Decks 7, 9 and 14: every notes figure now has a hero frame

Lecture 7 gains the Grand Canyon, the Huygens surface view of Titan, the Magellan map of Venus, Bennu and Pluto; Lecture 9 the oxygen history, the Archean climate models, the Venus magma-ocean evolution, the Earth accretion tracers and the Shark Bay stromatolites; Lecture 14 the pebble-accretion growth curves, the NC-CC timeline and the radius valley. Each hero carries a caption with the claim the notes make of it.

Author: timlichtenberg

book/_static/slides/lecture07.pdf

@@ -481,13 +481,25 @@ \section{Erosion and weathering}
   \end{columns}
 \end{frame}
 
+\begin{frame}
+  \centering
+  \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.64\paperheight, keepaspectratio]{grand_canyon_colorado}}\\
+  {\footnotesize The Colorado River in the Grand Canyon: the river has cut about 1.6 km through nearly flat-lying Paleozoic sedimentary rock in the past 5 to 6 Myr, the type example of sustained fluvial erosion on Earth. The stepped walls record differential erosion: resistant limestone and sandstone stand as cliffs, weaker shale erodes to slopes. Credit: Alex Demas/USGS, public domain.}
+\end{frame}
+
 % ── Two kinds of Martian water feature ────────────────────
 \begin{frame}
   \centering
   \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.72\paperheight, keepaspectratio]{mars_outflow_aram}}\\
   {\footnotesize An outflow channel through Aram Chaos: braided islands and scoured troughs record catastrophic floods, in contrast to the dendritic valley networks that record precipitation. Credit: NASA/JPL-Caltech/MSSS.}
 \end{frame}
 
+\begin{frame}
+  \centering
+  \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.62\paperheight, keepaspectratio]{titan_huygens_surface}}\\
+  {\footnotesize The surface of Titan from ESA's Huygens probe on 14 January 2005, the only image taken from the surface of an outer-solar-system body, in three enlarged crops. The rounded decimetre-scale blocks are water ice, rounded by methane fluvial transport, on a damp dark plain of organic sediment in a dried-out riverbed: liquid methane shapes Titan's surface today. Credit: ESA/NASA/JPL-Caltech/University of Arizona, public domain.}
+\end{frame}
+
 % ── Glacial and chemical weathering ───────────────────────
 \begin{frame}{Glacial and chemical weathering}
   \begin{columns}[c]
@@ -522,6 +534,12 @@ \section{Remote sensing of surfaces}
   \end{description}
 \end{frame}
 
+\begin{frame}
+  \centering
+  \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.64\paperheight, keepaspectratio]{venus_magellan}}\\
+  {\footnotesize Venus from the Magellan radar mission (1990 to 1994), coloured from Venera lander measurements. Synthetic aperture radar mapped 98\% of the surface at about 100 m resolution through the permanent cloud deck: more than 1600 volcanic centres, lava plains over about 80\% of the surface, and a uniform crater population that implies a global mean surface age of only 300 to 700 Myr. Credit: NASA/JPL, public domain.}
+\end{frame}
+
 \begin{frame}
   \centering
   \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.72\paperheight, keepaspectratio]{crism_mineral_map}}\\
@@ -554,6 +572,12 @@ \section{Regolith and space weathering}
   \end{columns}
 \end{frame}
 
+\begin{frame}
+  \centering
+  \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.64\paperheight, keepaspectratio]{bennu_osiris_rex}}\\
+  {\footnotesize Bennu from OSIRIS-REx in December 2018, from 24 km: boulders at every scale on the about 490 m body, no smooth ponded plains, and a very low bulk density that implies high porosity, a rubble pile of collisional fragments reaccumulated under self-gravity. OSIRIS-REx returned 121.6 g of this material to Earth in September 2023. Credit: NASA/Goddard/University of Arizona, public domain.}
+\end{frame}
+
 \begin{frame}
   \centering
   \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.72\paperheight, keepaspectratio]{space_weathering}}\\
@@ -597,6 +621,12 @@ \section{Cryovolcanism on icy bodies}
   {\footnotesize Voyager 2 mosaic of Neptune's moon Triton: active nitrogen geyser streaks cross the pink $\mathrm{N_2}$/$\mathrm{CH_4}$ polar frost (bottom), while cantaloupe terrain of dimples and ridges dominates the north. Credit: NASA/JPL/Voyager 2.}
 \end{frame}
 
+\begin{frame}
+  \centering
+  \makebox[\linewidth][c]{\includegraphics[width=0.95\paperwidth, height=0.64\paperheight, keepaspectratio]{pluto_true_color}}\\
+  {\footnotesize Pluto in enhanced true colour from New Horizons, 14 July 2015: the bright western lobe of the heart-shaped Tombaugh Regio is Sputnik Planitia, a crater-free plain of convecting nitrogen ice bordered by water-ice mountains, and the dark reddish equatorial terrains are coated in tholins, organics made by radiation chemistry. A small, distant dwarf planet can be geologically active today. Credit: NASA/JHUAPL/SwRI, public domain.}
+\end{frame}
+
 % ════════════════════════════════════════════════════════════
 \sectionimage{io_nusku_change}{A new eruption on Io, JunoCam 2024. Credit: NASA/JPL-Caltech/SwRI/MSSS/Jason Perry}
 \section{Recent advances}