adsabs/AstroCLIMB huggingface dataset:
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Detailed industrial scheme of the cold head designed for the EXCITING project, provided by Cryoscan©. This design is proprietary of Cryoscan©.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: LILBID spectra of (a) acetone, (b) acetone-D6, and (c) propanal. Acetone-D6 is measured to demonstrate that LILBID produces a protonated molecular peak of the analyte compound. It is not possible to differentiate this peak in other compounds in this work due to the interference of water cluster features at the same mass.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: LILBID spectra of (a) 2-hexanone and (b) hexanal.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: LILBID spectra of (a) 2-butanone and (b) butanal.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Normalized relative intensity LILBID mirror plot for 2-butanone (black) and butanal (red).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Normalized relative intensity LILBID mirror plot for acetone (black) and propanal (red).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Peak ratio of relative intensities of 44, 45, and 43 u, such as 44 + 45/43, corresponding to LILBID-produced fragment cations for ketones and aldehydes with carbon numbers of three, four, and six. The x-axis represents the number of carbon atoms, where C3, C4, and C6 stand for carbon three, four, and six compounds, respectively. The y-axis represents the peak ratio.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Percentages of cumulative relative intensities (ion yields) of all mass lines corresponding to LILBID- and EI-produced fragment cations within mass ranges (a) 26–33 and (b) 41–45 u for ketones and aldehydes with carbon numbers of three, four, and six. The x-axis represents the number of carbon atoms, where C3, C4, and C6 stand for carbon three, four, and six compounds, respectively. The y-axis represents the accumulative relative intensities.
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Normalized relative intensity LILBID mirror plot for 2-hexanone (black) and hexanal (red).
Paper: Complementary Mass Spectral Analysis of Isomeric O-bearing Organic Compounds and Fragmentation Differences through Analog Techniques for Spaceborne Mass Spectrometers
Authors: Nozair Khawaja, Jon Hillier, Fabian Klenner, Lenz Nölle, Zenghui Zou, Maryse Napoleoni, Rene Reviol, Frank Postberg
Figure caption: Composition and formation pathways of molecular and fragment cations of (a) 2-hexanone and (b) hexanal- carbonyl compounds with six carbon atoms as produced by EI and LILBID.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Normalized radiant distributions of meteoroid fluxes in Mars’ orbit predicted by the DMZC for the OCCs and three orbital positions: aphelion (L s = 71°, (a)), perihelion (L s = 251°, (b)), and first crossing of the ecliptic plane (L s = 325°, (c)). The abscissa axis represents the ecliptic longitude, λ, corrected by the subsolar terminator (a = λ − λ 0 = 0° at 12 hr), and the ordinate axis b is the latitude measured from the orbital plane of Mars.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Average velocity distributions (in kilometers per second) of meteoroids in Mars’ orbit predicted by the DMZC from the OCCs and two particle diameters: D = 50 μm (a) and D = 1200 μm (b). The abscissa axis represents the ecliptic longitude, λ, corrected by the subsolar terminator (a = λ − λ 0 = 0° at 12 hr), and the ordinate axis b is the latitude measured from the orbital plane of Mars. The average velocity distribution for a given particle size does not change significantly with the orbital position and, therefore, these panels only show the corresponding results at perihelion (L s = 251°).
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the average diameter distribution (in microns) of meteoroids into the Martian atmosphere determined by the MIF model for the OCCs and three orbital positions: aphelion (L s = 71°, (a)), perihelion (L s = 251°, (b)), and first crossing of the ecliptic plane (L s = 325°, (c)). These distributions are represented as a function of the Local True Solar Time and the latitude at Mars. Note that the maximum diurnal size for the OCCs appears at L s = 244°.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Normalized velocity distributions in Mars’ orbit for the OCCs at perihelion (L s = 251°). The color profiles show the results for all those diameters modeled by both the DMZC and the MIF. The solid-black line also represents the normalized overall flux for each meteoroid population as a function of the impact velocity. Note that both the profiles of the velocity distributions for the different particle sizes and the overall flux are normalized to an area equal to unity.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Temperature (panels (a) and (b)) and atmospheric density (panels (c) and (d)) profiles for two orbital positions: L s = 90° (northern summer/southern winter) and L s = 270° (northern winter/southern summer) as a function of the altitude and the latitude at Mars. These data correspond to the MCD.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the average velocity distribution (in kilometers per second) of meteoroids into the Martian atmosphere modeled by the MIF model for the OCCs and three orbital positions: aphelion (L s = 71°, (a)), perihelion (L s = 251°, (b)), and first crossing of the ecliptic plane (L s = 325°, (c)). These distributions are represented as a function of the Local True Solar Time and the latitude at Mars.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Seasonal variability of the mass input with the orbital position for the JFCs (dark-blue line), ASTs (light-blue line), HTCs (yellow line), total mass input (black line), and total ablated (dashed red line). Note that the mass fluxes are expressed in tons sol−1 (1 solar day at Mars is equivalent to 1.0275 Earth days).
