adsabs/AstroCLIMB huggingface dataset:
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: The maximum possible eccentricity and mutual inclination between it and its companions achieved by an inner planet as a result of sweeping resonances given the inclinations/eccentricities of the outer planets. The reported maximum eccentricity and inclination values are found by calculating the predicted eccentricity and inclination excitation from a secular resonance. The inner planet’s initial eccentricity and inclination are set to 0.01 and 1°, respectively, for these calculations. These maximum values are not significantly affected by J 2 evolution, as J 2 serves primarily to move them rather than affect their magnitude (see Figure 2). Overplotted in white lines on the inclination panel are the contours within which the inner planet always transits, no matter its longitude of ascending node, for the labeled semimajor axis. The black dashed lines show the boundaries within which the two companion planets both always transit under the simplifying assumption that the inner of the two companion planets lies approximately on the line of sight. On the eccentricity panel are shown the contours within which δ is above the given value, for an inner planet with a  in  = 0.046, as well as the contour within which the inner planet does not cross the Roche Limit ﹩{R}_{L}={R}_{p}{(2{M}_{\star }/{M}_{p})}^{1/3}﹩ for a in = 0.046.
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: HD 106315's inner planet. Results of 1000 systems, represented by blue dots, integrated up to 2 Gyr of HD 106315 with an Earth-mass planet introduced inward of the two observed warm Neptunes, and 220 N-body simulations, represented by green stars if they remained stable and by cyan stars if planet–planet scattering or ejection occurred. Cyan stars do not appear in the bottom row, because their maximum mutual inclinations are greater than 60°. The left column represents initial J 2 = 2 × 10−5, while the right column represents J 2 = 6 × 10−4; these two values represent the bottom and top curves in Figure 1. The top row indicates for each run the minimum value of δ (see Equation (17)) achieved over the entire run. The shaded regions represent regions of instability, either from Roche limit crossing (left) or orbit crossing indicated by δ = 0 (right). The middle row indicates the maximum eccentricity achieved by the inner planet over each run. The bottom row indicates the maximum mutual inclination between the inner planet and the two warm Neptunes over the course of the run. The red curve indicates the maximum mutual inclination that the inner planet can have with its closest neighbor and still transit.
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: A range of possible J 2 evolutions for a 1.1 M ⊙ star after the evaporation of the disk as a function of time.
Paper: Let’s Sweep: The Effect of Evolving J 2 on the Resonant Structure of a Three-planet System
Authors: Thea H. Faridani, Smadar Naoz, Gongjie Li, Nicholas Inzunza
Figure caption: Comparison of the inner planet’s eccentricity and mutual inclination with the middle planet when calculated with the secular code used throughout this work (blue, central) and the N-body integrator HNBody (orange, outer). The blue curve is a subsection of the evolution of the inner planet in Figure 3, and the orange curve was initialized with the orbital elements and J 2 value of all planets 1.591  Gyr into the evolution shown in Figure 3.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Same as Figure 9 but for all of the regions.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Left: the HCO+ J = 1−0 spectra in the AS 209 disk for each unique observation day. The gray bars on the left represent the maximum and mean error (standard deviation) for all channels across all observations. Appendix B shows the spectra with error bars on each channel. Right: the disk-integrated continuum flux (F cont, bottom), disk-integrated HCO+ 1–0 flux (﹩{F}_{{\mathrm{HCO}}^{+}}﹩, middle), and normalized line flux with respect to the continuum (﹩{F}_{{\mathrm{HCO}}^{+}}/{F}_{\mathrm{cont}}﹩, top) for each day HCO+ 1–0 was observed in AS 209. Units for ﹩{F}_{{\mathrm{HCO}}^{+}}/{F}_{\mathrm{cont}}﹩ are mJy km s−1 mJy−1. Error bars indicate 1σ. Gray dashed lines in the bottom plot indicate ±10% of the average continuum flux.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: The moment-zero map of HCO+ 1–0 for each observation execution for each disk. Each column corresponds to a different disk, while each row represents a separate observation day. The date of observation is shown in the top of each plot. Each disk has its own unique color bar with units in mJy. The beam for each disk is shown in white in the bottom left of the top row of images.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: The 90 GHz continuum emission for each observation execution for each disk. Each column corresponds to a different disk, while each row represents a separate observation day. The date of observation is shown in the top of each plot. Each disk has its own unique color bar with units in mJy. The beam for each disk is shown in white in the bottom left of the top row of images.
