adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology of the Nearby K Dwarf σ Draconis Using the Keck Planet Finder and TESS
Authors: Marc Hon, Daniel Huber, Yaguang Li, Travis S. Metcalfe, Timothy R. Bedding, Joel Ong, Ashley Chontos, Ryan Rubenzahl, Samuel Halverson, Rafael A. García, Hans Kjeldsen, Dennis Stello, Daniel R. Hey, Tiago Campante, Andrew W. Howard, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley D. Baker, Jerry Edelstein, Chris Smith, Benjamin J. Fulton, Josh Walawender, Max Brodheim, Matt Brown, Dwight Chan, Fei Dai, William Deich, Colby Gottschalk, Jason Grillo, Dave Hale, Grant M. Hill, Bradford Holden, Aaron Householder, Howard Isaacson, Yuzo Ishikawa, Sharon R. Jelinsky, Marc Kassis, Stephen Kaye, Russ Laher, Kyle Lanclos, Chien-Hsiu Lee, Scott Lilley, Ben McCarney, Timothy N. Miller, Joel Payne, Erik A. Petigura, Claire Poppett, Michael Raffanti, Constance Rockosi, Dale Sanford, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Roger Smith, Jim Thorne, John Valliant, Adam Vandenberg, Shin Ywan Wang, Edward Wishnow, Truman Wold, Sherry Yeh, Ashley Baker, Sarbani Basu, Megan Bedell, Heather M. Cegla, Ian Crossfield, Courtney Dressing, Xavier Dumusque, Heather Knutson, Dimitri Mawet, John O'Meara, Guđmundur Stefánsson, Johanna Teske, Gautam Vasisht, Sharon Xuesong Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Left: observations of σ Dra from TESS Sector 41–60 photometry in black and from KPF RVs in purple. The inset is a zoom-in of the RV time series spanning 7 hr on 2023 June 20. Right: RV amplitude spectrum of σ Dra, in which a power excess corresponding to solar-like oscillations can be seen at frequencies ∼4000−6000 μHz.
Paper: The Diffusion Tensor of Protons at 1 au: Comparing Simulation, Observation, and Theory
Authors: P. L. Els, N. E. Engelbrecht, J. T. Lang, R. D. Strauss
Figure caption: Schematic of the slab (red line) and 2D (blue line) spectra employed in the simulations presented here. The x-axis denotes length and wavenumber and is to scale for nominal length scale parameters as listed in Table 1, which also provides an index of the symbols used. The bottom numeric values indicate length, and the top variables are for the corresponding wavenumbers. The y-axis is not to scale. The black horizontal bar denotes the range of proton maximal Larmor radii corresponding to the particle energies considered in this study.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: (a) Field lines plotted over the active region magnetogram with B  z  component on the background in gray scale; (1) cyan color twisted field lines over the base of the jet region, and (2) random field lines (white) over the active region. Panel (b) shows the loops in the 171 Å channel near the active region at the same instance. The green color box in panel (a) represents the field lines constituting the flux rope whose zoomed-in version is plotted in panel (c) with Direct Volume Rendering (DVR) of the twist (T  w ) parameter indicating a maximum value along the rope exceeding unity. The inset here is a cutout of the magnetogram shown in Figure 2 left panel. The green lines inside the inset mark the locations of the PILs, and the magenta arrow points toward the region where the flux rope is detected. The bald patch is highlighted in a black box in panel (a) and the field lines surrounding it are plotted in panel (d) with a distribution of squashing factor or Q map on the background. Regions with high Q value are found along the footpoints of the bald patch. We can also see the bald patch from a flipped side in the inset of panel (d).
