Paleogene Atlas
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PORT: Contém 15 mapas mundiais retratando o período Paleogeno (dentro da Era Cenozóica) / ENG: Contains 15 maps that show the configuration of lands and seas during the Paleogene period (Cenozoic Era).
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Recomendados
AAS National Conference 2008: Robert Lin
Session 4: Mars – The Best is Yet to Come
19 November 2008, Pasadena California
http://www.astronautical.org/conference/conference-2008
IRJET- Space Technology on Erosion Histories of Earth and Mars
This document discusses using space technology to analyze erosion histories on Earth and Mars by reconstructing ancient river channels. It proposes mapping channels identified in seismic data from the North Atlantic and Mars to model uplift rates over time. This could provide insights into mantle dynamics beneath the North Atlantic and test theories of early plate tectonics and water cycling on Mars. The methodology involves reconstructing drainage networks from terrain data, modeling river profiles, and inverting models to determine uplift histories that fit observed profiles. Analyzing erosion patterns in this way could improve understanding of geological processes on multiple planets.
Progressin physicalgeography 2015-pnek-168-98
This document summarizes recent progress in techniques for dating landslides globally. It analyzes over 950 dated landslides, with 734 dated since 2000. Traditional methods rely mainly on radiocarbon dating, but cosmic ray exposure techniques are increasingly used to date both accumulation (e.g. landslide boulders) and depletion (e.g. landslide scarps) parts of landslides. Regional landslide chronologies have improved, though are still less extensive than for fluvial, glacial or eolian landforms. The most data exists for mountain areas in North America, South America, Europe, the Himalayas and New Zealand. Dated landslides in plate interiors are lacking, especially in South
Multi-phase volcanic resurfacing at Loki Patera on Io
The Jovian moon Io hosts the most powerful persistently active
volcano in the Solar System, Loki Patera1,2. The interior of this
volcanic, caldera-like feature is composed of a warm, dark floor
covering 21,500 square kilometres3 surrounding a much cooler
central ‘island’4. The temperature gradient seen across areas of
the patera indicates a systematic resurfacing process4–9, which
has been seen to occur typically every one to three years since the
1980s5,10. Analysis of past data has indicated that the resurfacing
progressed around the patera in an anti-clockwise direction at a
rate of one to two kilometres per day, and that it is caused either
by episodic eruptions that emplace voluminous lava flows or by a
cyclically overturning lava lake contained within the patera5,8,9,11.
However, spacecraft and telescope observations have been unable to
map the emission from the entire patera floor at sufficient spatial
resolution to establish the physical processes at play. Here we report
temperature and lava cooling age maps of the entire patera floor at
a spatial sampling of about two kilometres, derived from groundbased
interferometric imaging of thermal emission from Loki Patera
obtained on 8 March 2015 ut as the limb of Europa occulted Io.
Our results indicate that Loki Patera is resurfaced by a multi-phase
process in which two waves propagate and converge around the
central island. The different velocities and start times of the waves
indicate a non-uniformity in the lava gas content and/or crust bulk
density across the patera.
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
The importance of continents, oceans and plate tectonics for the evolution of...
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
PROBING FOR EVIDENCE OF PLUMES ON EUROPA WITH HST/STIS
Roth et al. (2014a) reported evidence for plumes of water venting from a southern high latitude
region on Europa – spectroscopic detection of off-limb line emission from the dissociation
products of water. Here, we present Hubble Space Telescope (HST) direct images of Europa in
the far ultraviolet (FUV) as it transited the smooth face of Jupiter, in order to measure absorption
from gas or aerosols beyond the Europa limb. Out of ten observations we found three in which
plume activity could be implicated. Two show statistically significant features at latitudes similar
to Roth et al., and the third, at a more equatorial location. We consider potential systematic
effects that might influence the statistical analysis and create artifacts, and are unable to find any
that can definitively explain the features, although there are reasons to be cautious. If the
apparent absorption features are real, the magnitude of implied outgassing is similar to that of the
Roth et al. feature, however the apparent activity appears more frequently in our data.
