adsabs/AstroCLIMB huggingface dataset:
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: SMHM relation for all galaxies in the catalog at different redshifts: z = 0, top left; z = 1, top right; z = 2, bottom left; z = 3, bottom right. The color of the dots represents the sSFR. The big red circle and square represent the evolution of two example galaxies. The solid red line represents the abundance matching relation at z = 0, while the gray dashed line the derived average M H–M ⋆ relation at the specific redshift of the panel. The SMHM is an output of our model.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Total stellar mass function evolution with redshift: blue z = 0, orange z = 1, green z = 2, red z = 3, and magenta z = 5. Histograms are the SMF for surviving haloes; dashed lines are the total SMF reconstructed from our catalog, and solid lines are the fit by Davidzon et al. (2017). Our model is able to well reproduce the evolution of SMF up to z ∼ 5.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: sSFR–sHAR relation from abundance matching. Colors are as in Figure 1.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Example of evolution of two mock galaxies. Black line, halo mass; red line, stellar mass; green line, SFR in M ⊙ Gyr−1. Top panel shows a quenched galaxy, which formed all its stellar mass at z > 2 with large SFR; bottom panel, a star-forming one with low and prolonged SFR.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Bulge stellar mass function. Solid lines are model predictions; dots are GAMA data. In blue, the total bulge stellar mass function; in orange, the stellar mass function for ellipticals.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: sSFR distribution from the convolution of the SMF of active galaxies and the main sequence. Colors are as in Figure 1.
Paper: NuSTAR Observations of Four Mid-IR–Selected Dual AGN Candidates in Galaxy Mergers
Authors: Ryan W. Pfeifle, Kimberly Weaver, Shobita Satyapal, Claudio Ricci, Nathan J. Secrest, Mario Gliozzi, Laura Blecha, Barry Rothberg
Figure caption: Comparing the intrinsic AGN 12 μm luminosity to the total observed 2–10 keV luminosity. The intrinsic AGN 12 μm luminosity (derived via SED fitting) is given on the abscissa, and the total observed 2–10 keV luminosity is given on the ordinate. Mid-IR–selected mergers from Satyapal et al. (2017) and Pfeifle et al. (2019b) are shown as blue squares; mergers examined in this work with NuSTAR that hence have 2–10 keV luminosities derived from NuSTAR are shown in orange, where inverted triangles indicate upper limits, and the circle indicates J0841+0101, the only source detected by NuSTAR. Vertical lines connect sources observed with Chandra and NuSTAR. For comparison, we underlay the observed 2–10 keV X-ray and intrinsic AGN 12 μm luminosities from the Swift-BAT sample drawn from Ricci et al. (2017b) and Ichikawa et al. (2017, 2019); the column densities of the Swift-BAT sample are displayed through the auxiliary color map. The dashed line indicates the expected relation for unobscured AGNs from Asmus et al. (2015), while the dotted line indicates the ratio at which we expect the AGNs to be heavily obscured (Pfeifle et al. 2022).
