This document summarizes a chapter about planetary geology. It discusses:
- The interiors of terrestrial planets and how seismic waves reveal Earth's layered structure.
- Geological processes that shape planetary surfaces, like impact cratering, volcanism, tectonics, and erosion.
- How the amount of impact craters on a surface indicates its geological age.
- Evidence that water once flowed on Mars from features like dry riverbeds and rocks formed in water.
- Unique features of specific planets, like Venus' resurfaced crust and lack of plate tectonics on Venus.
- How plate tectonics shapes Earth's surface through seafloor spreading, subduction, and mountain formation
Origin of the Universe and the Solar SystemNikoPatawaran
The most widely accepted theory of planetary formation, known as the nebular hypothesis, maintains that 4.6 billion years ago, the Solar System formed from the gravitational collapse of a giant molecular cloud which was light years across.
Earth and Life Science - Theories on the Origin of the Solar SystemJuan Miguel Palero
This is a powerpoint presentation that is about one of the Senior High School Core Subject: Earth and Life Science. It is composed of the theories that explains the origin of the Solar System.
La razón principal para el estudio de atmósferas planetarias es tratar de entender el origen y evolución de la atmósfera de la tierra. Por supuesto, en el intento de comprender el funcionamiento de nuestro sistema solar o incluso la evolución de la Tierra como un organismo, la atmósfera de la tierra es esencialmente irrelevante, ya que su masa es despreciable.
Origin of the Universe and the Solar SystemNikoPatawaran
The most widely accepted theory of planetary formation, known as the nebular hypothesis, maintains that 4.6 billion years ago, the Solar System formed from the gravitational collapse of a giant molecular cloud which was light years across.
Earth and Life Science - Theories on the Origin of the Solar SystemJuan Miguel Palero
This is a powerpoint presentation that is about one of the Senior High School Core Subject: Earth and Life Science. It is composed of the theories that explains the origin of the Solar System.
La razón principal para el estudio de atmósferas planetarias es tratar de entender el origen y evolución de la atmósfera de la tierra. Por supuesto, en el intento de comprender el funcionamiento de nuestro sistema solar o incluso la evolución de la Tierra como un organismo, la atmósfera de la tierra es esencialmente irrelevante, ya que su masa es despreciable.
AS Level Physical Geography - Rocks and WeatheringArm Punyathorn
The earth's surface is an ever-changing entity. With the forces of weather and climate and tectonic variability, the rocks and minerals that make up the earth are always changing in size, shape and forms - a fascinating, ancient, never-ending process.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...Ana Luísa Pinho
Functional Magnetic Resonance Imaging (fMRI) provides means to characterize brain activations in response to behavior. However, cognitive neuroscience has been limited to group-level effects referring to the performance of specific tasks. To obtain the functional profile of elementary cognitive mechanisms, the combination of brain responses to many tasks is required. Yet, to date, both structural atlases and parcellation-based activations do not fully account for cognitive function and still present several limitations. Further, they do not adapt overall to individual characteristics. In this talk, I will give an account of deep-behavioral phenotyping strategies, namely data-driven methods in large task-fMRI datasets, to optimize functional brain-data collection and improve inference of effects-of-interest related to mental processes. Key to this approach is the employment of fast multi-functional paradigms rich on features that can be well parametrized and, consequently, facilitate the creation of psycho-physiological constructs to be modelled with imaging data. Particular emphasis will be given to music stimuli when studying high-order cognitive mechanisms, due to their ecological nature and quality to enable complex behavior compounded by discrete entities. I will also discuss how deep-behavioral phenotyping and individualized models applied to neuroimaging data can better account for the subject-specific organization of domain-general cognitive systems in the human brain. Finally, the accumulation of functional brain signatures brings the possibility to clarify relationships among tasks and create a univocal link between brain systems and mental functions through: (1) the development of ontologies proposing an organization of cognitive processes; and (2) brain-network taxonomies describing functional specialization. To this end, tools to improve commensurability in cognitive science are necessary, such as public repositories, ontology-based platforms and automated meta-analysis tools. I will thus discuss some brain-atlasing resources currently under development, and their applicability in cognitive as well as clinical neuroscience.
Comparing Evolved Extractive Text Summary Scores of Bidirectional Encoder Rep...University of Maribor
Slides from:
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Track: Artificial Intelligence
https://www.etran.rs/2024/en/home-english/
Seminar of U.V. Spectroscopy by SAMIR PANDASAMIR PANDA
Spectroscopy is a branch of science dealing the study of interaction of electromagnetic radiation with matter.
Ultraviolet-visible spectroscopy refers to absorption spectroscopy or reflect spectroscopy in the UV-VIS spectral region.
Ultraviolet-visible spectroscopy is an analytical method that can measure the amount of light received by the analyte.