Tsunami wave extensively_resurfaced_the_shorelines_of_an_early_martian_ocean
It has been proposed that ~3.4 billion years ago an ocean fed by enormous catastrophic floods covered
most of the Martian northern lowlands. However, a persistent problem with this hypothesis is the
lack of definitive paleoshoreline features. Here, based on geomorphic and thermal image mapping in
the circum-Chryse and northwestern Arabia Terra regions of the northern plains, in combination with
numerical analyses, we show evidence for two enormous tsunami events possibly triggered by bolide
impacts, resulting in craters ~30km in diameter and occurring perhaps a few million years apart. The
tsunamis produced widespread littoral landforms, including run-up water-ice-rich and bouldery lobes,
which extended tens to hundreds of kilometers over gently sloping plains and boundary cratered
highlands, as well as backwash channels where wave retreat occurred on highland-boundary surfaces.
The ice-rich lobes formed in association with the younger tsunami, showing that their emplacement
took place following a transition into a colder global climatic regime that occurred after the older
tsunami event. We conclude that, on early Mars, tsunamis played a major role in generating and
resurfacing coastal terrains.
Recomendados
AAS National Conference 2008: Robert Lin
Session 4: Mars – The Best is Yet to Come
19 November 2008, Pasadena California
http://www.astronautical.org/conference/conference-2008
IRJET- Space Technology on Erosion Histories of Earth and Mars
This document discusses using space technology to analyze erosion histories on Earth and Mars by reconstructing ancient river channels. It proposes mapping channels identified in seismic data from the North Atlantic and Mars to model uplift rates over time. This could provide insights into mantle dynamics beneath the North Atlantic and test theories of early plate tectonics and water cycling on Mars. The methodology involves reconstructing drainage networks from terrain data, modeling river profiles, and inverting models to determine uplift histories that fit observed profiles. Analyzing erosion patterns in this way could improve understanding of geological processes on multiple planets.
Progressin physicalgeography 2015-pnek-168-98
This document summarizes recent progress in techniques for dating landslides globally. It analyzes over 950 dated landslides, with 734 dated since 2000. Traditional methods rely mainly on radiocarbon dating, but cosmic ray exposure techniques are increasingly used to date both accumulation (e.g. landslide boulders) and depletion (e.g. landslide scarps) parts of landslides. Regional landslide chronologies have improved, though are still less extensive than for fluvial, glacial or eolian landforms. The most data exists for mountain areas in North America, South America, Europe, the Himalayas and New Zealand. Dated landslides in plate interiors are lacking, especially in South
Multi-phase volcanic resurfacing at Loki Patera on Io
The Jovian moon Io hosts the most powerful persistently active
volcano in the Solar System, Loki Patera1,2. The interior of this
volcanic, caldera-like feature is composed of a warm, dark floor
covering 21,500 square kilometres3 surrounding a much cooler
central ‘island’4. The temperature gradient seen across areas of
the patera indicates a systematic resurfacing process4–9, which
has been seen to occur typically every one to three years since the
1980s5,10. Analysis of past data has indicated that the resurfacing
progressed around the patera in an anti-clockwise direction at a
rate of one to two kilometres per day, and that it is caused either
by episodic eruptions that emplace voluminous lava flows or by a
cyclically overturning lava lake contained within the patera5,8,9,11.
However, spacecraft and telescope observations have been unable to
map the emission from the entire patera floor at sufficient spatial
resolution to establish the physical processes at play. Here we report
temperature and lava cooling age maps of the entire patera floor at
a spatial sampling of about two kilometres, derived from groundbased
interferometric imaging of thermal emission from Loki Patera
obtained on 8 March 2015 ut as the limb of Europa occulted Io.
Our results indicate that Loki Patera is resurfaced by a multi-phase
process in which two waves propagate and converge around the
central island. The different velocities and start times of the waves
indicate a non-uniformity in the lava gas content and/or crust bulk
density across the patera.
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
The importance of continents, oceans and plate tectonics for the evolution of...
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
PROBING FOR EVIDENCE OF PLUMES ON EUROPA WITH HST/STIS
Roth et al. (2014a) reported evidence for plumes of water venting from a southern high latitude
region on Europa – spectroscopic detection of off-limb line emission from the dissociation
products of water. Here, we present Hubble Space Telescope (HST) direct images of Europa in
the far ultraviolet (FUV) as it transited the smooth face of Jupiter, in order to measure absorption
from gas or aerosols beyond the Europa limb. Out of ten observations we found three in which
plume activity could be implicated. Two show statistically significant features at latitudes similar
to Roth et al., and the third, at a more equatorial location. We consider potential systematic
effects that might influence the statistical analysis and create artifacts, and are unable to find any
that can definitively explain the features, although there are reasons to be cautious. If the
apparent absorption features are real, the magnitude of implied outgassing is similar to that of the
Roth et al. feature, however the apparent activity appears more frequently in our data.