Paper: NuSTAR Observations of Four Mid-IR–Selected Dual AGN Candidates in Galaxy Mergers
Authors: Ryan W. Pfeifle, Kimberly Weaver, Shobita Satyapal, Claudio Ricci, Nathan J. Secrest, Mario Gliozzi, Laura Blecha, Barry Rothberg
Figure caption: The SDSS r-band and NuSTAR FPMA imaging for (top to bottom) J0122+0100, J0841+0101, J1221+1137, and J1306+0735. Left to right: SDSS r-band and NuSTAR FPMA 3–10, 10–24, and 3–24 keV bands. We smoothed the X-ray images with a 3 pixel Gaussian kernel and used the perceptually uniform sequential color map “magma” in MATPLOTLIB. Dashed 45″ radius circles represent the source extraction regions. The scale bar in the bottom right corner of each panel indicates an angular size of 60″.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: The left panel shows the mass accretion rate onto the black hole in units of the Bondi rate as a function of parameter s. The light green square, the dark green circle, and the blue triangles represent the mass accretion rates onto the black hole for l = 2, l = 1, and l = 0, respectively. The black hexagram shows the value of the mass accretion rate in the absence of outflows. The adiabatic index γ = 5/3 is adopted in the calculations. The right panel shows the variation in the radial velocity for three solutions l = 2, l = 1, and l = 0. The color bar shows the pressure of an accretion flow.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Mass accretion rate of the black hole in units of ﹩{\dot{M}}_{E}﹩ as a function of the temperature at the outer boundary T out. The density at the outer boundary is considered ρ 0 = 10−24gr/cm3. Solutions are for L = 85, α = 0.1, r out = 3r  B , and γ = 5/3.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Mass accretion rate as a function of parameters s and L. Left panel: mass accretion rate in the outer boundary ﹩{\dot{M}}_{\mathrm{out}}﹩. Right panel: Mass accretion rate onto the black hole ﹩{\dot{M}}_{\mathrm{BH}}﹩. In each panel, the horizontal axis displays the strength of the outflow, the vertical axis shows the angular momentum at the outer boundary, and the color bar represents the mass accretion rate. The darker shaded areas have lower mass accretion rates, and the lighter colors have larger mass accretion rates.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Left panel: mass accretion rate onto a BH as a function of the exponent s for different values of η, plotted for L = 85, l = 1 α = 0.1, γ = 5/3, and T out = 6.5 × 106 K. The color bar shows the specific angular momentum that is swallowed by the black hole. Right panel: mass accretion rate at the outer boundary as a function of the exponent s. The color bar shows the location of the sonic point.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Radial variation in the relative thickness of the flow H/r for s = 0, s = 0.2, and 0.4. The vertical dotted line indicates the location of the Bondi radius. The solutions are for L = 85, α = 0.1, γ = 5/3 and T out = 6.5 × 106 K, η = 1, r out = r  B . The color bar shows the density of the accretion flow.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: For L = 85, α = 0.1, γ = 5/3 and T out = 6.5 × 106 K, η = 1,. The comparison of the power (left) and momentum flux (right) of the outflow in the hot (Violet lines) and cold (Orange lines) accretion modes of AGNs with our model. As a comparison, the red dotted–dashed lines show the wind’s power and momentum flux from Gan et al. (2014).
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Images of proplyds 142–301, 154–240, 155–338, 158–326, 158–327, and 159–359 at five wavelengths. ALMA Band 7 (0.86 mm) images, originally published by Eisner et al. (2018), are shown in the left column. Our ALMA Band 3 (3.1 mm) images CLEANed with a robust parameter of 0.5 and 2.0 are shown in the second and third columns, respectively. The fourth, fifth, and sixth columns show VLA images at K Band (1.3 cm), X Band (3.6 cm), and C Band (6 cm) from Sheehan et al. (2016). The size of each image is noted in the lower right, and the beam size is indicated by the white ellipse in the lower left. For scale, the beam size of the ALMA 3.1 mm (r = 0.5) image is 23 × 29 au. The color represents the surface brightness in units of millijansky/beam. The ALMA Band 7 images detect thermal dust emission from the disk, whereas the VLA images detect free–free emission from the proplyd ionization fronts. The Band 3 images reveal emission from both the dust and free–free components.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Surface brightness cuts across the Band 3 (r = 0.5) images of the proplyds. Each cut is the mean value of a 9 pixel (0.″072) wide strip centered on the disk. Blue lines are head-to-tail cuts with the origin at the disk and positive values toward the head. Red lines are horizontal cuts when the proplyd is rotated with the head facing up. The vertical dotted magenta line shows the location of the outer edge of the ionization front (r IF). The black line in the upper left indicates the minor axis of the beam (0.″057).
