adsabs/AstroCLIMB huggingface dataset:
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of 100 km rocky planetesimals breaking up by the ram pressure before their fragments collide with Jupiter’s core. From top to bottom, the panels correspond to 1/10, 1/3, and 1 full mass of Saturn. As shown here, breakup occurs deep in the envelope.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the final orbital eccentricities of 100 km rocky planetesimals in terms of their initial semimajor axes. The top-left panel shows the results for the system without Saturn. The top-right panel corresponds to 1/10 of Saturn’s mass. The bottom-left panel is for the system with 1/3 of the mass of Saturn, and the bottom-right panel shows the results for the system with 1 full Saturn mass.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of 100 km rocky planetesimals penetrating the envelope and striking the surface of Jupiter’s core at early times. From top to bottom, the panels correspond to 1/10, 1/3, and 1 full mass of Saturn.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the vaporization (top) and breakup (bottom) of 10 km mix-composition planetesimals for 1/10 of a Saturn mass. As shown here, vaporization is rare and ram pressure breakup is the dominant process.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: The tuning fork graphs of the accretion times of 100 km rocky planetesimals. The top-right panel corresponds to 1/10 of Saturn’s mass. The bottom-left panel is for the system with 1/3 of the mass of Saturn, and the bottom-right panel shows the results for the system with 1 full Saturn mass.
Paper: Detailed Calculations of the Efficiency of Planetesimal Accretion in the Core-accretion Model. II. The Effect of Saturn
Authors: Nader Haghighipour, Morris Podolak, Esther Podolak
Figure caption: Graphs of the breakup of 1 km pure-ice planetesimals due to ram pressure for different values of Saturn’s mass. From top to bottom, panels corresponds to 1/10, 1/3, and 1 full Saturn mass. As shown here, breakup happens at high altitudes in the envelope.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Left: Exposure-corrected 0.7–2 keV Chandra image of 3CR 196.1 with Hα + [N II]λ6584 (blue) and 8.4 GHz VLA (cyan) contours. The position of the centroid of the optical host, which corresponds to the radio core position is shown as a black cross. The Chandra image has a pixel scale of 0.″492 (corresponding to ∼1.6 kpc) and was smoothed with a 1.″5 radius Gaussian kernel. X-ray contours are drawn at 0.25  · 10−15 erg cm−2s−1. Hα + [N II]λ6584 contours were drawn at 5, 10, 20, 50, and 100 times the rms. 8.4 GHz VLA contours were drawn at 5, 20, and 50 times the rms level of the background. Hα and the [N II]λ6584 emission present an offset with respect to the borders of the X-ray cavity. The northeastern radio lobe is co-spatial with the X-ray emission peak, while the southwestern lobe is co-spatial with the X-ray cavity. Right: Redward [N II]λ6584 emission with the same exposure-corrected 0.7–2 keV Chandra contours (red) and Hα + [N II]λ6584 contours (blue) overlaid as in the left panel. The (a) and (b) regions marked in the figure show the extraction areas of the spectra in Figure 2.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Spectra extracted from regions a and b (top and bottom panels in Figure 1, right panel, respectively). The top spectrum could be fitted using a single Gaussian component for each line, while the bottom one shows an extra redward component in all lines except for the Hβ and [O III]λ λ4960, 5008 lines. Black markers point to the rest-frame position of each line while red markers are located at 21 Å from the rest frame (∼1000 km s−1). The uncertainties in the spectra are shown in gray.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: Comparison of the ACF(Δf) functions derived from our observations (green dots) with the best-fit theoretical predictions for the extended-medium model with power-law spectral index α as a fitting parameter (solid blue lines) and for the thin-screen model (dashed red lines) with the same spectral index for comparison. For better comparison all functions were normalized by their HWHM frequency lags, Δf 1/2. Only the inner part of the ACFs down to 45% or up to Δf/Δf 1/2 ∼ 1.2 for which a good fit could be obtained for all pulsars was used for the fit. The parameter, α, which is essentially the same for our ACFs for both models for the fitting range is given for each pulsar. For some pulsars the width of the scintles in terms of Δf 1/2 relative to the receiver bandwidth of 16 MHz was relatively large so that only a shortened version of the functions was plotted.