Presentation is loading. Please wait.

Presentation is loading. Please wait.

Figure 3 from Ab Initio Free Energy Calculations of the Solubility of Silica in Metallic Hydrogen and Application to Giant Planet Cores F. González-Cataldo.

Published byConrad Shepherd Modified over 6 years ago

Similar presentations

Presentation on theme: "Figure 3 from Ab Initio Free Energy Calculations of the Solubility of Silica in Metallic Hydrogen and Application to Giant Planet Cores F. González-Cataldo."— Presentation transcript:

1 Figure 3 from Ab Initio Free Energy Calculations of the Solubility of Silica in Metallic Hydrogen and Application to Giant Planet Cores F. González-Cataldo et al ApJ doi: / X/787/1/79 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

Download ppt "Figure 3 from Ab Initio Free Energy Calculations of the Solubility of Silica in Metallic Hydrogen and Application to Giant Planet Cores F. González-Cataldo."

Similar presentations

Figure 4 from The Hubble Space Telescope Cluster Supernova Survey. II. The Type Ia Supernova Rate in High-redshift Galaxy Clusters (Image 1 of 3) K. Barbary.

Figure 4 from The Hubble Space Telescope Cluster Supernova Survey. II. The Type Ia Supernova Rate in High-redshift Galaxy Clusters (Image 1 of 3) K. Barbary.
Figure 7 from Effects of Circumnuclear Disk Gas Evolution on the Spin of Central Black Holes (Image 1 of 7) Umberto Maio et al. 2013 ApJ 767 37 doi:10.1088/0004-637X/767/1/37.

Figure 7 from Effects of Circumnuclear Disk Gas Evolution on the Spin of Central Black Holes (Image 1 of 7) Umberto Maio et al ApJ doi: / X/767/1/37.
Figure 6 from HST/WFC3 Near-infrared Spectroscopy of Quenched Galaxies at z ~ 1.5 from the WISP Survey: Stellar Population Properties (Image 1 of 8) A.

Figure 6 from HST/WFC3 Near-infrared Spectroscopy of Quenched Galaxies at z ~ 1.5 from the WISP Survey: Stellar Population Properties (Image 1 of 8) A.
Figure 14 from MUSCLE W49: A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and the Mass.

Figure 14 from MUSCLE W49: A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and the Mass.
Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34.

Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al ApJ doi: / X/787/1/34.
Figure 14 from The Compositional Diversity of Extrasolar Terrestrial Planets. I. In Situ Simulations (Image 1 of 4) Jade C. Bond et al. 2010 ApJ 715 1050.

Figure 14 from The Compositional Diversity of Extrasolar Terrestrial Planets. I. In Situ Simulations (Image 1 of 4) Jade C. Bond et al ApJ
Figure 4 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 9) N. M. McClure-Griffiths et al. 2012 ApJS 199 12 doi:10.1088/0067-0049/199/1/12.

Figure 4 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 9) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.
Figure 15 from Spectral Energy Distributions of QSOs at z > 5: Common Active Galactic Nucleus-heated Dust and Occasionally Strong Star-formation (Image.

Figure 15 from Spectral Energy Distributions of QSOs at z > 5: Common Active Galactic Nucleus-heated Dust and Occasionally Strong Star-formation (Image.
Figure 15 from Star Formation in the Central 400 pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects (Image 1 of 2) F. Yusef-Zadeh.

Figure 15 from Star Formation in the Central 400 pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects (Image 1 of 2) F. Yusef-Zadeh.
Figure 5 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 5) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.

Figure 5 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 5) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.
Figure 3 from Multiple Component Outflows in an Active Region Observed with the EUV Imaging Spectrometer on Hinode (Image 1 of 11) P. Bryans et al. 2010.

Figure 3 from Multiple Component Outflows in an Active Region Observed with the EUV Imaging Spectrometer on Hinode (Image 1 of 11) P. Bryans et al
K. Decker French et al ApJ doi: / X/801/1/1 Information:

K. Decker French et al ApJ doi: / X/801/1/1 Information:
Figure 15 from Cloud–Cloud Collision as a Trigger of the High-mass Star Formation: a Molecular Line Study in RCW120 (Image 1 of 5) K. Torii et al. 2015.

Figure 15 from Cloud–Cloud Collision as a Trigger of the High-mass Star Formation: a Molecular Line Study in RCW120 (Image 1 of 5) K. Torii et al
Figure 7 from The Evolution of Dwarf Galaxy Satellites with Different Dark Matter Density Profiles in the ErisMod Simulations. I. The Early Infalls Mihai.

Figure 7 from The Evolution of Dwarf Galaxy Satellites with Different Dark Matter Density Profiles in the ErisMod Simulations. I. The Early Infalls Mihai.
Figure 9 from A Direct Measurement of the Forward Shock Speed in Supernova Remnant 0509-67.5: Constraints on the Age, Ambient Density, Shock Compression.

Figure 9 from A Direct Measurement of the Forward Shock Speed in Supernova Remnant : Constraints on the Age, Ambient Density, Shock Compression.
Figure 2 from The Role of Active Region Loop Geometry. II

Figure 2 from The Role of Active Region Loop Geometry. II
Figure 5 from The ACS LCID Project. II

Figure 5 from The ACS LCID Project. II
Qing-Wen Tang et al ApJ doi: / X/806/2/194 Information:

Qing-Wen Tang et al ApJ doi: / X/806/2/194 Information:
Figure 8 from Dust Reddened Quasars in FIRST and UKIDSS: Beyond the Tip of the Iceberg (Image 1 of 5) Eilat Glikman et al. 2013 ApJ 778 127 doi:10.1088/0004-637X/778/2/127.

Figure 8 from Dust Reddened Quasars in FIRST and UKIDSS: Beyond the Tip of the Iceberg (Image 1 of 5) Eilat Glikman et al ApJ doi: / X/778/2/127.
Figure 4 from Electron Heating by the Ion Cyclotron Instability in Collisionless Accretion Flows. II. Electron Heating Efficiency as a Function of Flow.

Figure 4 from Electron Heating by the Ion Cyclotron Instability in Collisionless Accretion Flows. II. Electron Heating Efficiency as a Function of Flow.

Similar presentations

Ads by Google