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: HST/Advanced Camera for Surveys F435W image of the ONC center by Robberto et al. (2013) overlaid with the field of view of the ALMA Band 3 mosaic and the locations of the 12 proplyds presented in this paper (red circles). The bright Trapezium stars are visible in the center of the image. North is up, and East is left.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Same as Figure 2 but for proplyds 159–350, 170–249, 170–337, 173–236, and 177–341W. Note that the K Band (1.3 cm) image of 159–350 detects the disk component in addition to the ionization front.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Size of the proplyd disks measured from ALMA Band 3 and Band 7 images. The sizes agree for most sources although three are slightly smaller at Band 3. Proplyd 182–413 was not covered by the Band 7 observations and thus is excluded from this plot.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Same as Figures 2 and 3 but for proplyds 180–331 and 182–413. Proplyd 182–413 resides outside the bounds of the ALMA Band 7 mosaic.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: ALMA Band 3 image of the proplyd 180–331 showing the wind arc, which was also seen in HST images of this source. This is the only proplyd in our sample with a wind arc detected. The color scale is truncated, saturating the disk and proplyd head.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Size of the proplyd disks vs. their projected separation from θ 1 Ori C.
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: Top row: HXR lightcurves from RHESSI in discrete energy bands. The A0 and A1 flags (horizontal magenta lines) denote the RHESSI attenuator states. The A0 state corresponds to both thick and thin aluminum attenuators out of the detector field of view, and the A1 state corresponds to “thin in” and “thick out.” The N flag (horizontal cyan line) denotes RHESSI night, when the spacecraft field of view is occulted by Earth. The SAA flag (horizontal orange line) denotes instrument switch-off due to the crossing of the South Atlantic Anomaly. Also shown are the SXR lightcurves from GOES/XRS in the 1–8 Å wavelength range (black solid). Bottom row: Observed Lyα (red) and He II (blue) irradiance from GOES/EUVS-E and SDO/EVE, respectively. The vertical dashed line in each panel represents the peak of the 25–50 keV band for each flare.
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: Temporal evolution of the nonthermal parameters for each flare as derived from RHESSI HXR spectroscopy. First row: Electron rate (A). Second row: Spectral index (δ). Third row: Low-energy cutoff (E  c ). Fourth row: Nonthermal electron power (P nth). Fifth row: Reduced χ 2 value for the combined fit model at each interval. The vertical dashed gray line indicates the peak time of the RHESSI 25–50 keV energy band.
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: Normalized irradiance profiles for each of the three flares. Red and blue curves correspond to Lyα and He II data, respectively. Solid lines correspond to observational data from GOES/EUVS-E and SDO/EVE while dashed lines correspond to the predicted irradiance profiles from FISM2. Overplotted are vertical lines corresponding to the peaks of the 25–50 keV emission from RHESSI (dashed black) and the 1–8 Å emission from GOES/XRS (dotted black).
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: Images taken from SDO/AIA for each flare listed in Table 1 in the 94 Å (top row) and 304 Å (bottom row) filters approximately centered around the Lyα peaks. Each column represents a single flare and the timestamp of each image is shown in the title above each frame. Cyan boxes in each image indicate the flaring region.
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: RHESSI spectra from the HXR peak of each flare with individual fit components overlaid. Each plot shows the model fits to the count data at the peak of the impulsive phase, taken from detector 6. The normalized residuals are shown in the lower panels. The dotted lines indicate the energy range over which the fits were performed.
Paper: Observational Analysis of Lyα Emission in Equivalent-magnitude Solar Flares
Authors: Harry J. Greatorex, Ryan O. Milligan, Phillip C. Chamberlin
Figure caption: Nonthermal and radiated power as a function of time for each flare in the sample. The dotted lines indicate the impulsive phase integration limits. The shaded region represents P nth ± σ, where σ is taken as the standard deviation of P nth over the full set of RHESSI detectors used.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of the downstream to upstream PUI temperature and pressure ratios obtained from the hybrid simulations in the parameter space of M A, θ Bn, and ξ. Panel (a): dependence of ﹩{T}_{\mathrm{iso},\mathrm{PUI}}^{{\rm{d}}}/{T}_{\mathrm{PUI}}^{{\rm{u}}}﹩ on M A and θ Bn for ξ = 0.2, 0.3, and 0.4 is shown with symbols, while the best fits obtained with polynomial functions for each ξ are shown with color-coded surfaces. Panel (b): one-dimensional dependencies of the temperature ratios on M A for chosen ξ and θ Bn; the black lines show the best-fit analytic functions. Panel (c): the same as in panel (b), but for the pressure ratios.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of ﹩{T}_{\mathrm{iso},\mathrm{PUI}}^{{\rm{d}}}/{T}_{\mathrm{PUI}}^{{\rm{u}}}﹩ obtained from the hybrid simulations in the parameter space of M A, θ Bn, and β. The top panels show 2D distributions for three different shock angles. The black dots in the figure represent the values of M A and β in our global model. One-dimensional extractions of the dependency of ﹩{T}_{\mathrm{iso},\mathrm{PUI}}^{{\rm{d}}}/{T}_{\mathrm{PUI}}^{{\rm{u}}}﹩ on the Mach number and plasma beta are shown in panels (d) and (e). Panel (f) shows the distributions of ﹩{T}_{\mathrm{iso},\mathrm{PUI}}^{{\rm{d}}}/{T}_{\mathrm{PUI}}^{{\rm{u}}}﹩ in the extended range of parameters M A ∈ [1, 1500] and β ∈ [1, 1 × 105].