Paper: Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar
Authors: M. Fernández-López, J. M. Girart, J. A. López-Vázquez, R. Estalella, G. Busquet, S. Curiel, N. Añez-López
Figure caption: Ulrich (solid lines) and Mendoza (dashed lines) orbits overlapped with moment 0 of CH3OH 3(1,2)−2(0,2) emission. The same description as Figure 27 but models using the envelope radius r in = 790 au.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Same figure description as Figure 3, but for HD 163296.
Paper: MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission
Authors: Abygail R. Waggoner, L. Ilsedore Cleeves, Ryan A. Loomis, Yuri Aikawa, Jaehan Bae, Jennifer B. Bergner, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Charles J. Law, Romane Le Gal, Feng Long, Karin I. Öberg, Richard Teague, David J. Wilner
Figure caption: Same figure description as Figure 3, but for GM Aur.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME observed by Wind on 2020 April 20–21 at 1 au. Panel (a) shows magnetic field ( B ) magnitude and GSE components, (b) magnetic field latitudinal (θ  B ), and (c) azimuthal (ϕ  B ) angular components with respect to the ecliptic plane, (d) proton velocity ( V ), (e) density (n, black) and temperature (T, red), and (f) proton plasma-β. The vertical lines indicate the shock (solid red), the beginning of the mixing layer (dotted red) front boundary of the ICME (solid magenta), the magnetic cloud (dotted magenta and blue), and the rear boundary of the ICME (solid blue). In panel (d), −V  X  is shown to facilitate comparison. Abbreviations: ML  (mixing layer), MCFR (magnetic cloud front region), and MCRR (magnetic cloud rear region).
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: The spacecraft positions and the magnetic field measurements during the ICME front boundary passage on 2020 April 20. Panel (a) shows the spacecraft positions in the GSE XY plane, (b) the YZ plane in Earth radii (R E) and the magnetic field (c) magnitude, (d) the GSE X component, (e) the Y component, and (f) the Z component. The solar wind monitor and Themis C measurements are time shifted relative to MMS and Cluster using the solar wind velocity measurements and spacecraft separation along the X-axis. In panel (e), the pale magenta curve highlights the B  Y  changes discussed in the text for Themis C. Abbreviations: S/C (spacecraft).
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by the Themis C spacecraft. Panel (a) shows the magnetic field magnitude, (b) the field components in the local LMN coordinates, (c) proton (blue) and electron (red) densities, (d) proton velocity and the Walén prediction of V  L  from the sheath (ejecta) side on black (gray), (e) electron velocity, (f) the diamagnetic current density, and (g) the parallel (∣∣, solid) and perpendicular (⊥, dotted) proton and electron temperatures relative to the magnetic field.
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by the Wind spacecraft. Panel (a) shows the magnetic field magnitude, (b) the field components in the local LMN coordinates, (c) proton (blue) and electron (red) densities, (d) proton velocity and the Walén prediction of V  L  from the sheath (ejecta) side on black (gray), (e) electron velocity, and (f) the diamagnetic current density ( J   D ).
Paper: Multipoint Observations of the Dynamics at an ICME Sheath–Ejecta Boundary
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Julia Ruohotie, Mojtaba Akhavan-Tafti, Simon W. Good, Emilia K. J. Kilpua
Figure caption: ICME front boundary on 2020 April 20 observed by the DSCOVR and ACE spacecraft. Panels (a) and (b) show the magnetic field magnitude, and (c)–(f) the field components in local LMN coordinates. The blue shading in panels (a)–(d) displays the intervals that determine the normal directions. The red bars indicate the intervals shown in panels (e) and (f).