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Seasonal variability of the contribution to the total ablated mass determined by the CABMOD-MIF model for the JFCs (a), the ASTs (b), and the HTCs (c) as a function of the planetographic latitude and the solar longitude (L s). Panel (d) represents the seasonal variability of the total mass influx.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Seasonal variability of the contribution to the total mass influx determined by the CABMOD-MIF model for the JFCs (a), the ASTs (b), and the HTCs (c) as a function of the planetographic latitude and the solar longitude. Panel (d) represents the seasonal variability of the total mass influx.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Plot of 84Kr/36Ar vs. 132Xe/36Ar with several notable cosmochemical end-members: Solar (Lodders 2003; Meshik et al. 2014), CC gray box (range of the carbonaceous chondrite compositions; compilation from Bekaert et al. 2020), 67P/C-G (Rubin et al. 2018), and Early Atm (initial Earth atmospheric composition before Xe loss; Zahnle et al. 2018). Squares (blue and green; Bar-Nun & Owen 1998; Notesco et al. 2003) and orange diamonds (this study) show the composition of experimental cometary ices if formed from a solar composition at various temperatures of formation. Error bars for both this study and Notesco et al. (2003) represent the standard error of the repeated experiments for one temperature of formation at 1σ. Lines between symbols are for visual aid only. Starting from a solar composition, a depletion in Ar alone will lead to variation along the 1:1 (black dashed line) direction. All three experiments show variations along this line when increasing the temperature to 50–60 K. Both the Bar-Nun & Owen study and our work show a shift toward higher 132Xe/36Ar when forming ice above 60 K. Although this shift appears critical to reach the observed composition of 67P/C-G, none of those experiments achieve it.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: The N2 and noble gas release during the heating from 28 to 200 K at a rate of 1  K minute−1 of a representative experiment starting with a H2O:N2:Ar:Kr:Xe mixture. A fraction of each guest species is frozen on or below the ice and sublimates at the respective sublimation temperature, while the trapped fractions are released simultaneously at around 145 K, before water starts sublimating at 160 K. Note the log scale for the signal intensity.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Schematic representation of the EXCITING experiment. v: high vacuum valve. μv: micrometer flow control valve. Cryo: cryogenic trap (see Figure 2). IG: ion gauge. QMS: quadrupole mass spectrometer. The NG bottle contains noble gases (Ar, Kr, and Xe) and nitrogen, L1 and L2 refer to the two loops of gas flow discussed in the main text, and P1 and P2 are two turbomolecular pumps.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Xenon gas release during the heating from 28 to 180 K at a rate of 1  K minute−1 of a representative experiment starting with an H2O:Xe mixture. Peaks corresponding to frozen Xe sublimation and release of trapped Xe are observed at ∼75 and ∼140 K, respectively. The two-step release of trapped Xe at 135 and 144 K is discussed in the main text. Water sublimation is clearly observed from 160 K. The apparent decrease of the H2O background signal when Xe is released results from a competition (or pressure effect) inside the QMS, since Xe has a slightly lower FIP (Xe-FIP = 12.13 eV) than water (H2O-FIP = 12.65 eV).
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: The N2/Ar, Kr/Ar, and Xe/Ar ratios of the five duplicates of the experiment at 28 K (dashed lines) as a function of temperature rise between 135 and 148 K, around the release peak of trapped gas. For each elemental ratio, the thick line is the average of the five repeats, and the shaded envelope is the standard deviation of the five repeats at 1σ. The reproducibility is maximal around the peak of gas release between 143 and 146 K. The elemental ratios given in Table 1 are the integrated ratios over the duration of gas release and thus reflect the value of the ratios at the release peak.