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: (Left) Correct fit of synthetic mixed-mode frequencies to the peak-bagged modes of KIC 4912198, a red giant viewed pole-on. (Right) Solution with a comparable BayesOpt loss that incorrectly assigns the peak-bagged modes to the m = +1 component. This inaccurate assignment is reflected in the fractional contribution of each rotational component to the BayesOpt loss listed below each panel.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: (Left) Correct fit of synthetic mixed-mode frequencies to the peak-bagged modes of KIC 8429977, a red giant viewed edge-on. (Right) Solution with a comparable BayesOpt loss that incorrectly assigns the peak-bagged modes to the m = −1, 0 components. Similar to Figure 19 this inaccurate assignment is reflected in the fractional contribution of each rotational component to the BayesOpt loss listed below each panel.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Similar to Figure 21(a), but for the final results we report in our work. Here the incorrect fits have been rectified, leaving behind the correct fits that occupy a specific regime within this parameters space. The incorrect fits from Figures 19 and 20 are included. To confirm the validity of our analysis, we color coded points in the plots according to the number of rotationally split components (left) and stellar inclination angle as reported by Gehan et al. (2018).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Relative contributions of different rotational components to the BayesOpt loss. The sample in this plot has not been vetted, meaning that they are obtained directly from an automated run of BayesOpt over the sample in this work using the triplet rotational splitting assumption. The labels are provided by manual inspection of the fits. The incorrect fits from Figures 19 and 20 are included.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Stellar mass and bulk metallicity [M/H] for the 684 targets in our sample with chemical abundances from APOGEE DR17. Also shown is the Spearman coefficient (R) between the two parameters, with 1 indicating a perfect monotone correlation and 0 indicating the absence of any correlation.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Stretched period echelle diagrams for the seven metal-poor Kepler low-luminosity red giants.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: The distributions of the following quantities are shown in projection on the TS surface: (a) upstream shock angle (θ Bn); (b) compression ratio; (c) PUI-to-proton density ratio; (d) downstream PUI-to-proton temperature ratio; (e) downstream PUI-to-proton pressure ratio; and (f) ratio of our PUI temperature to the one obtained with the model of Shrestha et al. (2020). The distributions are presented in the Solar Ecliptic J2000 coordinates centered along the x-axis. The positions of V1 and V2 at the moment of their crossing of the TS, the NH current position, and the projection of the B ∞–V ∞ plane onto the TS surface (solid black line) are also shown. It should also be noted that each panel utilizes distinct ranges for the colorbar.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of the rate of change due to charge exchange for the proton density (S  n ), plasma pressure (S  p ), and plasma temperature (S  T ) along the x-axis from 70 to 140 au in Model 1 (red dots) and Model 2 (blue plus symbols). From the top to the bottom, these quantities are shown for the plasma, PUIs, and thermal protons.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of the density, pressure, and temperature of neutral H atoms in Model 1 (red lines) and Model 2 (blue lines) along the x-axis from 10 to 400 au. The top, middle, and bottom panels refer to H(1), H(2), and H(3). The TS and HP are shown by the dashed and solid gray vertical lines for Models 1 and 2, respectively.