Tsunami wave extensively_resurfaced_the_shorelines_of_an_early_martian_ocean
It has been proposed that ~3.4 billion years ago an ocean fed by enormous catastrophic floods covered
most of the Martian northern lowlands. However, a persistent problem with this hypothesis is the
lack of definitive paleoshoreline features. Here, based on geomorphic and thermal image mapping in
the circum-Chryse and northwestern Arabia Terra regions of the northern plains, in combination with
numerical analyses, we show evidence for two enormous tsunami events possibly triggered by bolide
impacts, resulting in craters ~30km in diameter and occurring perhaps a few million years apart. The
tsunamis produced widespread littoral landforms, including run-up water-ice-rich and bouldery lobes,
which extended tens to hundreds of kilometers over gently sloping plains and boundary cratered
highlands, as well as backwash channels where wave retreat occurred on highland-boundary surfaces.
The ice-rich lobes formed in association with the younger tsunami, showing that their emplacement
took place following a transition into a colder global climatic regime that occurred after the older
tsunami event. We conclude that, on early Mars, tsunamis played a major role in generating and
resurfacing coastal terrains.
PALEOMAP Project Update by Christopher R. Scotese: 2013/Third Annual PaleoGIS...
PALEOMAP Project Update by Christopher R. Scotese: 2013/Third Annual PaleoGIS...The Rothwell Group, L.P.
This document provides an update on the PALEOMAP Project. It thanks sponsors who have supported the PaleoAtlas. It highlights accomplishments in 2013, including a new global plate model, finalizing over 100 paleogeographic time slices in the PaleoAtlas, and beginning work on an Earth System Archive to define over 50 paleoclimate and paleoenvironmental variables. Plans for 2014 include further developing the Earth System Archive with additional paleoclimate simulations, adding new data layers to the PaleoAtlas, and continuing work on a book documenting Earth's history.Proterozoic Milankovitch cycles and the history of the solar system
The geologic record of Milankovitch climate cycles provides a rich
conceptual and temporal framework for evaluating Earth system
evolution, bestowing a sharp lens through which to view our
planet’s history. However, the utility of these cycles for constraining
the early Earth system is hindered by seemingly insurmountable
uncertainties in our knowledge of solar system behavior
(including Earth–Moon history), and poor temporal control for validation
of cycle periods (e.g., from radioisotopic dates). Here we
address these problems using a Bayesian inversion approach to
quantitatively link astronomical theory with geologic observation,
allowing a reconstruction of Proterozoic astronomical cycles, fundamental
frequencies of the solar system, the precession constant,
and the underlying geologic timescale, directly from stratigraphic
data. Application of the approach to 1.4-billion-year-old rhythmites
indicates a precession constant of 85.79 ± 2.72 arcsec/year (2σ),
an Earth–Moon distance of 340,900 ± 2,600 km (2σ), and length of
day of 18.68 ± 0.25 hours (2σ), with dominant climatic precession
cycles of ∼14 ky and eccentricity cycles of ∼131 ky. The results
confirm reduced tidal dissipation in the Proterozoic. A complementary
analysis of Eocene rhythmites (∼55 Ma) illustrates how the
approach offers a means to map out ancient solar system behavior
and Earth–Moon history using the geologic archive. The method
also provides robust quantitative uncertainties on the eccentricity
and climatic precession periods, and derived astronomical timescales.
As a consequence, the temporal resolution of ancient Earth
system processes is enhanced, and our knowledge of early solar
system dynamics is greatly improved.
A precise water_abundance_measurement_for_the_hot_jupiter_wasp_43b
This document presents a precise measurement of the water abundance in the atmosphere of the exoplanet WASP-43b using transmission and thermal emission spectroscopy from the Hubble Space Telescope. The key findings are:
1) The water content of WASP-43b's atmosphere is consistent with solar composition at planetary temperatures, ranging from 0.4 to 3.5 times the solar water abundance.
2) This metallicity measurement extends the trend seen in the solar system of lower metal enrichment for higher mass planets.
3) Measuring a planet's water content constrains its formation location in the protoplanetary disk and provides insight into planetary formation models.
Episodic Plate Tectonics on Europa: Evidence for Widespread Patches of Mobile...
