adsabs/AstroCLIMB huggingface dataset:
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Groundwater flux into each multiple-exit-breach tadpole crater as a function of radial permeability and initial aquifer head when 0.1 crater volumes of water have been discharged from the aquifer. (a) Arabia Terra 1; (b) Arabia Terra 2; (c) Hellas; (d) Noachis. Dashed white lines indicate the water supply rate necessary to overspill all breaches simultaneously (Table 3). There is no dashed line in panel (c) because the required input flux is not reached in our model. Gray shaded areas indicate negligible groundwater flow into the crater on the timescale of one model time step.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: (a) Schematic illustration of the 1D intrusion model. Parameter h  i  is the ice thickness, z int is the intrusion depth below the crater floor, and h int is the vertical thickness of the intrusion (assumed to have same diameter as the crater). The dashed line indicates the base of ice at z = 0. (b) Time evolution of vertical temperature profile (1D profile through the central point of the crater) for a 200 m thick intrusion with an initial temperature T int = 1300 K emplaced 500 m below the crater floor for a crater overlaid by 1 km of ice. The vertical red dashed line indicates T = 273 K. The dashed line indicates the base of ice at z = 0. (c) Total thickness of water melted per unit area at the base of a crater for intrusions of different thicknesses at a range of depths beneath the crater floor (Table 4). Black lines indicate maximum intrusion depth calculated from the difference between predicted and measured crater floor depths (Table 1). White lines indicate predicted initial crater depth, i.e., where each crater would be filled to the brim with melt. The key shows line styles corresponding to different multiple-breach tadpole craters.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Meltwater pond overspill modeling results for Noachis B1 (teal) and B2 (orange) (Figure 1) for measured breach parameters in Table 2 as a function of fractional melt pond area. (a) Schematic illustration of an ice-filled crater with a shallow melt pond smaller than the area of the crater with diameter D  p  overspilling the rim via a breach. For each overspill event, the initial water depth in the melt pond must be at least the depth eroded in the overspill model (z  e ; Warren et al. 2021). (b) Downward erosion of breach base per individual overspilling event. Smaller melt pond areas generate less erosion when they overspill the rim. (c) The number of overspill events required to carve each observed breach. The number of breaches required decreases as melt pond area increases. (d) Melt days required to generate the water volumes required per overspill event in panel (c) at a melt rate of 4 m yr−1 m2 (Kite et al. 2013) across the entire crater area. Modeling results for other multiple-breach tadpole craters are given in Appendix B.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: (a) Schematic illustration of simultaneous erosion of multiple rim breaches in a water-filled crater. The crater is supplied by a continuous water source such as precipitation or groundwater. Once the water level reaches the lowest point on the rim, an outlet breach begins eroding, but the flux of water out of that breach cannot keep up with the input flux. The water level continues to rise until new, higher breaches form to accommodate the overspilling water. In this scenario, the water source must be able to supply water at a rate greater than the combined flow rate out of the crater via the first breach and over the submerged crater rim. (b) Topographic rim profile of Hellas tadpole crater (Table 1; Figure 1) with pre-incision topography for Breach 1 (B1). The dotted blue line shows the water level. The solid blue line on the topographic profile shows wetted perimeters for portions of flow out of the crater (p  w,1 and p  w,2). Red hashed regions show cross-sectional areas (a 1 and a 2) of portions of flow out of the crater.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Example water fluxes into the crater from our groundwater model show that confined aquifers with high permeability (k  h ) and high initial pressure head (h  a ) can exceed the calculated flow out of the crater required to activate all channels simultaneously (Q in; Table 3, solid blue line) for Noachis (Table 1). This corresponds to Hypothesis 1, where liquid water overspills the crater rim. Panels show time evolution of (a) groundwater flux into tadpole crater and (b) cumulative groundwater flux into crater. Dotted vertical lines indicate the times when the groundwater discharge has filled 0.1, 0.5, and 1 times the crater volume (V  c ). Dashed lines indicate the instantaneous and cumulative flux at these times.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Groundwater flow through a confined aquifer with initial head >2000 m and permeability >10−12 m2 can sustain the water supply rate necessary to overspill both breaches simultaneously for tadpole crater Arabia Terra 2 (Table 3) from when the groundwater has supplied (a) 0.1 crater volumes of water to (b) 1 crater volume of water (i.e., the crater is filled to the brim with groundwater). This corresponds to Hypothesis 1, where liquid water overspills the crater rim. However, higher initial aquifer head and permeabilities are required to sustain fluxes greater than Q in until the crater is completely filled with water. Gray shaded areas indicate negligible groundwater flow into the crater on the timescale of one model time step. Modeling results for other multiple-breach tadpole craters are given in Appendix A.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Minimum required intrusion thickness as a function of intrusion depth to trigger basal melting of an ice sheet filling a multiple-breach tadpole crater. Minimum thickness is found by interpolating our melting model results to find the intrusion thickness at which zero melting occurs, i.e., the intrusion is too deep for heating around the margins to raise the surface temperature above 273 K.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Schematic illustration of our groundwater model. A homogeneous, radially symmetrical confined aquifer 3 km thick pressurized by an overlying cryosphere is fully penetrated by a network of fractures beneath the tadpole crater, extending to the crater rim at r = 0.5D  c , where D  c  is the crater diameter. The dashed black line indicates the axis of radial symmetry. We assume that the flux of water to the crater is limited by flow through the confined aquifer to the edge of the fracture network (blue arrows). The aquifer starts with an initial head (h 0) of h  a , which is a free parameter in our groundwater model (Table 4).