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Left panel: magnetogram of AR12280 at 20:24 UT with the same field of view as Figure 1. Notably, magnetogram at this timestamp is used for extrapolation further. Right panel: magnetogram at 20:36 UT, close to onset phase of the jet, as marked in panel (b) of Figure 1. The blue and red arrows represent the vector plots of positive and negative transverse components over the B  z  component in gray ranging from (−800 G, 800 G). The green contours show the polarity inversion lines. The black box denotes the jet base region and the white box covers the bright point region.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Progress of the angle between the flow vector and (1) the magnetic field (solid line) and (2) Lorentz force (dashed line). In both cases, θ is seen to approach 90◦, implying the action of plasma flow and Lorentz force on the untwisting of the flux rope field lines. This further supplements the orientation of  v  and  J  ×  B  around the flux rope depicted in the second column of Figure 8.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Evolution of orientations of Lorentz force (blue arrow) and plasma flow (yellow arrow) to the flux rope (in red color field lines) at a fixed location until the time period coverage as Figure 8. Initially, the Lorentz force pushes the field lines helping in untwisting it. Important to note is the direction of Lorentz force remaining nearly aligned with the flux rope axis toward the end. Both Lorentz force and flow remain perpendicular to the field line at the end, complementing the profile of angles calculated in Figure 10.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Evolution of EM-weighted log(T) over the active region until the growth of the jet region. Like Figure 1, the panel (a) denotes the state before the onset of the transients. Panel (b) marks the bright point region in the white box and panel (c) shows the hot loops in the flux rope eruption region which also comprises of the base part of the jet.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Time evolution of EM-weighted temperature near the jet base and bright point regions from DEM analysis. The left panel displays the total emission measure map within the ROIs at 20:50:37 UT. The regions under black and red boxes are utilized to determine the average temperature in the right panel. There is a sharp increase in the maximum temperature near the bright point region than the jet base.
Paper: Exploring the Magnetic and Thermal Evolution of a Coronal Jet
Authors: Sushree S. Nayak, Samrat Sen, Arpit Kumar Shrivastav, R. Bhattacharyya, P. S. Athiray
Figure caption: Variation of the magnitude of average magnetic field (∣ B ∣), current density (∣ J ∣), and Lorentz force (∣ J  ×  B ∣) over height in logarithmic scale.
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Spectra corresponding to the two fits on the right-hand side of Figures 4 and 5. The faint gray lines are the raw spectra, and the solid black lines are smoothed with a Gaussian kernel. Spectra are de-redshifted into the rest frame based on the reported z spec. Central wavelengths of Balmer lines are overplotted in both panels. Oxygen emission lines are overplotted in the top panel only. Top panel: spectrum for the galaxy with the largest ∣Δ z ∣ (top right of Figures 4 and 5). Bottom panel: spectrum for the X-ray-detected example galaxy with ∣Δ z ∣ > 0.15 (bottom right of Figures 4 and 5).
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Absolute error in ﹩\mathrm{ln}P({\boldsymbol{\vartheta }})﹩ for different configurations of the Hutchinson trace estimator. Deviations are computed relative to a directly computed ﹩\mathrm{ln}{P}_{\mathrm{ref}}({\boldsymbol{\vartheta }})﹩ with atol = rtol = 10−5. Upper panel shows the time taken for 256,000 prior evaluations using each configuration. Horizontal lines show the direct solution with different tolerances.
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Average function evaluation time vs. batch size (i.e., number of  ϑ  draws passed to the function) for the dominant functions in our log-posterior evaluation. Times are in GPU-sec and correspond to an NVIDIA A100 GPU.
Paper:  pop-cosmos: Scaleable Inference of Galaxy Properties and Redshifts with a Data-driven Population Model
Authors: Stephen Thorp, Justin Alsing, Hiranya V. Peiris, Sinan Deger, Daniel J. Mortlock, Boris Leistedt, Joel Leja, Arthur Loureiro
Figure caption: Median size of the fractional error on P( ϑ ), binned by ﹩\mathrm{ln}{P}_{\mathrm{ref}}({\boldsymbol{\vartheta }})﹩ for a range of solver tolerances.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: The average rotational profiles of all AIA channels starting from the chromosphere to the corona, along with the results from (1) H. B. Snodgrass (1984), (2) B. K. Jha et al. (2021), and (3) D. K. Mishra et al. (2024).
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: The variation in rotational parameters equatorial rotation rate (A) and latitudinal gradient (B) from the interior to the atmosphere (highlighted in gray) of the Sun as a function of radius (top panel; (a) and (b)) and logarithmic temperature (bottom panel; (c) and (d)), as obtained from this study, (1) D. K. Mishra et al. (2024), (2) B. K. Jha et al. (2021), and helioseismology. The height representative of Ca II K plages is obtained from M. Stix (1976), while the logarithmic temperature is obtained from H. A. Beebe (1971).
