adsabs/AstroCLIMB huggingface dataset:
Paper: Beyond Point Masses. III. Detecting Haumea’s Nonspherical Gravitational Field
Authors: Benjamin C. N. Proudfoot, Darin A. Ragozzine, William Giforos, Will M. Grundy, Mariah MacDonald, William J. Oldroyd
Figure caption: The change in Hi’iaka’s light-curve amplitude over time. Using the integrations similar to those shown in Figure 6, we calculate the light-curve amplitude using Equation (1) from Hastings et al. (2016). Note that the x-axis is different than Figure 6. Axis ratios were chosen to be similar to other solar system objects at similar size, as well as approximately matching the light-curve amplitude found in the literature (Hastings et al. 2016). The no-precession case is found by taking a fixed pole direction. The fast variations in these functions are due to Earth’s heliocentric orbit. Even for small obliquities, the light curve evolves significantly differently than the no-precession case. As in Figure 6, we find that the aligned case (0°) still shows precession and slightly different light-curve evolution when compared to the no-precession case. Long-term monitoring of Hi’iaka’s light curve may permit direct measurement of its spin pole over decadal timescales.
Paper: Beyond Point Masses. III. Detecting Haumea’s Nonspherical Gravitational Field
Authors: Benjamin C. N. Proudfoot, Darin A. Ragozzine, William Giforos, Will M. Grundy, Mariah MacDonald, William J. Oldroyd
Figure caption: The precession of Hi’iaka’s spin axis based on its initial obliquity. Similar to Figure 5, we show the precession of Hi’iaka’s spin axis in terms of ecliptic longitude and latitude. Initial integration parameters have been chosen to be representative of the posterior found in Table 2. The moments of inertia of Hi’iaka were chosen to be similar to objects of similar size, although their values only change the frequency of the precession. For different initial obliquities, we find different precession periods, matching analytical theory and results in the literature (e.g., Hastings et al. 2016). Interestingly, there are small variations when Hi’iaka’s spin is initially aligned with its orbit. Although initially there would be no net torque and no precession when aligned, since Hi’iaka’s orbit precesses the alignment is broken and precession begins.
Paper: Beyond Point Masses. III. Detecting Haumea’s Nonspherical Gravitational Field
Authors: Benjamin C. N. Proudfoot, Darin A. Ragozzine, William Giforos, Will M. Grundy, Mariah MacDonald, William J. Oldroyd
Figure caption: The normalized residuals of the best parameter set from our HST-only (nonrobust) orbit fit. x and y correspond to ecliptic longitude and latitude, which is the primary coordinate system used in MultiMoon. Hi’iaka residuals are shown as circles and Namaka with triangles. The color of each point corresponds to the observation date. The circles correspond to 1, 2, and 3σ error contours. As reported in the text, this fit corresponded to a reduced χ 2 ∼ 1.10. We find that although the fit quality is worse than would be desired, the p-value associated with the χ 2 statistic is 0.23, indicating an acceptable fit.
Paper: Beyond Point Masses. III. Detecting Haumea’s Nonspherical Gravitational Field
Authors: Benjamin C. N. Proudfoot, Darin A. Ragozzine, William Giforos, Will M. Grundy, Mariah MacDonald, William J. Oldroyd
Figure caption: Chaotic rotation of Namaka. When initialized, Namaka rotates once every 6 days and is aligned with its orbit. After just a few decades, Namaka becomes attitude-unstable and begins to tumble. Chaos is a natural consequence of Namaka’s eccentric orbit and is inevitable if Namaka has been substantially despun. In this sense, Namaka is very similar to Saturn’s satellite Hyperion, which chaotically rotates due to its eccentric orbit around Saturn (Wisdom et al. 1984; Klavetter 1989).
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The left panel shows the MOID − ΔToF for asteroid 4544 Xanthus with 99942 Apophis for 105 clones. The density indicates the relative probability under the observational uncertainty, as determined by JPL (left) and NeoDys (right).
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2026 December approach of asteroid 2009 JG2 to 99942 Apophis (103 clones). The right panel is zoomed in on a region near the origin.
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2023 December approach of asteroid 2016 FB12 to 99942 Apophis (103 clones). The right panel is zoomed in on a region near the origin.
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF plot for the 2026 December approach of asteroid 2016 CL18 to 99942 Apophis (103 clones). The threshold region of Equation (4) is shown in light blue. The JPL and NeoDys solutions put the asteroid into nonoverlapping regions of space approximately 10,000 km apart.