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: The four ACF(y) functions listed in Table 4 and plotted as a function of frequency lag Δf. The functions are normalized in amplitude and with respect to their HWHM, Δf 1/2, for easy comparison. All functions are two-sided; only one side is plotted. In addition, observed ACFs are plotted for four pulsars to display the range of ACF variations for comparison.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: The ACF(Δf) function (thick green line) for PSR B0823+26 compared with the extended-medium (solid blue curve) and thin-screen model (dashed red curve) but for frequency lags up to about 6 × Δf/Δf 1/2. The extended-medium model is drawn as in Figure 5 with α em = 3.56. The thin-screen model is plotted for α ts = 3.49 as a test, in an attempt to match the tail of the ACF without excessively changing the best-fit value of α = 3.56.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: Comparison of the ACF(Δf) functions derived from the observations (blue dots) with the theoretical predictions for the extended-medium scattering theories with power-law spectral index, α, as a fitting parameter. The solid line shows the best-fitting model for the inner part of the ACF(Δf) down to 45% consistently for all pulsars. The surrounding dotted lines indicate Δα = ±0.05 deviations from the best-fit value for illustration purposes. For better comparison all functions were normalized by their HWHM frequency lags, Δf 1/2.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: The magnitude of the Fourier transform of the observed ACFs, ∣ ﹩{ \mathcal F }{ \mathcal T }(\mathrm{ACF})﹩∣ (green dots), fit by the theoretical predictions for the extended-medium scattering theory with rounded power-law spectral index α (solid blue lines) and for the thin-screen model (dashed red lines) with the same value for α. Scattered points in the tail of some functions are due to noise. Delay is given as Δτ with Δτ 1/2 as the HWHM listed in Table 2.
Paper: Electron Density Variations in the Interstellar Medium and the Average Frequency Profile of a Scintle from Pulsar Scintillation Spectra
Authors: N. Bartel, M. S. Burgin, E. N. Fadeev, M. V. Popov, N. Ronaghikhameneh, T. V. Smirnova, V. A. Soglasnov
Figure caption: The four functions, y, in Table 4 plotted as a function of frequency, f. Three functions are normalized in amplitude and width to facilitate comparison. The fourth function, K, is plotted with the respective normalization parameter corresponding to the function, E. It goes to infinity at f → 0. As in Figure 7, all functions are two-sided; only one side is plotted.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Same as Figure 4, but with LSNe labeled based on their distinct groups. We see that LSNe do not perfectly separate into distinct classes, even after subdividing them. But some trends so start to appear: Slow SLSN-like LSNe mostly reside in the SLSNe-dominated parameter space; Fast Ic-like LSNe mostly overlap with the existing SNe Ic population; Fast SLSN-like and Slow Ic-like LSNe lie outside the typical parameter space occupied by SLSNe or SNe Ic.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves and spectra of the Fast Ic-like LSNe group. Only r-band light curves and their respective MOSFiT models are shown. Spectra are arbitrarily scaled. Individual references are listed in Appendix A.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Peak r-band magnitude as a function of rise time for LSNe, labeled by their distinct groupings. We see that LSNe do appear to separate well in terms of rise time and absolute peak magnitude, forming four distinct quadrants.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves and spectra of the Slow Ic-like LSNe group. Only r-band light curves and their respective MOSFiT models are shown. Spectra are arbitrarily scaled. Individual references are listed in Appendix A.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves and spectra of the Other group. Only r-band light curves and their respective MOSFiT models are shown. Spectra are arbitrarily scaled. Individual references are listed in Appendix A.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Revised sunspot group numbers compiled in this study for 1727–1748. New additions from forgotten records (Section 2), revised data from known records (Section 3), confirmed data from known records (Section 3), unconfirmed data from known records (V+16), Wargentin’s records (A18), Japanese records in 1749 (Hayakawa et al. 2018a = H+18a), and revised data for 1729–1731 (Hayakawa et al. 2018b = H+18b) are shown as blue diamonds, red circles, green squares, black dots, black diamonds, green diamonds, and orange squares, respectively.(The data used to create this figure are available.)