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: The variation in rotational constants with the progression of cycles 24 and 25 compared with the sunspot number. The shaded area in each color represents the uncertainty in determining the respective parameters.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: Panels (a) and (b) depict an example pair of images, temporally separated by 6 hr, after projection onto the heliographic grid. Red rectangular boxes in (a) and (b) represent the selected bands (B1 and B2) for cross-correlation, spanning −20° to −5° in latitude and ±45° in longitude in this example.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: The trend in (a) equatorial rotation rate (A), and (b) differential gradient (B) with increasing height above the photosphere. All error bars in the y-axes correspond to the uncertainty pertained in determining the parameters A and B, whereas the error bars along the x-axis correspond to the errors as determined by the original studies as listed in Table 1. The variation in (c) equatorial rotation rates and (d) differential gradients of the solar atmosphere as obtained with temperature.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: An example pair of images showing the effectiveness of Gaussian smoothing. (a) The Level 1.5 data from 1600 Å with small-scale brightenings, network bright points, and fracture in plage regions. (b) The data after smoothing, as a result of convolution with a Gaussian kernel.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: Comparison of the rotational profile at the depth of (a) 0.94 R ⊙, with that obtained for 171 Å and 304 Å, and (b) 1600 Å with 0.965 R ⊙ at all latitudes.
Paper: Exploring the Dynamic Rotational Profile of the Hotter Solar Atmosphere: A Multiwavelength Approach Using SDO/AIA Data
Authors: Srinjana Routh, Bibhuti Kumar Jha, Dibya Kirti Mishra, Tom Van Doorsselaere, Vaibhav Pant, Subhamoy Chatterjee, Dipankar Banerjee
Figure caption: A representative plot of the rotational profiles obtained from helioseismological data assuming a symmetric distribution of rotation rates in both hemispheres.
Paper: Visible Opacities of S-type Stars: The d 3Φ–a 3Δ Band System of ZrO
Authors: Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Ab initio TDM curve (real form) for the d 3Φ–a 3Δ transition of ZrO calculated in this work, by S. R. Langhoff & C. W. Bauschlicher Jr. (1990), and by A. N. Perri et al. (2023). The y-axis is in atomic units (a.u.) with 1 a.u. = 2.542 D.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible Opacities of S-type Stars: The d 3Φ–a 3Δ Band System of ZrO
Authors: Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: An overview of the ZrO spectrum (red, upward) and simulation (downward) showing d 3Φ–a 3Δ (blue) from this analysis and B 1Π–X 1Σ+ (black) from P. F. Bernath et al. (2024).
Paper: Visible Opacities of S-type Stars: The d 3Φ–a 3Δ Band System of ZrO
Authors: Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: A comparison between the line positions from this study and those from A. N. Perri et al. (2023) is presented for the 0–0, 1–1, 2–2, 3–3, 4–3, and 4–5 bands of the ZrO d 3Φ–a 3Δ transition. The y-axis shows the difference between the line positions from PGOPHER and A. N. Perri et al. (2023) in cm−1, while the x-axis represents the rotational quantum number (J).
Paper: Visible Opacities of S-type Stars: The d 3Φ–a 3Δ Band System of ZrO
Authors: Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: Overview emission spectrum of ZrO (red, upward) and simulation (downward)) of Δv = 0 bands of the d 3Φ–a 3Δ transition of ZrO (blue: 0–0 band, green: 1–1 band, purple: 2–2 band, orange: 3–3 band, and red: 4–4 band).
Paper: Visible Opacities of S-type Stars: The d 3Φ–a 3Δ Band System of ZrO
Authors: Peter F. Bernath, Manish Bhusal, Jacques Liévin
Figure caption: The spectrum of ZrO (upward) and simulation (downward) for the 3Φ3–3Δ2 subband of the 0–0 band of the d 3Φ–a 3Δ transition.
Paper: Detecting Detached Black Hole Binaries through Photometric Variability
Authors: Chirag Chawla, Sourav Chatterjee, Neev Shah, Katelyn Breivik
Figure caption: Same as Figure 11 but for the BH–LCs in our delayed model.
