adsabs/AstroCLIMB huggingface dataset:
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Same as the Figure 6, but for the end views.
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Panel (a) illustrates the number density distributions at 15:32 UT and 15:34 UT along the white dashed line in Figure 10(a), respectively. Panel (b) illustrates the time–distance diagram of two wavelike structures along the red solid line in Figure 10(a).
Paper: Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model
Authors: J. H. Guo, Y. W. Ni, Z. Zhong, Y. Guo, C. Xia, H. T. Li, S. Poedts, B. Schmieder, P. F. Chen
Figure caption: Panels (a) and (d), respectively, show the side views of the synthesized white-light images at 15:30 UT and 15:36 UT. Panels (b) and (e), respectively, show the side views of the synthesized EUV 193 Å running-difference images at 15:30 UT and 15:36 UT. The pink arrows in panels (d) and (e) indicate the CME leading front and “EIT wave,” respectively. Panels (c) and (f) show the STEREO/COR1 images with the superposition of EUVI 195 Å running-difference images at 15:46 and 15:51 UT, respectively. The blue (red) dashed lines outline the CME leading front (forward shock wave), and the solid lines outline the two components of the EUV waves.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The same as Figure 13 except for the initial inclination of the test particles chosen randomly between 0° ≤ I ≤ 30°.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The same as Figure 14 except for the range in the semimajor axis of 40 au ≤ a ≤ 49 au.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The same as Figure 14 except for the range in the semimajor axis of 60 au ≤ a ≤ 80 au.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The same as Figure 14 except for the range in the semimajor axis of 50 au ≤ a ≤ 60 au.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: Dynamical maps of the trans-Neptunian region between 34 au ≤ a ≤ 40 au and 0 ≤ e ≤ 0.6. The inclinations and the longitudes of ascending node are kept fixed at I = 0° and Ω = 0°. The arguments of perihelion ω and the mean anomalies M are chosen randomly. Blue hexagons: initial (a, e) values of TNOs in long-term resonances; pink diamonds: initial (a, e) values of TNOs in short-term resonances; black (/white—in the subsequent figures) stars: initial (a, e) values of nonresonant TNOs. Solid lines: (a,e) values resulting in Neptune- or Uranus-crossing orbits. Dashed lines: distances of three Hill radii from the two giant planets. Vertical lines on the top of the panels: MMRs hosting more than 10 TNOs. Left panel: map of Δe. Right panel: map of Δa.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2014 QH563 engaged in a 13:9 inclination-type MMR with Neptune. The structure of the figure is the same as of Figure 7, but showing this time the FAIR panel and the time evolution of the critical argument corresponding to an inclination-type MMR.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 1999 RH215 engaged in a 7:4 MMR with Neptune. The structure of the figure is the same as of Figure 4. Note the episodical libration of the critical arguments ﹩{{\rm{\Theta }}}_{1}^{(I)}﹩ and ﹩{{\rm{\Theta }}}_{1}^{(e)}﹩.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2013 TK227, a temporary Trojan of Neptune. The structure of the figure is the same as of Figure 7.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2007 TC434 engaged in a 9:1 MMR with Neptune. The structure of the shown panels is the same as in Figure 4; however, in this case, only ﹩{{\rm{\Theta }}}_{1}^{(e)}﹩ librates, therefore, neither the panel to identify the inclination-type MMR nor the time evolution of ﹩{{\rm{\Theta }}}_{1}^{(I)}﹩ are displayed. This object is involved only in an eccentricity-type MMR.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2004 KV18, identified previously as a temporary Trojan of Neptune. Our long-term numerical integration shows that this object is captured temporarily in a 13:3 eccentricity-type MMR spending there about 4 × 107 yr. The structure of the figure is the same as of Figure 7.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2015VK167 engaged in a 5:3 MMR with Neptune. The structure of the figure is the same as of Figure 4. In this case, ﹩{{\rm{\Theta }}}_{1}^{(I)}﹩ librates only temporarily, while ﹩{{\rm{\Theta }}}_{1}^{(e)}﹩ librates during the whole numerical integration.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The number distributions of the 4121 TNO of our sample, with respect to the eccentricities and inclinations.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the asteroid 2014 RL86 engaged in a 25:3 eccentricity-type MMR with Neptune. The structure of the figure is the same as of Figure 7.