A nearly pole-to-pole survey near 140°E longitude on Europa revealed many areas that exhibit past lateral surface motions, and these areas were examined to determine whether the motions can be described by systems of rigid plates moving across Europa's surface. Three areas showing plate-like behavior were examined in detail to determine the sequence of events that deformed the surface. All three areas were reconstructed to reveal the original pre-plate motion surfaces by performing multi-stage rotations of plates in spherical coordinates. Several motions observed along single plate boundaries were also noted in previous works, but this work links together isolated observations of lateral offsets into integrated systems of moving plates. Not all of the surveyed surface could be described by systems of rigid plates. There is evidence that the plate motions did not all happen at the same time, and that they are not happening today. We conclude that plate tectonic-like behavior on Europa occurs episodically, in limited regions, with less than 100 km of lateral motion accommodated along any particular boundary before plate motions cease. Europa may represent a world perched on the theoretical boundary between stagnant and mobile lid convective behavior, or it may represent an additional example of the wide variations in possible planetary convective regimes. Differences in observed strike-slip sense and plate rotation directions between the northern and southern hemispheres raise the question of whether tidal forces may influence plate motions
Final Year Project - Observation and Characterisation of Exoplanets
This document summarizes a student report on the observation and characterization of exoplanets. It explores various exoplanet detection techniques, recent increases in Earth-sized planet discoveries, and relationships between stellar and planetary parameters. The student conducted photometry on three known transiting exoplanets - Hat-P-25b, Wasp-43b, and Wasp-2b - using the Sedgwick telescope. Light curves were produced and used to calculate planetary properties. A program called the Exoplanetary Pixelization Transit Model was created and tested to better fit light curves computationally.
Geology-2016-Malusà et al-G37407.1
1) The study uses detrital zircon U-Pb geochronology on sandstone samples from the Adriatic foredeep ranging from 32-18 Ma to track the indentation of the Adriatic microplate beneath the Central Alps.
2) The ratio of Variscan to Caledonian zircon grains sharply increases at around 24-23 Ma, marking the westward shift of the Adriatic indenter and associated right-lateral motion along the Insubric fault.
3) This suggests the indentation of Adria beneath the Central Alps occurred around 24-23 Ma, providing the first time constraint on major strike-slip motion along the poorly dated Insubric fault.
Modern water at low latitudes on Mars: Potential evidence from dune surfaces
Landforms on the Martian surface are critical to understanding the nature of surface processes in the recent
past. However, modern hydroclimatic conditions on Mars remain enigmatic, as explanations for the formation
of observed landforms are ambiguous. We report crusts, cracks, aggregates, and bright polygonal ridges on the
surfaces of hydrated salt-rich dunes of southern Utopia Planitia (~25°N) from in situ exploration by the Zhurong
rover. These surface features were inferred to form after 1.4 to 0.4 million years ago. Wind and CO2 frost processes can be ruled out as potential mechanisms. Instead, involvement of saline water from thawed frost/snow is
the most likely cause. This discovery sheds light on more humid conditions of the modern Martian climate and
provides critical clues to future exploration missions searching for signs of extant life, particularly at low latitudes with comparatively warmer, more amenable surface temperatures.
Describe and explain satellite remote sensing mission for monitoring.pdf
Describe and explain satellite remote sensing mission for monitoring water, carbon and global
climate change.
Solution
In recent years, the subjects of water, carbon, and global climate change
have attracted worldwide attention by scientists and the media. Climate
change, whether associated with human- induced or natural
variations, has and will continue to be important to policy makers and the
public. It is clear from reports such as that by the Intergovernmental Panelon Climate Change
(IPCC) [1] that
Earth observations play a critical role in providing information for assessment
and modeling. Improving these observations, better quality and newvariables, is a goal of most
national
and intergovernmental space agencies. Major initiatives are under waythat will result in benefits
to a broad
range of our global society. In the United States, a decadal study [2] was recently completed by
the
Committee on Earth Science and Applications of the US National Research
Council. The committee called for a commitment from the U.S. administration
to Earth observations to secure benefits for mankind. The report gives both
direction and a large boost to U.S. satellite programs as it recommended NOAA
to restore key observational capabilities of satellite missions and also that NASA
and NOAA launch 17 new satellite missions in the next 10 years. The study also
adds an additional focus to these missions: societal benefits.
Other countries have also been expanding their Earth observation programs
with numerous advanced concept satellite missions. Of particular relevance to
this issue are articles describing the
Earth observing programs of the
European Space Agency (ESA),
the Japanese Aerospace Exploration
Agency (JAXA), the China National
Space Administration (CNSA), the
Canadian Space Agency (CSA), and
the National Space Program Office
(NSPO) of Taiwan.