What is greenhouse gasses and how many gasses are there to affect the Earth.moosaasad1975
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
Cancer cell metabolism: special Reference to Lactate PathwayAADYARAJPANDEY1
Normal Cell Metabolism:
Cellular respiration describes the series of steps that cells use to break down sugar and other chemicals to get the energy we need to function.
Energy is stored in the bonds of glucose and when glucose is broken down, much of that energy is released.
Cell utilize energy in the form of ATP.
The first step of respiration is called glycolysis. In a series of steps, glycolysis breaks glucose into two smaller molecules - a chemical called pyruvate. A small amount of ATP is formed during this process.
Most healthy cells continue the breakdown in a second process, called the Kreb's cycle. The Kreb's cycle allows cells to “burn” the pyruvates made in glycolysis to get more ATP.
The last step in the breakdown of glucose is called oxidative phosphorylation (Ox-Phos).
It takes place in specialized cell structures called mitochondria. This process produces a large amount of ATP. Importantly, cells need oxygen to complete oxidative phosphorylation.
If a cell completes only glycolysis, only 2 molecules of ATP are made per glucose. However, if the cell completes the entire respiration process (glycolysis - Kreb's - oxidative phosphorylation), about 36 molecules of ATP are created, giving it much more energy to use.
IN CANCER CELL:
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
introduction to WARBERG PHENOMENA:
WARBURG EFFECT Usually, cancer cells are highly glycolytic (glucose addiction) and take up more glucose than do normal cells from outside.
Otto Heinrich Warburg (; 8 October 1883 – 1 August 1970) In 1931 was awarded the Nobel Prize in Physiology for his "discovery of the nature and mode of action of the respiratory enzyme.
WARNBURG EFFECT : cancer cells under aerobic (well-oxygenated) conditions to metabolize glucose to lactate (aerobic glycolysis) is known as the Warburg effect. Warburg made the observation that tumor slices consume glucose and secrete lactate at a higher rate than normal tissues.
This pdf is about the Schizophrenia.
For more details visit on YouTube; @SELF-EXPLANATORY;
https://www.youtube.com/channel/UCAiarMZDNhe1A3Rnpr_WkzA/videos
Thanks...!
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
3. 9.1 Connecting Planetary Interiors and
Surfaces
• Our goals for learning:
– What are terrestrial planets like on the
inside?
– What causes geological activity?
– Why do some planetary interiors create
magnetic fields?
6. Earth's Interior
• Core: highest
density; nickel and
iron
• Mantle: moderate
density; silicon,
oxygen, etc.
• Crust: lowest
density; granite,
basalt, etc.
7. • Applying what we have learned about Earth's
interior to other planets tells us what their
interiors are probably like.
Terrestrial Planet Interiors
9. Lithosphere
• A planet's outer
layer of cool, rigid
rock is called the
lithosphere.
• It "floats" on the
warmer, softer rock
that lies beneath.
10. Strength of Rock
• Rock stretches
when pulled slowly
but breaks when
pulled rapidly.
• The gravity of a
large world pulls
slowly on its rocky
content, shaping
the world into a
sphere.
11. Special Topic:
How do we know what's inside Earth?
• P waves push
matter back
and forth.
• S waves
shake matter
side to side
12. Special Topic:
How do we know what's inside Earth?
• P waves go
through Earth's
core, but S
waves do not.
• We conclude
that Earth's
core must have
a liquid outer
layer.
13. Thought Question
What is necessary for differentiation to occur in a
planet?
a) It must have metal and rock in it.
b) It must be a mix of materials of different density.
c) Material inside must be able to flow.
d) All of the above
e) b and c
14. Thought Question
What is necessary for differentiation to occur in a
planet?
a) It must have metal and rock in it.
b) It must be a mix of materials of different density.
c) Material inside must be able to flow.
d) All of the above
e) b and c
16. Heating of Planetary Interiors
• Accretion and
differentiation
when planets were
young
• Radioactive decay
is most important
heat source today.
17. Cooling of Planetary Interiors
• Convection
transports heat as
hot material rises
and cool material
falls.
• Conduction
transfers heat
from hot material
to cool material.
• Radiation sends
energy into space.
18. • Smaller worlds cool off faster and harden earlier.
• The Moon and Mercury are now geologically
"dead."
Role of Size
19. • Heat content depends on volume.
• Loss of heat through radiation depends on
surface area.
• Time to cool depends on surface area divided by
volume:
• Larger objects have a smaller ratio and cool
more slowly.
3
Surface area–to–volume ratio =
4πr 2
4πr 3
=
3
r
Surface Area–to–Volume Ratio
20. Why do some planetary interiors create
magnetic fields?
21. Sources of Magnetic Fields
• Motions of
charged particles
are what create
magnetic fields.