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2023 December approach of asteroid 373135–99942 Apophis (103 clones).
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2017 July approach of asteroid 2014 AD16 to 99942 Apophis (103 clones).
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2028 February approach of asteroid 2022 KN3 to 99942 Apophis (103 clones). The right panel is zoomed in on a region near the origin.
Paper: Encounter Circumstances of Asteroid 99942 Apophis with the Catalog of Known Asteroids
Authors: Paul Wiegert, Benjamin Hyatt
Figure caption: The MOID − ΔToF for the 2025 October approach of asteroid 25143 Itokawa to 99942 Apophis (103 clones).
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Plots of the relative abundances of craters in the labeled groups as a function of angular distance from the apex of motion, calculated in 30° bins and plotted every 10°. The green dotted curve is calculated for a purely leading/trailing asymmetry from Wang & Zhou (2016). The black dotted curves represent the calculated random population of 100,000 craters uniformly distributed on a sphere, scaled by the fraction of highland terrain in each 0.°1 × 0.°1 box, and truncated at ±70° latitude (panels (a)–(d) and (g)), or ±42° latitude and including 70° to 290° E longitude (panels (e) and (f)). MF2003 = craters from Morota & Furumoto (2003b); MF2003 region = our albedo-rayed craters located within the study area of Morota & Furumoto (2003); cold spots are from Williams et al. (2018). Error bars are 1/N 1/2.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Size–frequency plots for highland rayed craters; left: near vs. far-side craters; right: leading vs. trailing hemisphere craters. Both plots are normalized to the appropriate area of highland terrain.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: CSFD plots of highland albedo-rayed craters with and without rocks (left) and highland albedo-rayed craters and highland rocky craters (right). Both plots are normalized to the area of highland terrain in the study region. Dotted curves are Neukum et al. (2001) isochrons, labeled in Gyr.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Cumulative (left) and differential (right) size–frequency plots of highland craters in our database. Dashed/dotted curves labeled with numbers are isochrons calculated using Neukum et al. (2001), labeled in Gyr. In the left panel, orange symbols are all the Robbins (2019) craters in the highlands with diameters 1–200 km.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Normalized cumulative histograms of latitudinal distribution of highland craters, scaled by the area in each latitude band. The uniform population here represents 100,000 random craters drawn from a uniform-on-a-sphere distribution (of which 82,829 fall in the highlands), scaled by both by area and fraction of highland terrain in each 0.°1 latitude band.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Normalized differential histograms of latitudinal distribution of highland craters, scaled by the area in 0.1° latitude bands. Top left: albedo rays; top right: thermophysical rays; bottom left: rocks; bottom right: uniform random distribution of 500 craters scaled by area and by fraction of highland terrain in each latitude band.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: CSFD plots of albedo-rayed craters with and without rocks (left) and albedo-rayed craters and rocky craters (right), all in the maria. Both plots are normalized to the area of mare terrain in the study region. Dotted curves are Neukum et al. (2001) isochrons, labeled in Gyr.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Normalized cumulative histograms of diameter distributions of rayed and rocky craters on lunar near- and far-hemisphere highlands, normalized by area of highlands in each region.
