adsabs/AstroCLIMB huggingface dataset:
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Scans along the tails of the SPACEOBS images. The panels are labeled (a)–(i), corresponding to the dates shown in Table 2 (“Code” column). The black lines correspond to the observations and the red line to the model. The horizontal axes are labeled in kilometers projected on the sky plane, and the vertical axes are expressed in mag arcsec−2. These scans were obtained using a single power-law size distribution with κ = −2.5. The total dust mass released is 3.2 × 107 kg.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Appearance of the ejecta tail on an image taken at the 1 m telescope of the LULIN Observatory in Taiwan on October 12, 18:19 UT (Lin et al. 2023). The upper panel is the original unstretched image, while the lower panel shows a heavily stretched display to show the double tail structure. Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Upper panel: SPACEOBS observation on 2022 October 16 (image labeled (c) in Table 2) of the ejecta barely showing the double tail structure. Lower panel: result of the simple Monte Carlo modeling. Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (d), (e), and (f) display the SPACEOBS images at the corresponding dates in Table 2, and panels (d1), (e1), and (f1) display the corresponding synthetic images generated with the simple Monte Carlo model. All images are stretched between 28 and 22 mag arcsec−2, except synthetic image (d1), which has been heavily stretched between 30 and 25 mag arcsec−2, barely showing the secondary tail north of the main tail. Axes are labeled in kilometers projected on the sky plane. North is up and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Isophote fields in the innermost regions for the earliest images, (a), (b), (c), and (d) (see Table 2). The observations are represented by black contours and the model by red contours. The isophote levels are 17, 19, 21, and 23 mag arcsec−2 for images (a) and (b) and 17, 19, and 21 mag arcsec−2 for images (c) and (d). Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (a), (b), and (c) display the SPACEOBS images at the corresponding dates in Table 2, and panels (a1), (b1), and (c1) display the corresponding synthetic images generated with the simple Monte Carlo model. All images are stretched between 28 and 22 mag arcsec−2. Axes are labeled in kilometers projected on the sky plane. North is up and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (g), (h), and (i) display the SPACEOBS images at the corresponding dates in Table 2, and panels (g1), (h1), and (i1) display the corresponding synthetic images generated with the simple Monte Carlo model. All images are stretched between 28 and 22 mag arcsec−2. Axes are labeled in kilometers projected on the sky plane. North is up and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Aperture photometry by BOOTES compared with the simple Monte Carlo model predictions. The solid line is the magnitude as given in the JPL-Horizons system.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (m), (n), and (o) display HST images on the corresponding dates in Table 3, and panels (m1), (n1), and (o1) display the corresponding synthetic images generated with the detailed Monte Carlo model described in Section 3.2. All images are stretched between 22 and 17 mag arcsec−2. Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panel (l) displays the central portion of image (l) (see Table 3), and panel (l1) displays the corresponding modeled image. The right panel depicts the isophote fields with contours at 20, 19, and 18 mag arcsec−2 (black contours correspond to the observation and red contours to the model). All panels are labeled in kilometers projected on the sky and oriented north up, east to the left.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (p) and (q) display HST images on the corresponding dates in Table 3, and panels (p1) and (q1) display the corresponding synthetic images generated with the detailed Monte Carlo model described in Section 3.2. All images are stretched between 22 and 17 mag arcsec−2. Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Panels (j), (k), and (l) display HST images on the corresponding dates in Table 3, and panels (j1), (k1), and (l1) display the corresponding synthetic images generated with the detailed Monte Carlo model described in Section 3.2. The HST images are stretched between 22 and 17 mag arcsec−2 and the modeled ones between 25 and 20 mag arcsec−2 to show the antisolar tail that would not be seen otherwise because of their thinness. Axes are labeled in kilometers projected on the sky plane. North is up, and east is to the left in all images.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Cumulative impacting dust mass on Didymos and Dimorphos during the 20 days following impact.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Linear momentum transferred per second to the surfaces of Didymos (red line) and Dimorphos (blue line) as a function of time since the DART impact.
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Schematic drawing of the vectors shown in Equation (3).
Paper: Characterization of the Ejecta from the NASA/DART Impact on Dimorphos: Observations and Monte Carlo Models
Authors: Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Jian-Yang Li, Alessandro Rossi, Fabio Ferrari, Masatoshi Hirabayashi, Eugene Fahnestock, Alain Maury, Robert Sandness, Andrew S. Rivkin, Andy Cheng, Tony L. Farnham, Stefania Soldini, Carmine Giordano, Gianmario Merisio, Paolo Panicucci, Mattia Pugliatti, Alberto J. Castro-Tirado, Emilio Fernández-García, ignacio Pérez-García, Stavro Ivanovski, Antti Penttila, Ludmilla Kolokolova, Javier Licandro, Olga Muñoz, Zuri Gray, Jose L. Ortiz, Zhong-Yi Lin
Figure caption: Light curves from HST images with a 0.″2 aperture (Li et al. 2023; black filled circles) compared with BOOTES photometry (with 6"–7" apertures depending on seeing conditions; red filled circles) and the model results (open circles connected by black and red solid lines for HST and BOOTES, respectively).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Unit contacts derived from mapping on the color-ratio mosaic derived from the FC color filters; the primary determiner of where contacts are defined is color.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Global data from the Dawn spacecraft used for this mapping effort, shown in simple cylindrical projection; north is up, centered on 0° latitude, and the scale is similar for each figure. (A) LAMO data overlaid on HAMO data. (B) FC color-ratio data (Nathues et al. 2022). (C) Hillshade map. (D) Digital Terrain Model. (E) VIR Band II center map. (F) VIR Band II depth map. (G) Eucrite abundance as interpreted from GRaND data. (H) GRaND hydrogen abundance.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Unit contacts derived from mapping on the FC clear filter mosaic; the primary determiner of where contacts are defined is morphology (topography, albedo, surface texture).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Selected craters and fossae shown in same field of view for (A) FC HAMO mosaic and (B) a mosaic of multispectral data in the wavelength range 0.44–0.98 μm. See Section 4 for a detailed explanation of the global mosaic.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Global hybrid map of Vesta (1:300k). Impact craters >5 km in diameter, and linear structures >5 km in length are shown. (a) Equatorial area (0°–45° latitude). (b) Polar areas (45°–90° latitude).
