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1) The most recent supercontinent periods were 237 million years ago and 1,100 million years ago, and the continents did not recently break up from a supercontinent like Pangea or Rodinia. 2) Westerly winds caused by atmospheric pressure shifts would cause gyres to form around warm equatorial waters, causing the warm water to crash into continents and transfer heat to cooler surrounding oceans. 3) Surface currents allow heat transfer from the equator to poles via the Coriolis effect deflecting winds.
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Academic
Search Premier
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Section:
BEYOND LIMITS: WHERE WE'RE HEADED
ECOLOGY
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penetrate to the ocean, which may be the foundation of Charon’s canyons.
Plain language summary: When ocean-bearing moons begin to cool down, their oceans can freeze. As new ice
accretes to the bottom of the existing ice shell, the added volume of the ice can stress the shell. Pluto’s largest
moon, Charon, has canyons and cryovolcanic flows that may have formed in response to a freezing ocean. Here,
we model the formation of fractures within Charon’s ice shell as the ocean underneath it freezes to explore the
evolution of Charon’s interior and surface. We find that an ocean source for cryovolcanic flows is unlikely
because the ice shell would have had to be much thinner than current thermal evolution models imply. However,
freezing the ocean may have produced the stresses that formed canyons later in Charon’s history.
9. the great time questions, part 3
Rates of erosion, sedimentation in oceans, and preservation of flat surfaces provide data favoring a recent creation rather than long geological ages. Erosion is too fast to allow old continents to still exist, and should have filled the oceans with sediment many times over. Flat surfaces assumed to be very old also should have eroded away, yet remain level. Gaps between sedimentary layers known as paraconformities show little erosion across boundaries of assumed long time spans, challenging the geological timescale. These various factors suggest the Earth is much younger than assumed by conventional geology.
Origin and interiors of the earth LECTURE OF CIVIL ENGINEERING DRAWING
This document provides an overview of engineering geology and the interior structure of Earth. It discusses:
- Engineering geology as the application of geology to civil engineering projects.
- The interior structure of Earth, including the crust, mantle (with upper, lower, and outer layers), liquid outer core, and solid inner core.
- Theories for the origin of Earth, including the nebular hypothesis of Kant and Laplace where Earth formed from a contracting gas cloud/nebula around the sun.
Inventory of CO2 available for terraforming Mars
We revisit the idea of ‘terraforming’ Mars — changing its environment to be more Earth-like in a way that would allow terrestrial
life (possibly including humans) to survive without the need for life-support systems — in the context of what we know
about Mars today. We want to answer the question of whether it is possible to mobilize gases present on Mars today in nonatmospheric
reservoirs by emplacing them into the atmosphere, and increase the pressure and temperature so that plants or
humans could survive at the surface. We ask whether this can be achieved considering realistic estimates of available volatiles,
without the use of new technology that is well beyond today’s capability. Recent observations have been made of the loss
of Mars’s atmosphere to space by the Mars Atmosphere and Volatile Evolution Mission probe and the Mars Express spacecraft,
along with analyses of the abundance of carbon-bearing minerals and the occurrence of CO2 in polar ice from the Mars
Reconnaissance Orbiter and the Mars Odyssey spacecraft. These results suggest that there is not enough CO2 remaining on
Mars to provide significant greenhouse warming were the gas to be emplaced into the atmosphere; in addition, most of the CO2
gas in these reservoirs is not accessible and thus cannot be readily mobilized. As a result, we conclude that terraforming Mars
is not possible using present-day technology.
Venusian Habitable Climate Scenarios: Modeling Venus Through Time and Applica...
One popular view of Venus' climate history describes a world that has spent much of its life
with surface liquid water, plate tectonics, and a stable temperate climate. Part of the basis for this
optimistic scenario is the high deuterium to hydrogen ratio from the Pioneer Venus mission that was
interpreted to imply Venus had a shallow ocean's worth of water throughout much of its history. Another
view is that Venus had a long-lived (∼100 million years) primordial magma ocean with a CO2 and steam
atmosphere. Venus' long-lived steam atmosphere would sufficient time to dissociate most of the water
vapor, allow significant hydrogen escape, and oxidize the magma ocean. A third scenario is that Venus had
surface water and habitable conditions early in its history for a short period of time (<1 Gyr), but that a
moist/runaway greenhouse took effect because of a gradually warming Sun, leaving the planet desiccated
ever since. Using a general circulation model, we demonstrate the viability of the first scenario using the
few observational constraints available.We further speculate that large igneous provinces and the global
resurfacing hundreds of millions of years ago played key roles in ending the clement period in its history
and presenting the Venus we see today. The results have implications for what astronomers term “the
habitable zone,” and if Venus-like exoplanets exist with clement conditions akin to modern Earth, we
propose to place them in what we term the “optimistic Venus zone.”