The ESA has a long history of
Earth observation from space that
began with meteorological missions
and has included a series of increasingly
sophisticated radars that have
provided valuable data about climate
and the changing environment. The
ESA’s current and future Earth observing
is under its Living Planet
Programme and includes the Earth
Explorer, meteorological, and Sentinel
missions.
JAXA has supported a wide range
of satellite-based instruments and
platforms that have and will provide
global Earth observations for water,
carbon, and climate. Of particular
note for the future is the commitment
to the Global Change Observation
Mission (GCOM) that will launch a
series of two types of satellites (water
and climate) to provide consistent and
continuous observations of key variables
over a 15-year period.
In addition to the United States,
ESA, and JAXA programs, there are
strong satellite-based Earth observing
programs in Canada, China, Argentina,
Taiwan, and Brazil.
In this Special Issue some of the
most significant recent and future Earth
observing satellites planned to monitor
water, carbon and global clima.
Low upper limit_to_methane_abundance_on_mars
1) The Tunable Laser Spectrometer on the Curiosity rover measured methane in the Martian atmosphere on six occasions and found no detection of methane, with an upper limit of 1.3 parts per billion.
2) This contradicts previous orbital and ground-based observations over the last decade that reported detectable methane plumes containing tens of parts per billion of methane.
3) The low measured methane level is not consistent with calculations of methane dispersal from previous large plume detections and suggests methane is being destroyed more rapidly than can be explained by current models.
A continuum from_clear_to_cloudy_hot_jupiter_exoplanets_without_primordial_wa...
Uma pesquisa de 10 exoplanetas quentes, do tamanho de Júpiter, conduzida com os telescópios Spitzer e Hubble da NASA levou uma equipe de astrônomos a resolverem um mistério que já durava algum tempo – por que alguns desses mundos têm menos água do que o esperado? A descoberta, oferece novas ideias sobre uma vasta coleção de atmosferas planetárias na nossa galáxia e sobre como os planetas são formados.
Dos quase 2000 planetas confirmados orbitando outras estrelas, um subconjunto deles são planetas gasosos com características similares ao planeta Júpiter, mas, como suas órbitas são muito próximas de suas estrelas, eles são terrivelmente quentes.
A proximidade desses exoplanetas das suas estrelas, faz com que seja difícil observá-los. Devido a essa dificuldade, o Hubble só conseguiu explorar poucos desses exoplanetas, chamados de Júpiteres Quentes, no passado. Esses estudos iniciais descobriram que alguns planetas possuem menos água do que era previsto pelos modelos atmosféricos.
Uma equipe internacional de astrônomos tem atacado o problema fazendo o maior catálogo espectroscópico de atmosferas de exoplanetas até o momento. Todos os planetas no catálogo seguem órbitas orientadas de modo que o planeta passa em frente da estrela quando visto da Terra. Devido a esse trânsito, parte da luz da estrela viaja pela atmosfera externa do exoplaneta. “A atmosfera deixa sua impressão digital única na luz da estrela, que nós podemos estudar, quando ela chega até nós”, explicou a coautora Hannah Wakeford, do Goddard Space Flight Center da NASA , em Greenbelt, Maryland.
Fluvial Features of Mars
-Examined features ranging from valley systems in Margaritifer Sinus to inverted topography in Aeolis/Zephyria Plana
-Studied and analyzed MOLA, THEMIS-VIS, OMEGA, MOC, CRISM, HRSC, and CTX imagery
Beyond water on mars
Mars exploration has been guided by the search for water. The more complex quest by Mars Science
Laboratory for habitable environments should illuminate the Martian environmental history, and
possibly deliver insights into extraterrestrial life.
Mineralogy of a_mudstone_at_yellowknife_bay_gale_crater_mars
The document summarizes the mineralogical analysis of two mudstone samples, John Klein and Cumberland, collected from Yellowknife Bay on Mars by the Curiosity rover. X-ray diffraction analysis found that the samples contain detrital basaltic minerals, calcium sulfates, iron oxides/hydroxides, iron sulfides, amorphous material, and trioctahedral smectites. The smectite in John Klein has a basal spacing of ~10 Å indicating little water interlayer hydration, while Cumberland smectite has a spacing of ~13.2 Å, suggesting partial chloritization or interlayer ions that facilitate water retention. The mudstone minerals are similar to nearby eolian deposits but
Carboniferous_Permian_paleogeography_of the assembly of pangaea.pdf
This document summarizes the tectonic events surrounding the assembly of the supercontinent Pangaea from the Late Proterozoic to the Early Mesozoic. It describes three general sequences: 1) the breakup of Rodinia and drifting of continents in the Late Proterozoic, 2) the convergence and collisions of continents and terranes from the Ordovician to Devonian forming Laurussia, and 3) the final collisions of Gondwana with Laurussia and Siberia from the Mississippian to Permian assembling Pangaea, with eastern Pangaea assembling into the Early Mesozoic. It also provides a global reconstruction of the tectonic plates
The habitability of Proxima Centauri b - I. Irradiation, rotation and volatil...