Paper: The EXCITING Experiment Exploring the Behavior of Nitrogen and Noble Gases in Interstellar Ice Analogs
Authors: Matthieu G. Almayrac, David V. Bekaert, Michael W. Broadley, David J. Byrne, Laurette Piani, Bernard Marty
Figure caption: Diagram of the cryogenic head system allowing noble gases/water mixtures to be condensed at ∼30 K under high vacuum and exposed to Lyα light (with a H2D2 light source unit L11798 by the Hamamatsu company). HV: high vacuum. UHV: ultrahigh vacuum.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: Steady-state solutions of (a) separation velocity (cm yr−1), (b) solid overpressure (MPa), and (c) melt fraction for a case with η  l  = 10 and η  s  = 1020 Pa s. Colors indicate the amount of tidal heating, corresponding to 50 (red), 200 (orange), 400 (green), and 550 TW (blue). The thickness of a high-melt-fraction layer (ϕ > 20%; gray dashed in (c)) exceeds 50 km only when the rate of tidal dissipation is larger than 550 TW.
Paper: A Subsurface Magma Ocean on Io: Exploring the Steady State of Partially Molten Planetary Bodies
Authors: Yoshinori Miyazaki, David J. Stevenson
Figure caption: Schematic illustration of Io’s interior with (a) a magmatic sponge and (b) a subsurface magma ocean. An enlarged view of eruption through the crust is also shown on the right. Parameters defined in Sections 2 and 4.1 are labeled to the corresponding reservoirs. Our results suggest that a magmatic sponge would swiftly separate into two phases and create a magma ocean, which is a rheologically liquid layer with ϕ > 0.4. It is noted that the crust and the partially molten layer are connected by a transition zone, where upwelling magma solidifies to heat the subsiding crust (Section 4.2).
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Mass ablated fraction of a meteor, f  ab , estimated by the CABMOD model as a function of initial diameter and entry velocity, and a fixed ZA of 45°. The left panel shows the ablated fraction for a Martian latitude of −90° and a solar longitude L s = 90° (northern summer/southern winter), and the right panel represents a Martian latitude of 60° and a solar longitude L s = 270° (northern winter/southern summer). The dashed red lines indicate the ablation fraction of a particle with an initial diameter of 200 μm entering at 20 km s−1. Note that particles ablate more efficiently for the atmospheric conditions represented in panel (a): the ablation efficiencies are 80% (left panel) and 60% (right panel), respectively. The wavy structure of the contours is an artifact caused by the discretization of the particle size distribution.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the relative mass influx of meteoroids into the Martian atmosphere determined by the MIF model for the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i) and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). These distributions are represented as a function of the LTST and the latitude at Mars. In all cases, the minimum mass influx occurs at aphelion. In contrast, the maximum mass input is located around the first crossing of the ecliptic plane for JFCs and ASTs, and at perihelion for HTCs.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the total injection rates (in atoms m−3 s−1) of Na (a, b, and c), Mg (d, e, and f), and Al (g, h, and i) estimated by the CABMOD-MIF model and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). The maximum ablation rates of the three metals appear at perihelion and for the Martian latitudes of 30° (Mg and Na) and −15° (Al). In the case of Al, this metal is comparatively more refractory than Na and Mg and, therefore, it is mainly injected at latitudes where small and fast particles are dominant (see Figures 4(h) and 5(h)). Note that the color scales are different for each meteoric metal.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the injection rates (in atoms m−3 s−1) of Mg estimated by the CABMOD-MIF model for the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i) and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, middle panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels). The corresponding latitudes of the maximum ablation rates of Mg are −20° for JFC (L s = 325°, (c)), −5° for the ASTs (L s = 325°, (f)), and 30° for the HTCs (L s = 251°, (h)), respectively. Note that the HTCs are comparatively the main mass contribution to the total injection rates. The color scales are different for each meteoroid population.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Seasonal variability of the total injection rates (in atoms m−3 s−1) of Na (a), Mg (b), and Al (c) estimated by the CABMOD-MIF model as a function of the pressure level (in pascals) and the Martian latitude at L s = 270° (northern winter/southern summer). Note that the color scales are different for each meteoric metal.
Paper: A Modeling Study of the Seasonal, Latitudinal, and Temporal Distribution of the Meteoroid Mass Input at Mars: Constraining the Deposition of Meteoric Ablated Metals in the Upper Atmosphere
Authors: Juan Diego Carrillo-Sánchez, Diego Janches, John M. C. Plane, Petr Pokorný, Menelaos Sarantos, Matteo M. J. Crismani, Wuhu Feng, Daniel R. Marsh
Figure caption: Diurnal variability of the fraction ablated of Na (left panels), Mg (middle panels), and Al (right panels) modeled by the CABMOD-MIF model for the JFCs (a, b, and c), the ASTs (d, e, and f), and the HTCs (g, h, and i) and three orbital positions: aphelion (L s = 71°, top panels), perihelion (L s = 251°, center panels), and first crossing of the ecliptic plane (L s = 325°, bottom panels).