Density of seawater , correlations related to the calculation
Density of seawater , correlations related to the calculation
C cycle .pdf
The carbon cycle involves the movement of carbon between different reservoirs on Earth, including the atmosphere, oceans, biosphere, lithosphere, and hydrosphere. Carbon moves between these reservoirs through both fast and slow carbon cycles. The fast carbon cycle involves the exchange of carbon between the atmosphere and biosphere through photosynthesis and respiration, while the slow carbon cycle moves carbon between the atmosphere, oceans, and lithosphere over geological timescales through chemical weathering, sediment formation, and volcanism. Key aspects of the carbon cycle include the solubility pump, biological pump, and carbonate pump, which transfer carbon from surface waters to the deep ocean and sediments, lowering atmospheric CO2 levels.
The divergent fates of primitive hydrospheric water on Earth and Mars
The document summarizes research comparing how Earth and Mars differently sequestered early surface water into their mantles. It finds that hydrated Martian basalts can structurally bind about 25% more water than terrestrial basalts, and retain it to greater depths within Mars. Calculations suggest over 9% of the Martian mantle may contain hydrous minerals from surface reactions, versus only about 4% for Earth's mantle. Additionally, hydrated Martian crust experiences little density change upon hydration or dehydration, allowing efficient overplating and burial in Mars' early stagnant-lid tectonic regime. This provided an important sink for Martian surface water and a mechanism for oxidizing its mantle. In contrast, Earth
Carbon sequestration
Carbon sequestration involves capturing carbon dioxide emissions from large point sources like power plants and storing it long-term to mitigate climate change. There are three main carbon sequestration methods: terrestrial through plants and soils, geological by injecting CO2 underground, and ocean storage by injecting it deep into the ocean. While carbon sequestration could help reduce emissions, concerns include potential leakage of stored CO2 and impacts on ocean life from ocean storage. More research is still needed but carbon sequestration may prove effective if sites are carefully selected and monitored.
Cauchi Melissa Capstone Draft 4
This document discusses how rising temperatures and ocean acidification due to climate change threaten coral reefs by comparing current projections to conditions during the Paleocene-Eocene Thermal Maximum (PETM). The PETM saw temperatures and CO2 levels exceed today while coral reefs survived but were forced to migrate from mid-latitudes. Similarly, under the "business as usual" RCP 8.5 emissions scenario, coral reefs face high risk of extinction by 2050 due to the current rapid rate of warming, leaving only coral skeletons in algal slime. The Great Barrier Reef will be among the first affected as oceans absorb excess CO2, becoming more acidic and unsuitable for coral growth and survival.
Global tectonics
The document discusses the composition and structure of the Earth's interior based on seismic data and studies of meteorites and mantle rocks. It can be summarized as follows:
1) The Earth is composed of an iron-nickel core surrounded by a silicate mantle and crust. The density increases towards the center.
2) The continental crust averages 30 km thick and has a composition ranging from granodiorite to diorite. The oceanic crust is 6-7 km thick and composed of three layers: an upper volcanic layer, a middle intrusive gabbro layer, and a lower ultramafic layer.
3) The mantle extends from the Moho to the core-mantle boundary. Se
Water planets in_the_habitable_zone_atmospheric_chemistry_observable_features...
This document discusses atmospheric models for water planets in the habitable zone. It begins by introducing water planets and noting that Kepler-62e and -62f are the first candidates for habitable zone water planets. It then outlines assumptions for atmospheric composition and cycling of gases like CO2 and CH4 through clathration in high-pressure water ice. Models suggest water planet atmospheres would be similar to terrestrial planets, with CO2 or H2O dominance depending on stellar flux. The habitable zone is only slightly different for water planets due to atmospheric albedo dominance. Kepler-62e and -62f are discussed as case studies for temperate water planets receiving fluxes of 1.2 and 0.41 times Earth's
Planetary Vacuums, Atmospheres, & Life
While does our earth have a 21% Oxygen Atmosphere,
when our neighboring planets, Mars, and Venus, have mostly Carbon Dioxide?
Could our earth have a runaway greenhouse effect like Venus?