Proxima b is a planet with a minimum mass of 1.3 M⊕ orbiting within the habitable zone (HZ) of Proxima Centauri, a very low-mass,
active star and the Sun’s closest neighbor. Here we investigate a number of factors related to the potential habitability of Proxima b
and its ability to maintain liquid water on its surface. We set the stage by estimating the current high-energy irradiance of the planet
and show that the planet currently receives 30 times more EUV radiation than Earth and 250 times more X-rays. We compute the time
evolution of the star’s spectrum, which is essential for modeling the flux received over Proxima b’s lifetime. We also show that Proxima
b’s obliquity is likely null and its spin is either synchronous or in a 3:2 spin-orbit resonance, depending on the planet’s eccentricity and
level of triaxiality. Next we consider the evolution of Proxima b’s water inventory. We use our spectral energy distribution to compute
the hydrogen loss from the planet with an improved energy-limited escape formalism. Despite the high level of stellar activity we find
that Proxima b is likely to have lost less than an Earth ocean’s worth of hydrogen (EOH) before it reached the HZ 100–200 Myr after
its formation. The largest uncertainty in our work is the initial water budget, which is not constrained by planet formation models. We
conclude that Proxima b is a viable candidate habitable planet.
Conclusive Results
This document discusses how satellite observations over the past 50 years have revolutionized the field of earth sciences. It describes how early satellite missions taught scientists not only about the earth but how to improve satellite technology. Precise measurements from satellites have enabled major advances in understanding plate tectonics, topography, seismology and more. The ubiquity of GPS has provided vital data on phenomena like sea level change, earthquakes and volcanoes. Open data policies have maximized the benefits of earth observations.
Mercator Ocean newsletter 42
This document summarizes three recent space missions - SMOS, GOCE, and CRYOSAT - and their applications to physical oceanography. SMOS measures sea surface salinity from space using an interferometric radiometer and has produced initial global salinity maps from SMOS observations, though accuracy goals have not yet been reached due to data processing challenges. GOCE measures Earth's gravity field and will help estimate ocean mean dynamic topography. CRYOSAT, though aimed at sea ice thickness, also provides altimeter data over oceans that can be combined with other altimeter missions.
Journey to Mars – Exploring Deep Space Habitation Avenues
Critical review and discussion on how existing advanced wastewater technologies can support mankind in making sustainable long duration space explorations, especially to reach the Martian surface.
Lilas_poster
1) The study examines the geomorphic evolution of the Lilas River fan delta in central Evia, Greece through geomorphic mapping, stratigraphic analysis of cores and samples, and dating.
2) Stratigraphic analysis identified marine deposits from 10-20m depth indicating past sea level rise, overlain by fluvial sediments marking the current Holocene delta. At least four former distributary channels were also identified.