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Best-fit values of the nonthermal parameters in the zira, srcut, and power-law scenarios, as a function of the region and for different analysis setups. Error bars are estimated at the 90% confidence level. Each color represents the instrument used and the energy range considered: black for Chandra in the 4–6 keV band; red for NuSTAR data in the 4–5.5 keV band; purple for NuSTAR in the 9–15 keV band; and cyan for NuSTAR in the 15–40 keV band.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: NuSTAR (black), INTEGRAL (green), and SWIFT (red) spectra of Cas A fitted with different models. The normalization of each spectrum is readjusted to the NuSTAR ones through the setplot area command available within XSPEC. The solid line represents the model. Panels from top to bottom: spectra are fitted with the zira, srcut, and pow/jitter model, respectively (the jitter model provides the same description as the pow). Left column panels: NuSTAR spectra from all of the observations are simultaneously fitted. All of the spectra are rebinned for graphical purposes. Right column panels: NuSTAR spectra from all of the observations are combined.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: NuSTAR spectra from the NW (top line), N (central line), and SW (bottom line) regions fitted with the srcut (left column), jitter (central column), and pow (right column) models in 4–5.5 keV and 9–40 keV and with corresponding residuals.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Values of ﹩{\chi }_{r}^{2}﹩ for fits performed with different nonthermal models in the 4–6 keV, 9–15 keV, and 15–40 energy bands of the NuSTAR spectra. Black, green, and blue represent models with a power-law, srcut, and zira component, respectively.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: NuSTAR spectra in the 4–5.5 keV and 9–40 keV compared with the best-fit model (solid line) obtained by fitting only the 4–5.5 keV band for regions NW (on the left) and SW (on the right). The yellow area marks the spectral region in which the fit is performed. Each panel shows the 4–6 keV best-fit value of the nonthermal parameter considered: Γ, E break (in keV units), and E cut (in keV units) for the pow, srcut, and zira models, respectively.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Ratios of nonthermal to total flux in the 4–6 keV band obtained from the fits in the 0.5–8 keV band as a function of the region.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Same as Figure 7 but here the fit is performed in the 15–40 keV band and extrapolated down to 3 keV.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Same as Figure 7 but for all of the regions considered.
Paper: Jitter Radiation as an Alternative Mechanism for the Nonthermal X-Ray Emission of Cassiopeia A
Authors: Emanuele Greco, Jacco Vink, Amael Ellien, Carlo Ferrigno
Figure caption: Same as Figure 8 but for all of the regions.
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: Broadband fluence spectra for three GRBs with detections or limits on the dust scattering. The spectra for GRB 230307A (red) are from Sun et al. (2023). For GRB 221009A (black) we indicate the best estimate (solid) and the maximum and minimum values (dashed) for the soft X-ray fluence derived from the analysis of dust scattering rings (Tiengo et al. 2023), while the gamma-ray spectrum is from Frederiks et al. (2023). For GRB 031203 (blue) we indicate two estimates of the soft X-ray fluence from dust scattering analysis by Tiengo & Mereghetti (2006) (lowest) and Watson et al. (2006) (highest), while the gamma-ray spectrum is from Vianello et al. (2009).
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: EPIC-pn image in the 0.3–10 keV energy range of the field of GRB 230307A. The yellow circles show the expected position of scattering rings produced by dust in the Magellanic Bridge, for distances of 50 kpc (outermost circle) and 70 kpc (innermost circle). The sources listed in Table 1 are indicated by the small circles.
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: X-ray flux between 0.3 and 10 keV of GRB 230307A (black histogram: LEIA) and its afterglow (blue: Swift/XRT; red: XMM-Newton/EPIC; green: Chandra/ACIS-S). The light curve of the afterglow has been fitted with a power law in the range T 0 + [1.3, 25.3] days (dashed line).
