radius from Long et al. (2019).
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Eruptive prominence as detected by Metis VL channel on 2021 April 26 at 01:05 UT (upper panels—Stokes I, Q, U); on middle panels, Stokes I, Q, U are shown on 2021 April 25 at 15:05 UT as the pre-event image. Lower panels show the prominence observation with pre-event corona subtracted. Note that three Stokes images are shown with different contrasts in order to enhance structures of interest, but they have been obtained within the same field of view.
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Selected brightest pixels in Stokes I within two prominence arms, which we denote “northern” and “southern.” In the zoomed-in panel, the most intense northern pixel, studied in detail, is marked by a green square.
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Height variations of I, Q, and U through the brightest pixels shown by orange crosses in Figure 3.
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Position of the Solar Orbiter during prominence observations.
Paper: Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
Authors: Ken-ichi Tadaki, Tadayuki Kodama, Yusei Koyama, Tomoko L. Suzuki, Ikki Mitsuhashi, Ryota Ikeda
Figure caption: Size comparisons between the CO, 870 μm, and 4.4 μm emissions for eight massive SFGs (magenta pentagons). The solid lines show the 1:1 correspondence between the circularized effective radii compared. Blue circles indicate the T20 sample with ALMA 870 μm and JWST 4.4 μm data, but without CO data.
Paper: Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
Authors: Ken-ichi Tadaki, Tadayuki Kodama, Yusei Koyama, Tomoko L. Suzuki, Ikki Mitsuhashi, Ryota Ikeda
Figure caption: Best-fit model radial profiles of sSFR, gas-depletion timescale, and gas-mass fraction. Solid red lines and shaded region show the average and standard deviation in eight massive SFGs, respectively. Black dashed lines show the individual models.
Paper: Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
Authors: Ken-ichi Tadaki, Tadayuki Kodama, Yusei Koyama, Tomoko L. Suzuki, Ikki Mitsuhashi, Ryota Ikeda
Figure caption: Normalized visibility amplitudes vs. uv distances for our sample of 10 massive SFGs. Magenta and cyan symbols show 870 μm and CO data, respectively. Dashed lines indicate the best-fitting model for exponential profile.
Paper: Dwindling Surface Cooling of a Rotating Jovian Planet Leads to a Convection Zone That Grows to a Finite Depth
Authors: Bradley W. Hindman, J. R. Fuentes
Figure caption: Isocountours of the asymptotic depth of the convection zone within a rotating planet with a surface cooling rate that varies like ∼t −1. The asymptotic depth is shown as a function of the buoyancy frequency N of the stably stratified interior and the planet's rotation rate Ω. To ease interpretation, we have indicating the rotation rate of Jupiter with the dotted horizontal line. The two blue dashed lines provide isocontours for h ∞ = 10−2 R J and for h ∞ = 10−1 R J. The red shaded region indicates all values consistent with current constraints for Jupiter's outer convection zone h ∞ ∈ [0.3 R J, 0.5 R J] (e.g., Militzer et al. 2022). All isocontours were calculated using Equation (17) and Table 1.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: The distribution of upper level energies E  u  and Einstein-A coefficients (top panels, with color-coding reflecting E  u  values) across infrared wavelengths naturally traces radial temperature gradients in inner disks within and across the water snow line (bottom panel, where the spectrum is scaled to a distance of 130 pc). This figure is partly adapted from Figure 1 in Blevins et al. (2016) and Figure 13 in Banzatti et al. (2023). The MIRI lines used in the analysis in Section 3 are marked with black circles.
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: Correlations between water line luminosities and accretion luminosity. Left: using blended water lines at 17.1–17.4 μm from Spitzer-IRS (data and regression adopted from Banzatti et al. 2020). Middle: using high-energy (6000–8000 K) water lines from JWST-MIRI from this work and Paper I. Right: using low-energy (900–3000 K) water lines (see Figure 1).
Paper: AC Her: Evidence of the First Polar Circumbinary Planet
Authors: Rebecca G. Martin, Stephen H. Lubow, David Vallet, Narsireddy Anugu, Douglas R. Gies
Figure caption: 3D visualizations showing two different views of the AC Her binary system with a polar circumbinary disk. The disk has two parts that are separated by the gap that the putative planet has cleared out. The orbital radius of the planet is shown at 8 a b (Section 3). The outer disk (dark red) is the gas and dust disk that is observed (Section 2). The outer edge of the observed disk extends beyond what is shown in the figure. The possible inner disk (light red) is a dust depleted disk that has not been observed (Section 3). The inner disk is shown to extend from 1.6 a b to 7 a b. The post-AGB star (magenta sphere) and the companion (yellow sphere) are shown at apastron separation. The binary orbits are to scale relative to each other but the sizes of the stars and the planet are not. The left panel shows a view with the disk almost edge on and right panel shows the observed view in the plane of the sky. AC Her is located at a distance of 1402 pc (Gaia Collaboration et al. 2016). The observationally inferred binary semimajor axis is a b = 2.01 mas = 2.83 au (Anugu et al. 2023).