3) The fan delta extended towards the south and north Evia Gulf and was classified as arcuate dominated by fluvial sediment supply, waves, and longshore drift. Progradation of 500m occurred at the current river mouth in the past 160 years, while the coast
RHEOLOGY Physical pharmaceutics-II notes for B.pharm 4th sem students
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Chapter 4 - Islamic Financial Institutions in Malaysia.pptx
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This document provides an update on the PALEOMAP Project. It thanks sponsors who have supported the PaleoAtlas. It highlights accomplishments in 2013, including a new global plate model, finalizing over 100 paleogeographic time slices in the PaleoAtlas, and beginning work on an Earth System Archive to define over 50 paleoclimate and paleoenvironmental variables. Plans for 2014 include further developing the Earth System Archive with additional paleoclimate simulations, adding new data layers to the PaleoAtlas, and continuing work on a book documenting Earth's history.Proterozoic Milankovitch cycles and the history of the solar system
The geologic record of Milankovitch climate cycles provides a rich
conceptual and temporal framework for evaluating Earth system
evolution, bestowing a sharp lens through which to view our
planet’s history. However, the utility of these cycles for constraining
the early Earth system is hindered by seemingly insurmountable
uncertainties in our knowledge of solar system behavior
(including Earth–Moon history), and poor temporal control for validation
of cycle periods (e.g., from radioisotopic dates). Here we
address these problems using a Bayesian inversion approach to
quantitatively link astronomical theory with geologic observation,
allowing a reconstruction of Proterozoic astronomical cycles, fundamental
frequencies of the solar system, the precession constant,
and the underlying geologic timescale, directly from stratigraphic
data. Application of the approach to 1.4-billion-year-old rhythmites
indicates a precession constant of 85.79 ± 2.72 arcsec/year (2σ),
an Earth–Moon distance of 340,900 ± 2,600 km (2σ), and length of
day of 18.68 ± 0.25 hours (2σ), with dominant climatic precession
cycles of ∼14 ky and eccentricity cycles of ∼131 ky. The results
confirm reduced tidal dissipation in the Proterozoic. A complementary
analysis of Eocene rhythmites (∼55 Ma) illustrates how the
approach offers a means to map out ancient solar system behavior
and Earth–Moon history using the geologic archive. The method
also provides robust quantitative uncertainties on the eccentricity
and climatic precession periods, and derived astronomical timescales.
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A precise water_abundance_measurement_for_the_hot_jupiter_wasp_43b
This document presents a precise measurement of the water abundance in the atmosphere of the exoplanet WASP-43b using transmission and thermal emission spectroscopy from the Hubble Space Telescope. The key findings are:
1) The water content of WASP-43b's atmosphere is consistent with solar composition at planetary temperatures, ranging from 0.4 to 3.5 times the solar water abundance.
2) This metallicity measurement extends the trend seen in the solar system of lower metal enrichment for higher mass planets.
3) Measuring a planet's water content constrains its formation location in the protoplanetary disk and provides insight into planetary formation models.
Episodic Plate Tectonics on Europa: Evidence for Widespread Patches of Mobile...
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2) The ratio of Variscan to Caledonian zircon grains sharply increases at around 24-23 Ma, marking the westward shift of the Adriatic indenter and associated right-lateral motion along the Insubric fault.
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Landforms on the Martian surface are critical to understanding the nature of surface processes in the recent
past. However, modern hydroclimatic conditions on Mars remain enigmatic, as explanations for the formation
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surfaces of hydrated salt-rich dunes of southern Utopia Planitia (~25°N) from in situ exploration by the Zhurong
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Describe and explain satellite remote sensing mission for monitoring water, carbon and global
climate change.
Solution
In recent years, the subjects of water, carbon, and global climate change
have attracted worldwide attention by scientists and the media. Climate
change, whether associated with human- induced or natural
variations, has and will continue to be important to policy makers and the
public. It is clear from reports such as that by the Intergovernmental Panelon Climate Change
(IPCC) [1] that
Earth observations play a critical role in providing information for assessment
and modeling. Improving these observations, better quality and newvariables, is a goal of most
national
and intergovernmental space agencies. Major initiatives are under waythat will result in benefits
to a broad
range of our global society. In the United States, a decadal study [2] was recently completed by
the
Committee on Earth Science and Applications of the US National Research
Council. The committee called for a commitment from the U.S. administration
to Earth observations to secure benefits for mankind. The report gives both
direction and a large boost to U.S. satellite programs as it recommended NOAA
to restore key observational capabilities of satellite missions and also that NASA
and NOAA launch 17 new satellite missions in the next 10 years. The study also
adds an additional focus to these missions: societal benefits.
Other countries have also been expanding their Earth observation programs
with numerous advanced concept satellite missions. Of particular relevance to
this issue are articles describing the
Earth observing programs of the
European Space Agency (ESA),
the Japanese Aerospace Exploration
Agency (JAXA), the China National
Space Administration (CNSA), the
Canadian Space Agency (CSA), and
the National Space Program Office
(NSPO) of Taiwan.
The ESA has a long history of
Earth observation from space that
began with meteorological missions
and has included a series of increasingly
sophisticated radars that have
provided valuable data about climate
and the changing environment. The
ESA’s current and future Earth observing
is under its Living Planet
Programme and includes the Earth
Explorer, meteorological, and Sentinel
missions.