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: DEM of Pingualuit crater. Modified from Figure 7 in Desiage et al. (2015). Black brackets indicate locations of breaches with elevations in meters above sea level. White and yellow ellipses highlight paleoshorelines corresponding to 575 m (the elevation of breach 3). All elevations have an error of ±1 m.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Schematic illustration of an ice sheet retreating in two stages that progressively expose lower rim topography. The first stage is where the ice sheet fills most of crater in (a) profile view and (b) birds-eye view. The second stage is where the ice sheet recedes and exposes lower points on the crater rim in (c) profile view and (d) birds-eye view.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: A plot of the 83 HST search fields. Each box marks the approximate area of a combined WFC3/UVIS field using both detectors. Five fields ended up not being useful, due to guide star failures (red) or moonlight (orange). The green boxes represent the 40-orbit HST pilot fields, and the blue boxes show the additional full program fields excluding the repeated fields to follow up on the detected objects. The five discoveries from the search are marked with a red cross and labeled with the eventual object designation. The black circles are a simulated KBO population from the CFEPS model with hot classical KBOs and CCKBOs included.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Sky signal example. The plotted histogram shows the residuals from a 2D fit to the sky in a single image. The thick orange curve is a LOWESS curve of the histogram, and the peak is used as an estimate of the mode. The vertical green lines mark the mode and the −1σ point on the low side of the distribution. The gray shaded region shows the approximate Gaussian representation of the sky signal and noise.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Sample image from field KBO1-R7R6 in each of two visits separated by 1.05 hr. This field was part of the pilot search, and 2014 MU69 is in the top chip on the right side in the area marked by the white box. The visit numbers of HST program 13633 are shown in the lower right corner of each image.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Sample images from our second reduction pipeline for the 2014 MU69 discovery image. Top: images from a single visit are shifted both by eye and then through an optimization routine to remove the stars. Bottom: the star-subtracted images are then searchable for KBOs in the field. The inlay on the bottom right is an extracted .png used for evaluation of reality.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Sample SuprimeCam image data from 2011. Two epochs are shown of the discovery images for 2011 HL103. The red arrow (or image) shows the location at the first epoch, and the cyan arrow (or image) shows the location at the second epoch. The stacked images are in the left column. Template-subtracted images are in the middle column. The right column shows the color stack of the two epochs. See text for more details.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Confirmation graphic for discovery of (486958) Arrokoth.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Sky-plane offsets from the nominal guide orbit over the course of a single HST orbit for visit icii11. Black circles are the motion of all targetable KBOs from the synthetic orbit sample. Red circles are the sky-plane motions of the chosen guide orbit grid, and blue circles are the buffers of sky motion each covers to within a single HST WFC3 pixel. The point at (0,0) is the nominal guide orbit.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Confirmation graphics for a typical false-positive detection.