Paper: The Population of Young Craters on the Moon: New Catalog and Spatial and Temporal Analysis
Authors: Rebecca R. Ghent, Emily S. Costello, A. H. Parker
Figure caption: Map (sinusoidal projection) of mare regions between 70° S and 70° N, used for area calculations.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: Example of a Pourbaix diagram of the Fe–O–H system. The driving variables are the pH and reduction potential Eh; the latter values are expressed relative to the standard hydrogen electrode. Eh is a measure of the oxidation state of the system. Within a region demarcated by black lines, the indicated species/mineral is the most stable form of iron. The aqueous species regions are shaded in color to highlight that they are of greatest interest in the present application of measuring soluble salts from samples of ocean water. The sizes of their regions depend on the activity of the species. Here they are assumed to have activities of 10−6—close to our experimentally determined detection limit for ferric sulfate. Dashed lines show cases of strongly oxidized and reduced conditions as points of reference. This diagram was constructed using thermodynamic data from the SUPCRT database (Helgeson 1978; Shock et al. 1997), together with the Nernst equation. Note: Fe2O3 = hematite, Fe3O4 = magnetite, Fe0 = native iron.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: Simplified interpretations of the (non)detection and characterization of iron in ice grains from ocean worlds with SUDA-type instruments. Three scenarios are considered: (a) detection of Fe (II)-dominated grains, (b) detection of significant Fe (III) in ice grains, and (c) no Fe detection. In addition to iron, the detection of aluminum ions (Al3+) in ice grains would support a salt source from an acidic ocean composition. In both scenarios (a) and (b), the case of ice grains originating from a plume (i.e., fresh surface material) is distinct from ice grains originating from the surface, where older material has likely undergone oxidation. In the case of surface material, the age of this material may be constrained by investigating its surface appearance, including geological features. In case (c), the characterization of the pH (e.g., by detection in the grains of other ions, like hydroxide) could put constraints on the oxidation state in the case of a circumneutral pH, while the case of a low pH would hint at a nonoceanic fluid origin (e.g., a perched melt of water and sulfuric acid) of the ice grains (as seen in Figure 5, iron is soluble at low pH, whatever the oxidation state of the ocean). In the case of a high-pH ocean, iron would not be present as ions (but incorporated in very poorly soluble minerals; Figure 5) and therefore not detectable in ice grains.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID cation mass spectra recorded with a delay time of 5.1 μs for (a) iron (II) chloride (FeCl2), with an example of the iron isotope pattern for [Fe2+ (OH)]+, and (b) iron (III) chloride (FeCl3). In the spectrum in panel (b), two distinct peaks are observed at m/z 73 at a similar intensity, corresponding to a pure water cluster [H3O(H2O)3]+ and to [Fe2+(OH)]+ (Figure A2).
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID anion mass spectra recorded with a delay time of 6.0 μs for (a) iron (II) chloride (FeCl2) and (b) iron (III) chloride (FeCl3).
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID anion mass spectra recorded with a delay time of 5.4 μs for (a) iron (II) sulfate (FeSO4) and (b) iron (III) sulfate (Fe2[SO4]3).
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: Zoomed-in section of the LILBID cation mass spectra of iron (III) chloride (FeCl3), recorded with a delay time of 5.1 μs. Two distinct peaks are observed at m/z 73 at a similar intensity, corresponding to a pure water cluster [H3O(H2O)3]+ (m/z 73.05) and to [Fe2+(OH)]+ (m/z 72.94). To resolve the two peaks, a mass resolution of about 500 is required.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: The LILBID laboratory setup coupled to a ToF mass spectrometer, reproducing the impact ionization mass spectra of ice grains recorded in space (figure reproduced from Klenner et al. 2019). The principle of delayed extraction of the ions as a function of their initial velocities is shown in the lower right inset.
Paper: Probing the Oxidation State of Ocean Worlds with SUDA: Fe (II) and Fe (III) in Ice Grains
Authors: Maryse Napoleoni, Lucía Hortal Sánchez, Nozair Khawaja, Bernd Abel, Christopher R. Glein, Jon K. Hillier, Frank Postberg
Figure caption: LILBID cation mass spectra of iron (II) chloride (FeCl2), recorded with a delay time of 4.5 μs.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Bias introduced by the PSF on the dopplergrams and its suppression thanks to the first-order developments of F m and v d (Equations (A4) and (A5)). Left panel: simulation of the difference between the measured and true velocity maps v m − v d, i.e., the velocity bias, introduced by a 2″ Gaussian PSF. The image used in this simulation is the same as with Figure 10. For the velocity map, we employed a solid-body rotator with Jupiter’s period measured in the system III. Middle panel: difference between the measured data and the estimate of the true dopplergram ﹩\widehat{{v}_{{\rm{d}}}}﹩ obtained by applying Equation (A15). Right: difference between the true and retrieved velocity maps ﹩\widehat{{v}_{{\rm{d}}}}-{v}_{{\rm{d}}}﹩. Color bars indicate line-of-sight velocities expressed in m s−1.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Effect of the PSF on an image of Jupiter taken by HST. The top left image was taken by HST on 2018 April 17 and is used as F(x, y). The bottom left image is the same but convolved by a Gaussian PSF corresponding to a seeing of 1.″5; it corresponds to F m(x, y). The middle panel shows a cut of F (black) and F m (red) along the x-axis in the equatorial region, while the right panel shows a cut along the y-axis at the central meridian. The PSF P is represented under the photometric profiles as a blue line. The HST image has the observation ID idg216i9q and is available on the MAST. It was rectified from the 133.°2508 inclination on the detector with a bilinear interpolation.