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: Top panel: EPIC-pn (black), -MOS1 (red), and -MOS2 (green) spectra of the afterglow of GRB 230307A fitted with an absorbed power law. The blue dashed line indicates, for comparison, the spectrum expected with the intrinsic absorption ﹩{N}_{{\rm{H}}}^{{\rm{HOST}}}=2.73\times {10}^{21}﹩ cm−2 measured in the prompt emission. Bottom panel: residuals of the best fit in units of σ.
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: Pseudo-distance distribution extracted from EPIC-pn and -MOS events in the 0.5–4 keV energy range. The red line represents the best power-law fit to the data, while the vertical dashed lines indicate the relevant distance range for the analysis of interstellar dust in the Magellanic Bridge.
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: Light curve of GRB 230307A at energies above 75 keV obtained with the SPI/ACS detector. The bin size is 50 ms. The inset shows a zoom of the initial part.
Paper: XMM-Newton and INTEGRAL Observations of the Bright GRB 230307A: Vanishing of the Local Absorption and Limits on the Dust in the Magellanic Bridge
Authors: Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Andrea Tiengo, Dominik P. Pacholski
Figure caption: Confidence contours (1σ, 2σ, and 3σ) of photon index Γ and absorption at the GRB redshift ﹩{N}_{{\rm{H}}}^{\mathrm{HOST}}﹩.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: IR absorbance spectra of the initial gas mixture H2:CH4:N2 (99%:0.5%:0.5%) at ambient temperature (black) and after 22 hr of heating at different set temperatures: 473 K (red), 673 K (blue), 873 K (green), and 1073 K (violet). Spectra have been offset for clarity.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Difference of absorbance after irradiation (A irradiation) and before irradiation (A heating) for the H2:CH4:N2 (99%:0.5%:0.5%) gas mixture and for different gas temperatures—ambient temperature (black) and different set temperatures: 473 K (red), 673 K (blue), 873 K (green), and 1073 K (violet). Spectra have been offset for clarity.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Transmission of UV photons at Ly α  (121.6 nm) through the 48 cm long gas cell as a function of the distance to the UV lamp at the beginning of the experiments, considering the absorption by CH4 for the H2:CH4:N2 gas mixture and by CH4 and H2O for the H2:CH4:H2O gas mixture.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: IR absorbance spectra of the initial gas mixture H2:CH4:H2O (98.4%:0.8%:0.8%) at ambient temperature (black) and after 22 hr of heating at different set temperatures: 473 K (red), 673 K (blue), 873 K (green), and 1073 K (violet). Spectra have been offset for clarity.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Contributions from the different temperature regions of the cell to the spectrum of CH4 simulated for the H2:CH4:N2 (99%:0.5%:0.5%) gas mixture after 22 hr at a set temperature of 673 K. The simulated spectrum is shown in Figure 8.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: IR absorbance spectra of the H2:12CH4:N2 (99%:0.5%:0.5%) gas mixture (bottom) and the H2:13CH4 (99.4%:0.6%) gas mixture (top) after 22 hr of heating at 1073 K. Spectra have been offset for clarity.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Mixing ratios of CO after 22 hr of heating, methane consumption efficiency (﹩{e}_{{\mathrm{CH}}_{4}})﹩, and mixing ratios of C2H6, CO, and C2H2 after 24 hr of irradiation of the H2:CH4:N2 gaseous mixtures at ambient temperature (295 K) and the different set oven temperatures: 473, 673, 873, and 1073 K.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Top: methane consumption efficiency (﹩{e}_{{\mathrm{CH}}_{4}}﹩) and mixing ratios of C2H6 and C2H2 after 105 s as calculated by the 0D thermo-photochemical model for an H2:CH4:N2 (99%:0.5%:0.5%) gas mixture at different temperatures: 295, 473, 673, 873, and 1073 K. Bottom: methane consumption efficiency (﹩{e}_{{\mathrm{CH}}_{4}}﹩) and mixing ratios of C2H6 and C2H2 after 105 s as calculated by the 0D thermo-photochemical model for an H2:CH4:N2:H2O (98.99%:0.5%:0.5%:0.01%) gas mixture at different temperatures: 295, 473, 673, 873, and 1073 K.