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: (a) The temperature of sub-Jovian Europa as it passes through eclipse. This temperature profile is based on the thermal model of S. K. Trumbo et al. (2017a). Sub-Jovian Europa was observed for 2 hr before eclipse and 6 hr after eclipse (no observations during eclipse owing to the lack of reflected light). The bottom of the drop indicates the end of eclipse. The sub-Jovian temperature takes ∼6 hr to recover from the estimated ∼20 K drop during eclipse. Spectra were averaged for each of the ∼1 hr time intervals. Orange indicates pre-eclipse observations, and blue indicates post-eclipse observations. (b) Integrated band area calculated for each ∼1 hr window. A factor of <2 change is observed both between the measurements immediately pre-eclipse and immediately post-eclipse and between the weakest 3.5 μm absorption at 2 hr pre-eclipse and the strongest 3.5 μm absorption 5 hr post-eclipse. This small change is attributable to rotation of Europa across this time period and rules out a strong response to the eclipse temperature drop (discussed in Section 3). As errors associated with the unknown background continuum dominate over those due to noise, we estimate error bars as the values given using a range of plausible continuum fits across the wavelength range from 3.33–3.37 μm to 3.715–3.78 μm. (c) Example IRTF/Spex spectra comparing the 3.5 μm absorption 2 hr pre-eclipse with the absorption 4 hr post-eclipse. The boundaries of the selected time windows are thick in panel (b). Dashed gray lines outline the H2O2 band. Second-order polynomial continua are indicated by the dashed curves of the same color as the spectra. Continuum-removed absorptions are included to ease comparison of the band strengths. The depth of the 3 μm water-ice absorption band (shown here as the 3.2–3.7 μm range following the Fresnel peak) appears to increase after eclipse (blue), suggesting a possible rotational effect as Europa rotates from a more trailing/sub-Jovian geometry toward a more sub-Jovian/leading geometry.
Paper: Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions
Authors: Anna E. Engle, Jennifer Hanley, Sugata P. Tan, William M. Grundy, Stephen C. Tegler, Gerrick E. Lindberg, Jordan K. Steckloff, Shaelyn M. Raposa, Cecilia L. Thieberger, Shyanne Dustrud, Jessica J. Groven, Logan A. Pearce
Figure caption: Visual depiction of steps in the experimental protocol. Step 1: the alkane mixture is created in the gas phase in a 0.5-liter mixing chamber. Step 2: the mixture is released into the cell, where it condenses into a liquid. Step 3: nitrogen is injected and used to maintain the 1.5-bar vapor pressure. Step 4: the temperature in the cell is lowered. Steps 3 and 4 are repeated until ice forms or the cell overfills.
Paper: Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions
Authors: Anna E. Engle, Jennifer Hanley, Sugata P. Tan, William M. Grundy, Stephen C. Tegler, Gerrick E. Lindberg, Jordan K. Steckloff, Shaelyn M. Raposa, Cecilia L. Thieberger, Shyanne Dustrud, Jessica J. Groven, Logan A. Pearce
Figure caption: Interior side view of the cell (center) with example outputs from a 0.46 r  M  sample. The sapphire windows are positioned on opposite sides of the cell, with one side being used for collecting Raman spectra (left) and the other being used for visual inspection (right). Note: the blue tint in the photo is an attribute of the Raman probe, not a characteristic of the sample.
Paper: Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions
Authors: Anna E. Engle, Jennifer Hanley, Sugata P. Tan, William M. Grundy, Stephen C. Tegler, Gerrick E. Lindberg, Jordan K. Steckloff, Shaelyn M. Raposa, Cecilia L. Thieberger, Shyanne Dustrud, Jessica J. Groven, Logan A. Pearce
Figure caption: Fitted peaks for quantifying sample compositions using a 0.44 r  M  mixture as an example. The 2850–3000 cm−1 region is a compilation of overlapping C–H vibrational modes (listed in Table 1).
Paper: Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions
Authors: Anna E. Engle, Jennifer Hanley, Sugata P. Tan, William M. Grundy, Stephen C. Tegler, Gerrick E. Lindberg, Jordan K. Steckloff, Shaelyn M. Raposa, Cecilia L. Thieberger, Shyanne Dustrud, Jessica J. Groven, Logan A. Pearce
Figure caption: Examples of ice morphology in select CH4 alkane ratios. Panels (a)–(c) depict ice morphologies characteristic of the SELV region, panel (d) is representative of ice in the SELLNV region, and panels (e)–(f) show the ice morphology in samples that have passed the four-phase region and entered the SELNV equilibrium.
Paper: Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions
Authors: Anna E. Engle, Jennifer Hanley, Sugata P. Tan, William M. Grundy, Stephen C. Tegler, Gerrick E. Lindberg, Jordan K. Steckloff, Shaelyn M. Raposa, Cecilia L. Thieberger, Shyanne Dustrud, Jessica J. Groven, Logan A. Pearce
Figure caption: Typical composition phase diagrams: detection of the freezing temperature of a ternary mixture, with r  M  represented by the dotted line at a constant pressure P. (a) The complete topography at T 3; cooling starts at A in the LV region. (b) SLV regions at T 1 < T 2 < T 3; as the cooling proceeds to T 2, where the total composition B is still in the LV region. Upon further cooling to T 1, the total composition C is on the LV side of the corresponding SLV region, where solid is the incipient phase, which indicates that T 1 is the freezing temperature.