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Vesta as seen by Dawn. (a) Mosaic of images showing one hemisphere of Vesta. The central mound of the Rheasilvia impact structure can be seen at the bottom of the image. The three large craters in the center north of the image are the craters Marcia, Calpurnia, and Minucia from west to east; these are colloquially known as the “snowman” craters. (b) High-Altitude Mapping Orbit global mosaic showing some features and figure locations mentioned in this work. Image credit: NASA/JPL-Caltech/UCAL/MPS/DLR/IDA.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Type localities for map units and structures. Scales are as follows: for c2 Canuleia crater is ∼10 km diameter; for cf1, Numisia crater is ∼33 km diameter; for cf3, Calpurnia crater is ∼50 km diameter; for cf4, Licinia crater is ∼24 km diameter; for cf5, Oppia crater is ∼30 km short axis diameter; for lm, panel is ∼41 km across. All other panels are 60 km across.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: Contrast in ejecta color surrounding Rufillia and Octavia craters, plus the saturated, multicolor ejecta from the smaller Aelia crater. (A) FC HAMO mosaic. (B) FC color-ratio mosaic. (C) Hybrid map.
Paper: A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data
Authors: R. Aileen Yingst, Scott C. Mest, W. Brent Garry, David A. Williams, Daniel C. Berman, Tracy K. P. Gregg
Figure caption: The region with Perpennia, Serena, Rufillia, and Octavia craters shows the geologic contrast of the Rheasiliva outer flank unit 2, cratered terrain units cut by Divalia fossae, and the red-orange ejecta material from Octavia. (A) HAMO mosaic. (B) FC color-ratio mosaic.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Thermal evolution of Pluto for a (a) 100 km and (b) 50 km CH4-rich clathrate layer accreted early on at the top of the ice shell and (c) a 50 km dense layer of CO2-rich clathrates sedimented at the top of the rocky mantle. CH4-rich means that the clathrate layer has enough CH4 to be buoyant, whereas CO2-rich means that the clathrate layer does not have enough CH4 to make it buoyant (see Figure 3). This model assumes a “hot start” of Pluto’s interior following accretion that allows melting of the bulk of the volatile phase and formation of a global ocean at <10 Myr after Pluto’s formation. Pluto’s interior heats slowly from the decay of long-lived radioisotopes. Thermal metamorphism leads to the release of water from the silicates at temperatures beginning at ∼550 K, taking the petrological evolution model presented in Figure 5 as a reference.
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Volatiles released from metamorphism. Panel (a) illustrates Pluto’s mineral phase assemblage at 1000 MPa as a function of temperature. The left side of the plot shows the phase assemblage immediately after water–rock differentiation. Heating this assemblage causes mineral phase changes and organic matter breakdown, which release fluids. Although the IOM is depicted as one phase, its composition is continuously evolving with higher temperature as it breaks down. Panel (b) plots volatile release from the breakdown of IOM (data from Okumura & Mimura 2011) as a function of temperature. Panel (c) shows the abundance of H2O, CH4, and CO2 released as a function of temperature and pressure due to mineral phase changes. The vertical red lines mark significant volatile release events. The first event at ∼700 K marks water release from silicate dehydration. The second at ∼950 K is at the breakdown of carbonates, which releases CO2. The line at 1000 MPa indicates the isobar corresponding to the phase assemblage in panel (a).
Paper: Timing and Abundance of Clathrate Formation Control Ocean Evolution in Outer Solar System Bodies: Challenges of Maintaining a Thick Ocean within Pluto
Authors: Samuel W. Courville, Julie C. Castillo-Rogez, Mohit Melwani Daswani, Elodie Gloesener, Mathieu Choukroun, Joseph G. O'Rourke
Figure caption: Clathrate layer thicknesses from accreted cometary volatiles (wt% relative to accreted water ice) at 50 MPa. Accreted volatile abundances may result in the formation of thick clathrate layers at the base and/or top of the ocean. Panel (a) displays the difference in density of the ocean from the first mixed CO2–CH4 clathrates that form, with blue indicating buoyant clathrates. Assuming a water–rock ratio of 1.5, panels (b) and (c) display the total thickness of clathrates at the top and bottom of the ocean, respectively. Panels (d), (e), and (f) are the same as panels (a), (b), and (c), except that they assume a higher water–rock ratio of 10. The pie charts show the relative incorporation of volatile carbon into clathrates, ions, and carbonate minerals for the points annotated on the plots. The pie charts represent the point in time after clathrate formation potential has been exhausted but before the ocean begins to freeze water ice.