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Estimated annual sunspot group numbers and assumed error margins in 1725–1749, obtained by applying SS16’s brightest star method to the collection revised in this study.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Comparison of different reconstructions of sunspot group number and number of days with records from 1725 to 1750. The red, green, and blue curves show the sunspot group numbers from SS16 and C17, and CL16/20, namely the International Sunspot Number in CL16 divided by 20 as done in Muñoz-Jaramillo & Vaquero (2019). The gray bars show the number of days with records based on V+16 and Wargentin’s data from A18.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Winthrop’s sunspot drawings for 1739 April 20 and 22 in the Julian calendar, or 1739 May 1 and 3 in the Gregorian calendar, derived from MS HUM 9 (BOX 3, f. 1), courtesy of the Harvard University Archives. Winthrop’s records have otherwise been derived from his textual reports.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Examples of Van Coesfelt’s sunspot drawings for 1728 December and 1729 January, derived from Van Coesfelt (1730).
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Examples of Mucio Muzano’s sunspot drawings in Muzano (1754).
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Examples of Dûclos’s sunspot observations in plate of MHSBA (1736) for 1736 March 16 and 19.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Benjamin Martin’s sunspot drawing for 1737 August 25 in the Julian calendar (1737 September 5 in the Gregorian calendar).
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: The integrated intensity of HCO+ (1–0) is shown in color scale (mean rms = 40 mK km s−1). The white contours show the N(H2) distribution at levels [5, 9, 13, 20] × 1021 cm−2, taken from Spezzano et al. (2017). The red star shows the millimeter dust peak position (R. A. (J2000) = 05h04m17.ˢ21, decl. (J2000) = 25d10m42.ˢ8, Ward-Thompson et al. 1999). The crosses represent the positions where the spectra of Figure 2 have been extracted. The IRAM beam size (29”) and scalebar are shown in the bottom left and right corners, respectively.
Paper: Search for Quasiperiodic Oscillations in Precursors of Short and Long Gamma-Ray Bursts
Authors: Shuo Xiao, Wen-Xi Peng, Shuang-Nan Zhang, Shao-Lin Xiong, Xiao-Bo Li, You-Li Tuo, He Gao, Yue Wang, Wang-Chen Xue, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Cheng-Kui Li, Shu-Xu Yi, Xi-Lu Wang, Zhen Zhang, Ce Cai, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, De-Hua Wang, Xi-Hong Luo, Qi-Jun Zhi, Li-Ming Song, Ti-Pei Li
Figure caption: The light curves of precursors in GRB 100223110, GRB 141102536, GRB 160726065, and GRB 180511437. The green lines are the mean functions (i.e., FRED) from the maximum likelihood samples, the orange lines are the predictions based on the maximum likelihood samples, and the light blue vertical lines are the maximum likelihood start or end of the red noise and possible QPO. However, the InBF qpo of them are all less than three, that is, there is not enough significance to confirm the existence of a QPO. The time bin size of light curves is 1 ms.
Paper: Search for Quasiperiodic Oscillations in Precursors of Short and Long Gamma-Ray Bursts
Authors: Shuo Xiao, Wen-Xi Peng, Shuang-Nan Zhang, Shao-Lin Xiong, Xiao-Bo Li, You-Li Tuo, He Gao, Yue Wang, Wang-Chen Xue, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Cheng-Kui Li, Shu-Xu Yi, Xi-Lu Wang, Zhen Zhang, Ce Cai, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, De-Hua Wang, Xi-Hong Luo, Qi-Jun Zhi, Li-Ming Song, Ti-Pei Li
Figure caption: The Li–Ma significance vs. the p value (PDS) of potential QPOs. The Pearson correlation coefficients for them are 0.17 and 0.08 for precursors of SGRBs and LGRBs, respectively. Thus no clues are found for the common presence of QPOs in the precursors.
Paper: Search for Quasiperiodic Oscillations in Precursors of Short and Long Gamma-Ray Bursts
Authors: Shuo Xiao, Wen-Xi Peng, Shuang-Nan Zhang, Shao-Lin Xiong, Xiao-Bo Li, You-Li Tuo, He Gao, Yue Wang, Wang-Chen Xue, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Cheng-Kui Li, Shu-Xu Yi, Xi-Lu Wang, Zhen Zhang, Ce Cai, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, De-Hua Wang, Xi-Hong Luo, Qi-Jun Zhi, Li-Ming Song, Ti-Pei Li
Figure caption: PDS of precursors in SGRBs. The solid orange lines show the best-fitting power-law+constant models, and the black dotted lines represent the 3σ level. The number of frequencies searched is corrected.