22. Sources of Magnetic Fields
• A world can have a
magnetic field if
charged particles are
moving inside.
• Three requirements:
– Molten, electrically
conducting interior
– Convection
– Moderately rapid
rotation
23. What have we learned?
• What are terrestrial planets like on the inside?
– All terrestrial worlds have a core, mantle, and crust.
– Denser material is found deeper inside.
• What causes geological activity?
– Interior heat drives geological activity.
– Radioactive decay is currently main heat source.
• Why do some planetary interiors create magnetic
fields?
– Requires motion of charged particles inside a planet
24. 9.2 Shaping Planetary Surfaces
• Our goals for learning:
– What processes shape planetary
surfaces?
– How do impact craters reveal a surface's
geological age?
– Why do the terrestrial planets have
different geological histories?
26. Processes That Shape Surfaces
• Impact cratering
– Impacts by asteroids or comets
• Volcanism
– Eruption of molten rock onto surface
• Tectonics
– Disruption of a planet's surface by internal
stresses
• Erosion
– Surface changes made by wind, water, or ice
27. Impact Cratering
• Most cratering
happened soon after
the solar system
formed.
• Craters are about 10
times wider than object
that made them.
• Small craters greatly
outnumber large ones.
30. Volcanism
• Volcanism happens
when molten rock
(magma) finds a
path through
lithosphere to the
surface.
• Molten rock is called
lava after it reaches
the surface.
31. Runny lava makesRunny lava makes
flat lava plains.flat lava plains.
Slightly thickerSlightly thicker
lava makeslava makes
broadbroad shieldshield
volcanoesvolcanoes..
Thickest lava makesThickest lava makes
steepsteep
stratovolcanoesstratovolcanoes..
Lava and Volcanoes
32. • Volcanism also releases gases from Earth's
interior into the atmosphere.
Outgassing
33. • Convection of the mantle creates stresses in the
crust called tectonic forces.
• Compression of crust creates mountain ranges.
• Valley can form where crust is pulled apart.
Tectonics
34. Plate Tectonics on Earth
• Earth's continents slide around on separate
plates of crust.
35. Erosion
• Erosion is a blanket term for weather-driven
processes that break down or transport rock.
• Processes that cause erosion include:
– glaciers
– rivers
– wind
40. How do impact craters reveal a surface's
geological age?
41. History of Cratering
• Most cratering
happened in the
first billion years.
• A surface with
many craters
has not changed
much in 3 billion
years.
42. Cratering of Moon
• Some areas of
Moon are more
heavily cratered
than others.
• Younger regions
were flooded by
lava after most
cratering.
43. Cratering map of the MoonCratering map of the Moon's entire surface's entire surface
Cratering of Moon
44. Why do the terrestrial planets have different
geological histories?
45. • Smaller worlds cool off faster and harden earlier.
• Larger worlds remain warm inside, promoting
volcanism and tectonics.
• Larger worlds also have more erosion because
their gravity retains an atmosphere.
Role of Planetary Size
46. • Planets close to the Sun are too hot for rain, snow, ice
and so have less erosion.
• Hot planets have more difficulty retaining an
atmosphere.
• Planets far from the Sun are too cold for rain, limiting
erosion.
• Planets with liquid water have the most erosion.
Role of Distance from Sun
47. • Planets with slower rotation have less weather,
less erosion, and a weak magnetic field.
• Planets with faster rotation have more weather,
more erosion, and a stronger magnetic field.
Role of Rotation
48. Thought Question
How does the cooling of planets and potatoes vary
with size?
a) Larger size makes it harder for heat from inside to
escape.
b) Larger size means a bigger ratio of volume to
surface area.
c) Larger size takes longer to cool.
d) all of the above
49. Thought Question
How does the cooling of planets and potatoes vary
with size?
a) Larger size makes it harder for heat from inside to
escape.
b) Larger size means a bigger ratio of volume to
surface area.
c) Larger size takes longer to cool.
d) all of the above
50. What have we learned?
• What processes shape planetary surfaces?
– Cratering, volcanism, tectonics, erosion
• How do impact craters reveal a surface's
geological age?
– The amount of cratering tells us how long ago
a surface formed.
• Why do the terrestrial planets have different
geological histories?
– Differences arise because of planetary size,
distance from Sun, and rotation rate.
51. 9.3 Geology of the Moon and Mercury
• Our goals for learning:
– What geological processes shaped our
Moon?
– What geological processes shaped
Mercury?
53. Lunar Maria
• Smooth, dark
lunar maria are
less heavily
cratered than
lunar highlands.
• Maria were
made by floods
of runny lava.
54. LargeLarge
impactimpact
cratercrater
weakensweakens
crust.crust.