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: The dynamics of the dwarf planet Pluto engaged in a 3:2 MMR with Neptune. The first two panels in the uppermost row show the ﹩\lambda -{\lambda }^{{\prime} }﹩ vs. M and ﹩\lambda -{\lambda }^{{\prime} }﹩ vs. M + ω planes used to determine the type, order, and degree of the resonance by applying the FAIR method. The third panel reveals the region covered by Pluto in the (a, e) plane during the whole length of the numerical integration. The lower panels display, respectively, the time evolution of the orbital elements a, e, and I, and that of the critical arguments of the inclination- and eccentricity-type MMRs ﹩{{\rm{\Theta }}}_{1}^{(I)}﹩ and ﹩{{\rm{\Theta }}}_{1}^{(e)}﹩.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: Distribution of TNOs in the (a, e) plane. The gray dots denote nonresonant TNOs and the colored ones stand for eccentricity-type resonant TNOs: the blue dots indicate TNOs that are engaged in the given MMR throughout the whole 108 yr long time span of the numerical integration, and pink dots mark TNOs that are captured temporarily in the given MMR. The vertical green lines highlight the locations of MMRs with more than 10 members.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: Distribution of TNOs in the (a, I) plane. The gray dots denote nonresonant TNOs and the colored ones stand for inclination-type resonant TNOs: the red dots indicate TNOs that are engaged in the given MMR throughout the whole 108 yr long time span of the numerical integration, and the cyan dots mark TNOs that are captured temporarily in the given MMR. The vertical green lines highlight the locations of MMRs with more than 10 members.
Paper: A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune
Authors: E. Forgács-Dajka, E. Kővári, T. Kovács, Cs. Kiss, Zs. Sándor
Figure caption: Distribution of TNOs in the (e, I) plane. Left panel: TNOs involved in eccentricity-type MMRs—the color coding is the same as in Figure 1. Right panel: TNOs involved in inclination-type MMRs—the color coding is the same as in Figure 2.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: CCFs (after inversion and normalization) of a binary star with different T eff, calculated using various templates. The top, middle, and bottom panels display the CCFs of the binary star with T eff values of approximately 2500 K, 5500 K, and 8000 K, respectively. The red, blue, and green dashed lines represent the CCFs calculated using templates with T eff values of 2500 K, 5000 K, and 8000 K, respectively. The black solid line corresponds to the CCF calculated from the template used in this study, i.e., the solar spectrum.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: Examples of misclassified CCFs. Left: CCFs of misclassified single stars. Right: CCFs of misclassified SB2s. The top panel on the right shows a CCF with a secondary peak too small to be ignored by the model, while the bottom panel shows a CCF with primary and secondary star RVs that are too close to be distinguished by the model. The red dashed line represents the RV component of the CCF.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: The results of the CCFs calculated from the synthetic spectra in Figure 2. The red points are the peaks of the CCF, representing the RV of the spectra.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: Examples of synthetic spectra. The top and middle panels are synthetic single-star spectra; the bottom panel is the normalized double-star spectrum after summing two single-star spectra.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: Confusion matrix of the model on the testing set.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: The results of the inversion and normalization of the CCFs from Figure 3.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: Synthesis process of single- and binary star spectra.
Paper: Searching for Double-line Spectroscopic Binaries in the LAMOST Medium-resolution Spectroscopic Survey with Deep Learning
Authors: Zepeng Zheng, Zhong Cao, Hui Deng, Ying Mei, Lei Tan, Feng Wang
Figure caption: The results of the original CCFs (dashed lines) and the CCFs after five Softmax calculations (solid lines).
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Example of the extended (∼200 ″) PN JnEr 1 observed by GALEX (left; Bianchi & Thilker 2018) in FUV (blue) and NUV (yellow), and by PS1 (right) in g (blue), r (green), and y (red). North is up and east is to the left. In the GALEX imaging, the CSPN appears very bright and resolved, but the “best” measurement includes nebular emission: according to the pipeline, the best magnitude is obtained from a Kron elliptical aperture with a Kron radius of 5.″25 and semimajor and semiminor axis of 11.″63 and 9.″62, respectively. In PS1, it was measured as a pointlike source (with PS1_psfMag_r − PS1_kronMag_r < 0.04 according to the Chambers et al. 2016 definition of pointlike sources). Radial profiles for the two GALEX bands (bottom) are also shown. Aperture measurements are included in the catalog and should be used for the central star.