Paper: Hydrodynamic 3D Simulation of Roche Lobe Overflow in High-mass X-Ray Binaries
Authors: David Dickson
Figure caption: System ecliptic mapped with equipotential lines in black. Streamline arrows indicate flow pattern extending from the L1 point. Colored contours have been provided to map the transonic region. Accretion disk bands separated by the lower density gap are shown by density gradient.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for grains with astronomical silicate optical properties and a fractal dimension of 1.8. Values are computed for M = M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. Values are computed based on a 0.3 fractional conversion of the silicon and each point within the contour plot represents the same amount of condensable material.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Using the optical properties of aggregates of astronomical silicate grains as presented in this paper, and the aggregate distributions produced by solving the discrete Smoluchowski equation (as described in J. A. Paquette et al. 2023), the ratio of the radiation pressure force to gravity is calculated and plotted here. Results are presented for different values of the SiO sticking efficiency.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for astronomical silicate with a fractal dimension of 1.8. Values are computed for M = M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. The contour lines represent the location of the point where Γ = 1 and the corresponding fractional conversion of silicon is listed on the contour line.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for astronomical silicate with a fractal dimension of 2.8. Values are computed for M = M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. The contour lines represent the location of the point where Γ = 1 and the corresponding fractional conversion of silicon is listed on the contour line.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Variation in radiative pressure opacity with increasing aggregate size for astronomical silicate. The aggregate radiative pressure opacity per gram, κ agg, is scaled via the product of the number of primary particles in the aggregate, N, and the radiative pressure of a single primary particle, κ primary. Data are shown for both fractal dimensions of 1.8 and 2.8 and primary particle radii of (a) 0.01, (b) 0.05, (c) 0.1, and (d) 0.3 μm, and calculated at a wavelength of 1.0 μm.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Comparison between MSTM computed opacity data and MMF theory for forsterite for D  f  = 1.8.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Comparison between MSTM computed opacity data and MMF theory for astronomical silicate for D  f  = 1.8.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Comparison between MSTM computed opacity data and MMF theory for forsterite for D  f  = 2.8.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Comparison between MSTM computed opacity data and MMF theory for astronomical silicate for D  f  = 2.8.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Measured RMPSR of each low-latitude pulsar in our sample in the Local Arm region, except those in and beyond the Gum Nebula. The black dotted curves delineate the nominal inner and outer boundaries of the (magnetic) Local Arm derived from our analyses. A Perseus-to-Sagittarius Interarm region (not shown) is presumed to extend below the low-longitude end of the Local Arm (see Section 4.6). We model the magnetic field within the Local Arm to be parallel to our Local Arm’s outer boundary. The black cross at (x, y) = (0.0, 8.3) marks the location of the solar system.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Left: the geometrically corrected δRMSag as a function of Galactic longitude for the Sagittarius Arm pulsars of Figure 4. Right: same as the left panel, except that the magnetic field (positive is CCW) along the arm is displayed. Pulsar LOSs at negative (nonnegative) Galactic latitudes are shown with red (blue) symbols. Outliers are denoted with a cross and listed in Table 3.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Same as Figure 2, but for the Sagittarius Arm. The dotted–dashed line represents the Galactic longitude limit below which the LOS would also sample the next inward region, the Sagittarius-to-Scutum Interarm.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Left: geometrically corrected δRMLocal as a function of δDMLocal for the Local Arm pulsars shown in Figure 2 with negative Galactic latitudes. Right: same as the left panel, but for pulsars with positive Galactic latitudes. In each case, we show the best linear fit to the respective values. Outliers are shown with crosses, with details listed in Table 3.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Here, Γ is the ratio of the radiation pressure force to gravity for the entire aggregate distribution and Γ1 is the ratio of the radiation pressure force to gravity for single grains. Thus, the ratio of ratios Γ1/Γ is the strength of the contribution from single grains to that from the entire distribution. This is plotted for the same five values of the sticking coefficient used in the previous figure. Initially, the push from single grains is the entirety of the push as aggregates have not yet begun to form, but eventually the push from aggregates dominates the push from single grains.
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Locations of all low-latitude (∣b∣ ≤ 9°) pulsars measured and tabulated in J. Rankin et al. (2023). The solar system is marked by the black cross at (x, y) = (0.0, 8.3) kpc. The plotted locations of the spiral arm centers are from YMW17 (J. M. Yao et al. 2017).