Heat build-Heat build-
up allowsup allows
lava to welllava to well
up toup to
surface.surface.
EarlyEarly
surface issurface is
coveredcovered
with craters.with craters.
Cooled lava isCooled lava is
smoother andsmoother and
darker thandarker than
surroundings.surroundings.
Formation of Lunar Maria
58. Cratering of Mercury
• Mercury has a
mixture of heavily
cratered and
smooth regions like
the Moon.
• Smooth regions are
likely ancient lava
flows.
59. The Rembrandt Basin isThe Rembrandt Basin is
a large impact crater ona large impact crater on
Mercury.Mercury.
Hollows in a crater floorHollows in a crater floor
created by escaping gases.created by escaping gases.
Cratering of Mercury
60. • Long cliffs indicate that Mercury shrank early in
its history.
Tectonics on Mercury
61. What have we learned?
• What geological processes shaped our
Moon?
– Early cratering is still present.
– Maria resulted from volcanism.
• What geological processes shaped Mercury?
– Had cratering and volcanism similar to Moon
– Tectonic features indicate early shrinkage.
62. 9.4 Geology of Mars
• Our goals for learning:
– What geological processes have shaped
Mars?
– What geological evidence tells us that
water once flowed on Mars?
63. • Percival Lowell misinterpreted surface features
seen in telescopic images of Mars.
"Canals" on Mars
69. • Close-up photos of Mars show what appear to
be dried-up riverbeds.
Dry Riverbeds?
70. Insert TCP7e
Figure 9.29
Insert TCP7e
Figure 9.29
Erosion of Craters
• Details of some craters suggest they were once
filled with water.
71. Martian Rocks
• Mars rovers have found rocks that appear to
have formed in water.
72. Martian Rocks
• Mars rovers have found rocks that appear to
have formed in water.
73. Image Credit: NASA/JPL
Hydrogen Content
• Map of hydrogen content (blue) shows that low-
lying areas contain more water ice.
74. Crater Walls
• Gullies on crater
walls suggest
occasional liquid
water flows have
happened less
than a million
years ago.
75. What have we learned?
• What are the major geological features of
Mars?
– Differences in cratering across surface
– Giant shield volcanoes
– Evidence of tectonic activity
76. What have we learned?
• What geological evidence tells us that water
once flowed on Mars?
– Some surface features look like dry riverbeds.
– Some craters appear to be eroded.
– Rovers have found rocks that appear to have
formed in water.
– Gullies in crater walls may indicate recent
water flows.
77. 9.5 Geology of Venus
• Our goals for learning:
– What geological processes have shaped
Venus?
– Does Venus have plate tectonics?
79. Insert TCP7e
figure 9.35
Insert TCP7e
figure 9.35
Radar Mapping
• Its thick atmosphere forces us to explore
Venus's surface through radar mapping.
80. Cratering on Venus
• Venus has impact
craters, but fewer
than the Moon,
Mercury, or Mars.
81. Volcanoes on Venus
• It has many
volcanoes, including
both shield
volcanoes and
stratovolcanoes.
82. Tectonics on Venus
• The planet's
fractured and
contorted surface
indicates tectonic
stresses.
83. Erosion on Venus
• Photos of rocks
taken by
landers show
little erosion.
84. Does Venus have plate tectonics?
• Venus does not appear to have plate tectonics,
but entire surface seems to have been "repaved"
750 million years ago.
• Weaker convection?
• Thicker or more rigid lithosphere?
85. What have we learned?
• What geological processes have shaped
Venus?
– Venus has cratering, volcanism, and tectonics
but not much erosion.
• Does Venus have plate tectonics?
– The lack of plate tectonics on Venus is a
mystery.
86. 9.6 The Unique Geology of Earth
• Our goals for learning:
– How is Earth's surface shaped by plate
tectonics?
– Was Earth's geology destined from birth?
89. Continental Motion
• The idea of
continental drift
was inspired by
the puzzle-like fit
of the continents.
• Mantle material
erupts where the
seafloor spreads.
90. Seafloor Crust
• Thin seafloor
crust differs
from thick
continental
crust.
• Dating of the
seafloor
shows that it
is usually
quite young.
99. Earth's Destiny
• Many of Earth's
features are
determined by its
size, rotation,
and distance
from Sun.
• The reason for
plate tectonics is
not yet clear.
100. What have we learned?
• How is Earth's surface shaped by plate
tectonics?
– Measurements of plate motions confirm the
idea of continental drift.
– Plate tectonics is responsible for subduction,
seafloor spreading, mountains, rifts, and
earthquakes.
101. What have we learned?
• Was Earth's geology destined from birth?
– Many of Earth's features are determined by its
size, distance from Sun, and rotation rate.
– The reason for plate tectonics is still a
mystery.