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Optical (top panels) and UV (bottom panels) spectra of PN NGC 1501 (left) and NGC 3587 (right). The SDSS and PS1 (top) and GALEX (bottom) transmission curves are overlaid.
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Examples of extended PNs. GALEX NUV images of G 231.8+04.1 (top left panel) and G 164.8+31.1 (bottom left panel). The right-hand panels show the profile of the NUV flux and its error (blue stepped solid and dashed lines, respectively), the sigma-clipped NUV surface flux (red dotted line), the background estimation (red solid line), and the calculated NUV radius of each PN (vertical blue line; vertical purple line for FUV radius). The images have different sizes to optimally display the PNs; the extent is labeled in the figure.
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Top panel: curve of growth of GALEX NUV_MAG_APER_4 (6″) compared with the magnitudes measured in larger GALEX apertures (NUV_MAG_APER_5, NUV_MAG_APER_6, and NUV_MAG_APER_7; 9″, 12.″8, and 17.″3). Aperture correction from Morrissey et al. (2007) has been applied. Bottom panel: difference between the GALEX 6″ and 9″ radius aperture magnitudes. A difference larger than 0.036 (red solid line) indicates that the object is extended. For values below 0.036, we consider the object to be pointlike (see the text).
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Comparison of PN sizes estimated in optical images, as extracted from PNcat, and those calculated with the GALEX NUV radial profile analysis (top panel; the solid line is a 1:1 relation for comparison). The bottom panel shows the difference between the NUV radius and MajDiam/2 from PNcat. The inset figures enhance a reduced range of data.
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Distributions of GALEX FUVavg and NUVavg magnitudes (top) and FUV−NUV (bottom) in GUVPNcat. The vertical lines mark the saturation limit of each band in the upper panel.
Paper: The GRETOBAPE Gas-phase Reaction Network: The Importance of Being Exothermic
Authors: Lorenzo Tinacci, Simón Ferrada-Chamorro, Cecilia Ceccarelli, Stefano Pantaleone, Daniela Ascenzi, Andrea Maranzana, Nadia Balucani, Piero Ugliengo
Figure caption: Comparison of the network postcleaning (GRETOBAPE) over precleaning predicted abundance ratios (left panels) and postcleaning abundance (right panels) as a function of time for the cold molecular cloud model (Section 4.1.1). The three rows show three groups of species where the abundance ratios during the evolution are ≥103 or ≤10−3 (top panels), 10–103 or 0.1–10−3 (middle panels), and 3–10 or 0.1–0.3 (bottom panels). Only species with abundances larger than 10−13 at steady state are considered.
Paper: The GRETOBAPE Gas-phase Reaction Network: The Importance of Being Exothermic
Authors: Lorenzo Tinacci, Simón Ferrada-Chamorro, Cecilia Ceccarelli, Stefano Pantaleone, Daniela Ascenzi, Andrea Maranzana, Nadia Balucani, Piero Ugliengo
Figure caption: Original Si-bearing reaction network, visualized as a directed colored graph. The reactions are represented as solid lines and the species as nodes (differently from the representation described in Section 2.2, where reactions and species are both represented by nodes). The lines are colored based on the log 10 of the reaction rate constants calculated at 90 K and multiplied by the reactant densities at 5 × 103 yr in the “warm molecular outflow shock” model described in Section 4.1.2, using the original (precleaning) network. All rates larger than 10−10 are red, and those less than 10−25 are violet. The nodes are colored based on the graph distance of that species from Si+ (highlighted in black). The species removed from the original network are marked by red crosses, while those detected in the ISM are marked by blue squares. Please note that the digital format of the figure is vectorial and can be zoomed in to better look at the details.