Paper: Search for Quasiperiodic Oscillations in Precursors of Short and Long Gamma-Ray Bursts
Authors: Shuo Xiao, Wen-Xi Peng, Shuang-Nan Zhang, Shao-Lin Xiong, Xiao-Bo Li, You-Li Tuo, He Gao, Yue Wang, Wang-Chen Xue, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Cheng-Kui Li, Shu-Xu Yi, Xi-Lu Wang, Zhen Zhang, Ce Cai, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, De-Hua Wang, Xi-Hong Luo, Qi-Jun Zhi, Li-Ming Song, Ti-Pei Li
Figure caption: Distribution of the PDS slope (α) for precursors and main emissions of SGRBs and LGRBs.
Paper: Search for Quasiperiodic Oscillations in Precursors of Short and Long Gamma-Ray Bursts
Authors: Shuo Xiao, Wen-Xi Peng, Shuang-Nan Zhang, Shao-Lin Xiong, Xiao-Bo Li, You-Li Tuo, He Gao, Yue Wang, Wang-Chen Xue, Chao Zheng, Yan-Qiu Zhang, Jia-Cong Liu, Cheng-Kui Li, Shu-Xu Yi, Xi-Lu Wang, Zhen Zhang, Ce Cai, Ai-Jun Dong, Wei Xie, Jian-Chao Feng, Qing-Bo Ma, De-Hua Wang, Xi-Hong Luo, Qi-Jun Zhi, Li-Ming Song, Ti-Pei Li
Figure caption: P-value region vs. the fraction of times that the p value falls within ≤p value for PDS method. The black dotted line represents the perfect one-to-one relation.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Phase curves calculated using the broadband thermal emission from a radiating level at p rad = 750 hPa, for each GCM simulation. The primary and secondary eclipses would be at phases 0° and 180°. The solid black curve shows emission calculated using the full temperature field, and the dashed gray curve shows emission using the linear approximation given by Equation (24). The dashed red and blue curves show the contributions to the linear approximation from the rotational and divergent temperature fields, respectively.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Temperature anomaly T − T 0 at p = 750 hPa for each GCM simulation. For each simulation, full fields are shown in the top row. The next three rows show the zonal-mean rotational circulation, eddy-rotational circulation, and divergent circulation. For reference, T 0∣ p=750 hPa = 279.6, 281.2, 282.1, and 284.7 K, for the P = 4, 8, 16, and ∞  day simulations, respectively.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Temperature anomaly T − T 0(p) (contours) in the longitude–pressure plane, averaged meridionally from pole to pole (±90° latitude), shown for each GCM simulation. The top row shows the full circulation. Contributions to the full circulation from the eddy-rotational and divergent components are shown in the next two rows.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Free surface displacement (height; color contours) and horizontal velocity (quivers) obtained in a linear shallow water simulation without drag (P = 8 days, Earth’s radius). The height and velocity fields are decomposed into eddy-rotational (center panel) and divergent (right panel) components. The zonal-mean rotational component is small and so is not shown.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Phase curve calculated using broadband thermal emission from a radiating level at p = 200 hPa for the P = 4 day simulation. See the caption of Figure 5 for the meaning of each curve.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Subdivision of divergent geopotential height into contributions from different terms in the divergence equation (Equation (18) in the main text). The top row shows the total divergent height field for each simulation, and subsequent rows show contributions to the divergent height from different terms (labeled to the left of each row). Contributions from terms in the full divergence equation that are due to solely rotational circulation are not shown, as they do not contribute to the divergent geopotential by definition.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Subdivision of divergent geopotential height in the P = 4 day simulation into contributions from the linear u d β term (top panel) and nonlinear rotational-divergent terms (bottom panel).
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Structure of the potential function γ that appears in the momentum equations for the rotational and divergent circulations, obtained from the linear shallow water simulation.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Subdivision of rotational geopotential height in the P = 16 day simulation into contributions from linear (top panel) and nonlinear (bottom panel) terms.