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Normalized zonal reflectivity profile corresponding to the 502 nm OPAL map (red) compared to the normalized profile of −∇  h  ·  u   h  from the JIVE data (blue).
Paper: Three-dimensional Atmospheric Dynamics of Jupiter from Ground-based Doppler Imaging Spectroscopy in the Visible
Authors: Francois-Xavier Schmider, Patrick Gaulme, Raúl Morales-Juberías, Jason Jackiewicz, Ivan Gonçalves, Tristan Guillot, Amy A. Simon, Michael H. Wong, Thomas Underwood, David Voelz, Cristo Sanchez, Riley DeColibus, Sarah A. Kovac, Sean Sellers, Doug Gilliam, Patrick Boumier, Thierry Appourchaux, Julien Dejonghe, Jean Pierre Rivet, Steve Markham, Saburo Howard, Lyu Abe, Djamel Mekarnia, Masahiro Ikoma, Hidekazu Hanayama, Bun'ei Sato, Masanobu Kunitomo, Hideyuki Izumiura
Figure caption: Projection factors of the Doppler velocity for the three components of the motion. The projection factors shown here are calculated for an oblate planet, with an inclination of 3°, Jupiter’s typical inclination during the observations of 2018, and a phase of 4°, the maximum value during that period. The projection factors are calculated for the time of each image used in the treatment. Left: zonal component. Middle: meridional. Right: vertical motion.
Paper: Heat-flux-limited Cloud Activity and Vertical Mixing in Giant Planet Atmospheres with an Application to Uranus and Neptune
Authors: Huazhi Ge, 华志 葛, Cheng Li, Xi Zhang, Chris Moeckel
Figure caption: Conceptual art about cloud formation and moist convection in the atmosphere of different planets. Panel (a) shows that solar radiation is the driving force and the energy source of cloud formation in Earth’s atmosphere. On the other hand, panel (b) shows that the planetary heat flux is the driving force of cloud formation on giant planets since solar radiation stabilizes the atmosphere and against convection. Note that the concept in (b) is also applicable to free-floating substellar bodies like field brown dwarfs but not applicable to strongly irradiated giant planets like hot or warm Jupiter. Cloud morphology in this art does not necessarily represent the real ones.
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: QCM-derived mass-loss rate during warming of a H2O + NH3 + O3 sample (20:75:5; solid), of a H2O:HNO3 sample (dotted), and of a H2O + O3 sample (95:5; dashed).
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectra of a H2O + NH3 + O3 sample (68:24:8) during warming at a rate of 1.0 K minute−1. Spectra correspond to 50 K (black), 123 K (red), and 207 K (blue). The 50 and 123 K spectra are vertically offset for clarity. Inset: highlighting the fundamental O–H stretching region of the 207 K spectrum (note the significantly smaller optical depth scale).
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: Normalized band area for the 1033 cm−1 O3 absorption band in H2O + NH3 + O3 (25:70:5) samples deposited at 50 K and warmed at a rate of 5 K minute−1 to an isothermal annealing temperature (75.6 K, triangles; 80.6 K, open circles; 90.6 K, closed circles) and held for 24 hr. Inset: Arrhenius plot for the H2O + NH3 + O3 reaction. The temperatures used correspond to 75.6, 77.2, 78.7, 80.6, 82.7, 84.1, 85.6, 87.7, and 90.6 K.
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectrum of a H2O + NH3 + O3 sample (20:75:5) warmed at a rate of 0.1 K minute−1 to 200 K. Inset: the NIR region of the absorption spectrum.
Paper: Thermal Oxidation Reaction between NH3 and O3: Low-temperature Formation of an ﹩{\mathrm{NH}}_{4}^{+}﹩-bearing Salt
Authors: Patrick D. Tribbett, Mark J. Loeffler
Figure caption: IR spectra of a H2O + NH3 + O3 sample (20:75:5) warmed at a rate of 0.1 K minute−1 to 120 K (bottom, black), of partially crystalline ammonia hemihydrate or 2NH3:H2O at 123 K (middle, red), and of an amorphous H2O + HNO3 (1:1) mixture at 122 K (top, blue). Spectra are vertically offset for clarity.