JAXA has supported a wide range
of satellite-based instruments and
platforms that have and will provide
global Earth observations for water,
carbon, and climate. Of particular
note for the future is the commitment
to the Global Change Observation
Mission (GCOM) that will launch a
series of two types of satellites (water
and climate) to provide consistent and
continuous observations of key variables
over a 15-year period.
In addition to the United States,
ESA, and JAXA programs, there are
strong satellite-based Earth observing
programs in Canada, China, Argentina,
Taiwan, and Brazil.
In this Special Issue some of the
most significant recent and future Earth
observing satellites planned to monitor
water, carbon and global clima.
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2) This contradicts previous orbital and ground-based observations over the last decade that reported detectable methane plumes containing tens of parts per billion of methane.
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possibly deliver insights into extraterrestrial life.
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and its ability to maintain liquid water on its surface. We set the stage by estimating the current high-energy irradiance of the planet
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Mercator Ocean newsletter 42
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Date: May 29, 2024
Tags: Information Security, ISO/IEC 27001, ISO/IEC 42001, Artificial Intelligence, GDPR
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Remote Sensing and Geographic Information Systems
9
Changes in vegetation cover refer to variations in the distribution, composition, and overall
structure of plant communities across different temporal and spatial scales. These changes can
occur natural.
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Paleogene Atlas
- 1. See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/267569784 Atlas of Paleogene Paleogeographic Maps (Mollweide Projection), Maps 8-15, Volume 1, The Cenozoic, PALEOMAP Atlas for ArcGIS, PALEOMAP Project, Evanston, IL. Technical Report · June 2014 DOI: 10.13140/2.1.3417.6961 CITATIONS 15 READS 13,209 1 author: Christopher Robert Scotese Northwestern University 814 PUBLICATIONS 17,312 CITATIONS SEE PROFILE All content following this page was uploaded by Christopher Robert Scotese on 31 October 2014. The user has requested enhancement of the downloaded file.
- 3. Atlas of Paleogene Paleogeographic Maps This Atlas of Paleogne Paleogeographic Maps shows the changing paleogeography from the Paleocene (60.6 Ma) to the Late Oligocene (25.7 Ma). The maps are from volume 1 of the PALEOMAP PaleoAtlas for ArcGIS (Scotese, 2014). Absolute age assignments are from Ogg, Ogg & Gradstein (2008). For Maps 8, 10, 12, and 15, there are two versions of the paleogeography. One map shows the maximum highstand sea level (maximum flooding surface). The other map shows the minimum lowstand sea level (supersequence boundary). For each paleogeography there is an estimate of sea level change (m) relative to present- day sea level. The following maps are included in the Atlas of Paleogene Paleogeographic Maps: Map 08 Late Oligocene (Chattian, 25.7 Ma Ma) Aquitanian Superseqeunce Boundary & Late Oligocene Transgressive Systems Tract Map 09 Early Oligocene (Rupelian, 31.1 Ma) Maximum Flooding Surface Map 10 Late Eocene, (Priabonian, 35.6 Ma) Rupelian Supersequence Boundary & Priabonian Transgressive Systems Tract Map 11 late Middle Eocene (Bartonian, 38.8 Ma) Bartonian Transgressive Systems Tract Map 12 early Middle Eocene, (middle Lutetian, 44.6 Ma) Lutetian Maximum Flooding Surface & Lutetian Supersequence Boundary Map 13 Early Eocene (Ypresian, 52.2 Ma) Ypresian Maximum Flooding Surface Map 14 Paleocene/Eocene Boundary (PETM, Thanetian/Ypresian Boundary, 55.8 Ma) PETM Transgressive Systems Tract Map 15 Paleocene (Danian & Thanetian, 60.6 Ma) Paleocene Maximum Flooding Surface & Danian Supersequence Boundary This Atlas should be cited as: Scotese, C.R., 2014. Atlas of Paleogene Paleogeographic Maps (Mollweide Projection), Maps 8-15, Volume 1, The Cenozoic, PALEOMAP Atlas for ArcGIS, PALEOMAP Project, Evanston, IL. References Cited Ogg, J.G., Ogg, G., Gradstein, F.M., 2008. The Concise Geologic Time Scale, Cambridge University Press, Cambridge, UK, 177 pp. Scotese, C.R., 2014, The PALEOMAP Project PaleoAtlas for ArcGIS, version 2, Volume 1, Cenozoic Plate Tectonic, Paleogeographic, and Paleoclimatic Reconstructions, Maps 1-15, PALEOMAP Project, Evanston, IL.