Paper: JWST Reveals Excess Cool Water near the Snow Line in Compact Disks, Consistent with Pebble Drift
Authors: Andrea Banzatti, Klaus M. Pontoppidan, John S. Carr, Evan Jellison, Ilaria Pascucci, Joan R. Najita, Carlos E. Muñoz-Romero, Karin I. Öberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin A. Bergin, Nicholas P. Ballering, Michael R. Meyer, Simon Bruderer
Figure caption: JWST-MIRI-MRS spectra for the four disks. For clarity, the spectra are offset vertically by the following additive shifts: 0.05 Jy in CI Tau, 0.17 Jy in GK Tau, and 0.4 Jy in HP Tau. Illustrative models of molecular emission are shown for guidance at the bottom. Prominent dust features are approximately identified and marked with shaded regions. The estimated continuum that is subtracted before analyzing the water spectra is shown in red on each spectrum. Two ALMA images are shown on the right for reference regarding disk sizes and structures (the whole sample is included in Appendix A).
Paper: AC Her: Evidence of the First Polar Circumbinary Planet
Authors: Rebecca G. Martin, Stephen H. Lubow, David Vallet, Narsireddy Anugu, Douglas R. Gies
Figure caption: The contours show the inclination of the disk relative to the binary angular momentum vector (i bd, left) and relative to the binary eccentricity vector (i polar, right) as a function of the observed disk inclination i d and longitude of ascending node Ωd. The red crosses show the possible disk parameters from Hillen et al. (2015). The black points on the left panel show a coplanar disk (i bd = 0°, lower point) and a retrograde coplanar disk (i bd = 180°, upper point). The black points on the right panel show a polar aligned disk (i bd = Ωbd = 90°, lower point) and an antipolar aligned disk (i bd = 90° and Ωbd = 270°, upper point).
Paper: Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: (Top) Contours of the ion VDF f  i  at t ≈ 5τ A (white lines and color map) and the t ≈ 18τ A (red lines). Dotted vertical lines highlight w ∥ = 0 and w ∥ = v A. The red contour levels are chosen to emphasize changes in f  i  and do not correspond to the white contours (see text). (Bottom) f  i  vs. distance s along the oblique-ICW resonant contour shown with the black line in the top panel (s = 0 at w ∥ = 0). Colors are as in Figure 3(a). The thin black line is flat (﹩{{ \mathcal G }}_{\mathrm{res}}[{f}_{i}]=0﹩), while the dashed line shows an f  i  that is independent of w ⊥ (as expected from stochastic heating).
Paper: Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: (Left) Time evolution of the perpendicular diffusion energy coefficient ﹩{D}_{\perp \perp }^{E}﹩, showing the transition from the quasi-linear expectation ﹩{D}_{\perp \perp }^{E}\propto {w}_{\perp }^{2}﹩ to a flatter profile around t ≳ 11τ A. The inset shows the normalized perpendicular (orange) and parallel (purple) ion heating rates, illustrating a sharp drop in Q ⊥,i  associated with the change in ﹩{D}_{\perp \perp }^{E}﹩, while Q ∥,i  remains almost constant. (Right) Differential heating rates, ﹩{v}_{\mathrm{th}0}^{2}{\varepsilon }^{-1}{\partial }^{2}{Q}_{\perp ,\parallel ,i}/\partial {w}_{\perp }\partial {w}_{\parallel }﹩, computed from 〈 E  ⊥,∥  ·   w  ⊥,∥〉. The Q ⊥ profile (panels (b) and (c)) exhibits resonant structure at early times (top); the shaded region shows ﹩{w}_{\parallel \mathrm{res}}﹩ for oblique ICWs with ﹩{d}_{i}^{-1}\lt {k}_{\parallel }\lt 2{d}_{i}^{-1}﹩, around where there is a sharp drop-off in wave power (Figure 4). By late times it drops significantly and an ill-defined peak around w ⊥ ≃ v th appears, reminiscent of stochastic heating. The Q ∥ profile (panels (d) and (e)) maintains its structure, although spreads out modestly (accounting partially for its lower values).