Is there life on the billions of exo-planets?
greenhouse effect...............................................................
The document discusses the greenhouse effect on Earth and how it contributes to suitable conditions for liquid water. It notes that Earth's atmosphere is slightly warmer than expected due to greenhouse gases like water vapor and carbon dioxide trapping infrared radiation emitted from the surface. A mild greenhouse effect prevents temperatures from being too hot or cold for water to remain liquid. It also discusses how water vapor is the most abundant greenhouse gas and is important for regulating Earth's temperature through a feedback loop with carbon dioxide.
Changes in the earth and its atmosphere
The document summarizes changes to the Earth's core, mantle, crust, and atmosphere over time. It describes the theory of tectonic plates and how their movement causes earthquakes and volcanic eruptions. It explains how early theories of continental drift were rejected but later accepted when ocean floor investigations found evidence supporting plate tectonics. It also outlines how the atmosphere was initially composed of gases like carbon dioxide and methane, and how oxygen levels increased due to photosynthesis by plants and algae.
Chapter 13 – oceans and beaches
The document summarizes how oceans shape our lives by discussing the distribution of water on Earth, properties of ocean water, ocean motions, shoreline formations, and the barrier islands of North Carolina's Outer Banks. It explains that barrier islands formed due to rising sea levels, a large sand supply, a gently sloping coast, and wave energy. Humans are increasing the rate of barrier island migration through armoring and development, which reduces available sand and increases erosion risks. Ultimately, one cannot have buildings and beaches in the long run due to the dynamic coastal environment.
Planetary Atmospheres & Life
Why is the temperature of Venus hotter than Mercury that is closer to the sun.
Search for life in our (1) solar system and (2) Milky Way Galaxy
How life has and is now impacting our earth
Similar to Studysheet (20)
Caldeira, Ken. The Great Climate Experiment. Scientific Am.docx
Caldeira, Ken. The Great Climate Experiment. Scientific Am.docx
The challenges of driving Charon’s cryovolcanism from a freezing ocean
The challenges of driving Charon’s cryovolcanism from a freezing ocean
Origin and interiors of the earth LECTURE OF CIVIL ENGINEERING DRAWING
Origin and interiors of the earth LECTURE OF CIVIL ENGINEERING DRAWING
Venusian Habitable Climate Scenarios: Modeling Venus Through Time and Applica...
Venusian Habitable Climate Scenarios: Modeling Venus Through Time and Applica...
Density of seawater , correlations related to the calculation
Density of seawater , correlations related to the calculation
The divergent fates of primitive hydrospheric water on Earth and Mars
The divergent fates of primitive hydrospheric water on Earth and Mars
Water planets in_the_habitable_zone_atmospheric_chemistry_observable_features...
Water planets in_the_habitable_zone_atmospheric_chemistry_observable_features...
greenhouse effect...............................................................
greenhouse effect...............................................................
Studysheet
- 1. 1) The continents did not recently break up from a supercontinent such as Pangea or Rodinia. The most recent supercontinent period was 237 million years ago and before that, 1,100 million years ago. 2) Sheet 3) Westerlies caused by shifts in atmospheric pressure would cause Gyers to form around the warm equatorial waters. These winds would cause the warm water to crash into the surrounding continents spewing warm water into the surrounding cooler oceans and therefore creating a thermohaline circulation. 4) The surface currents will enable heat to be transferred from the equator towards the poles thanks to the earth’s coreolis effect which deflects the winds. 5) Yes I do expect bottom water formation. 6) 7) I expect there to be mediocre carbon burial rate because from the diagram I am able to see that the amounts of shallow oceans and deep oceans are in a current state of equilibrium. 8) I expect the average Co2 Concentrations to be slowly increasing because although the shallow to deep ocean ratios are almost equal, it still takes a very long time for the carbon to be absorbed by the ocean and transferred into rocks through sedimentary deposits. 9) I think that before, the atmostpheric Co2 concentrations were much higher because of the limited amounts of shallow oceans. The oceans were much deeper because of the closeness of the continents. 10) Because the continents are in a period of closing, the shallow oceans will become more limited which will make the Co2 absorption process via the oceans more tedious. 11) I feel that the earth is full of shallow oceans because of the distance between landmasses and that the absorption of Co2 by the oceans are very high in comparison to when the earth’s continents are more confined. Soon enough humans will cease the high Co2 emitting processes that are currently used today and Co2 will return to their normal cyclical points.