Paper: The GRETOBAPE Gas-phase Reaction Network: The Importance of Being Exothermic
Authors: Lorenzo Tinacci, Simón Ferrada-Chamorro, Cecilia Ceccarelli, Stefano Pantaleone, Daniela Ascenzi, Andrea Maranzana, Nadia Balucani, Piero Ugliengo
Figure caption: Same as Figure 3, but showing only the reactions removed from the cleaning process.
Paper: The GRETOBAPE Gas-phase Reaction Network: The Importance of Being Exothermic
Authors: Lorenzo Tinacci, Simón Ferrada-Chamorro, Cecilia Ceccarelli, Stefano Pantaleone, Daniela Ascenzi, Andrea Maranzana, Nadia Balucani, Piero Ugliengo
Figure caption: Three different ways to visualize and work with a reaction network: reaction list (left panel); colored directed graph (or colored di-graph), where circles correspond to chemical species, while squares indicate rate constants (middle panel); and nonsymmetric adjacency (or connectivity) matrix representation of the colored di-graph (right panel).
Paper: The GRETOBAPE Gas-phase Reaction Network: The Importance of Being Exothermic
Authors: Lorenzo Tinacci, Simón Ferrada-Chamorro, Cecilia Ceccarelli, Stefano Pantaleone, Daniela Ascenzi, Andrea Maranzana, Nadia Balucani, Piero Ugliengo
Figure caption: Histogram of the enthalpy ΔH(0) (red) of the endothermic reactions removed from the original network after the cleaning process. The inset (blue) shows the zoom-in of the 10–400 kJ mol−1 interval. The bin width is computed following the Freedman–Diaconis estimator (Freedman & Diaconis 1981).
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Condensation curves for detected gaseous organic species in Titan’s atmosphere. The black line in each panel represents Titan’s mean temperature profile, and the shaded gray area represents the range of retrieved temperature profiles using Cassini/CIRS data throughout the Cassini mission (Teanby et al. 2019). Note that the altitude axis on the right represents the altitude for the mean P–T profile. The solid condensation curves are plotted with the average mixing ratio, and the shaded regions are plotted using the observed upper and lower bond mixing ratios listed in Table 1. Solid condensation curves represent s-g transitions and dashed lines represent l-g transitions. Left: condensation curves for CH4, C2H6, C2H4, C2H2, C4H2, and C6H6. Center: condensation curves for C3H6, C3H8, C3H4-a (allene), C3H4-p (propyne), HCN, and HC3N. Right: condensation curves for CO2, CH3CN, C2H5CN, C2H3CN, C2N2, and C4N2.
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Comparison of the selected s-g SVP functions in Table 3 to the other evaluated s-g SVP functions in Table A1, for the first half of the species in Table 1. The solid lines represent the applicable temperature range (or the temperatures without brackets in Tables 3 and A1). The different SVP functions agree relatively well for the applicable temperature range. The dotted lines represent the extrapolated temperature range for each SVP function (or the temperatures without brackets in Tables 3 and A1). The different SVP functions start to deviate from each other for the extrapolated temperature range. Note that for benzene, we plot the unadjusted low-temperature s-g SVP expressions in Dubois et al. (2021); the adjusted s-g SVP expressions of Dubois et al. (2021) in Hudson et al. (2022) are similar to the independently measured SVP expressions in Hudson et al. (2022).
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Photochemistry in Titan’s upper atmosphere leads to the creation of numerous organic molecules, from simple organics in the gas phase to complex refractory organic solids that form Titan’s thick haze layers. The simple organics could undergo phase changes that, along with the complex organics, participate in various atmospheric and surface processes on Titan.
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Comparison of the selected s-g SVP functions in Table 3 to the other evaluated s-g SVP functions in Table A1, for the second half of the species in Table 1. The notations are the same as in Figure 3. The different SVP functions agree relatively well for the applicable temperature range, except for C4N2, which has one outlier s-g SVP. Similar to Figure 3, the different SVP functions start to deviate from each other for the extrapolated temperature range.
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Comparison of the selected l-g SVP functions in Table 3 to the other evaluated l-g SVP functions in Table A1, for the second half of the species in Table 1. The notations are the same as in Figure 3. The different SVP functions agree relatively well for the applicable temperature range, except HC3N, which has one outlier l-g SVP. Similar to Figure 3, the different SVP functions start to deviate from each other for the extrapolated temperature range.