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Atmosphere of Earth
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"Air" redirects here. For other uses, see Air (disambiguation).
"Qualities of air" redirects here. It is not to be confused with Air quality.
Blue light is scattered more than other wavelengths by the gases in the atmosphere, giving Earth a blue halo when seen from space onboard ISS at a height of 402–424 km (250–263 mi)
Composition of Earth's atmosphere by volume. Lower pie represents trace gases that together compose about 0.038% of the atmosphere (0.043% with CO2 at 2014 concentration). Numbers are mainly from 1987, with CO2 and methane from 2009, and do not represent any single source.
The atmosphere of Earth is the layer of gases, commonly known as air, that surrounds the planet Earth and is retained by Earth's gravity. The atmosphere of Earth protects life on Earth by creating pressure allowing for liquid water to exist on the Earth's surface, absorbing ultraviolet solar radiation, warming the surface through heat retention (greenhouse effect), and reducing temperature extremes between day and night (the diurnal temperature variation).
By volume, dry air contains 78.09% nitrogen, 20.95% oxygen,[1] 0.93% argon, 0.04% carbon dioxide, and small amounts of other gases. Air also contains a variable amount of water vapor, on average around 1% at sea level, and 0.4% over the entire atmosphere. Air content and atmospheric pressure vary at different layers, and air suitable for use in photosynthesis by terrestrial plants and breathing of terrestrial animals is found only in Earth's troposphere and in artificial atmospheres.
The atmosphere has a mass of about 5.15×1018 kg,[2] three quarters of which is within about 11 km (6.8 mi; 36,000 ft) of the surface. The atmosphere becomes thinner and thinner with increasing altitude, with no definite boundary between the atmosphere and outer space. The Kármán line, at 100 km (62 mi), or 1.57% of Earth's radius, is often used as the border between the atmosphere and outer space. Atmospheric effects become noticeable during atmospheric reentry of spacecraft at an altitude of around 120 km (75 mi). Several layers can be distinguished in the atmosphere, based on characteristics such as temperature and composition.
The study of Earth's atmosphere and its processes is called atmospheric science (aerology). Early pioneers in the field include Léon Teisserenc de Bort and Richard Assmann.[3]
Contents
[hide]
1 Composition
2 Structure of the atmosphere
2.1 Principal layers
2.1.1 Exosphere
2.1.2 Thermosphere
2.1.3 Mesosphere
2.1.4 Stratosphere
2.1.5 Troposphere
2.2 Other layers
3 Physical properties
3.1 Pressure and thickness
3.2 Temperature and speed of sound
3.3 Density and mass
4 Optical properties
4.1 Scattering
4.2 Absorption
4.3 Emission
4.4 Refractive index
5 Circulation
6 Evolution of Earth's atmosphere
6.1 Earliest atmosphere
6.2 Second atmosphere
6.3 Third atmosphere
6.4 Air pollution
7 Images from space
8 See also
9 References
10 External links
Composition
Main article: Atmospheric chemistry
Mean atmospheric water vapor
The three major constituents of air, and therefore of Earth's atmosphere, are nitrogen, oxygen, and argon. Water vapor accounts for roughly 0.25% of the atmosphere by mass. The concentration of water vapor (a greenhouse gas) varies significantly from around 10 ppm by volume in the coldest portions of the atmosphere to as much as 5% by volume in hot, humid air masses, and concentrations of other atmospheric gases are typically quoted in terms of dry air (without water vapor).[4] The remaining gases are often referred to as trace gases,[5] among which are the greenhouse gases, principally carbon dioxide, methane, nitrous oxide, and ozone. Filtered air includes trace amounts of many other chemical compounds. Many substances of natural origin may be present in locally and seasonally variable small amounts as aerosols in an unfiltered air sample, including dust of mineral and organic composition, pollen and spores, sea spray, and volcanic ash. Various industrial pollutants also may be present as gases or aerosols, such as chlorine (elemental or in compounds), fluorine compounds and elemental mercury vapor. Sulfur compounds such as hydrogen sulfide and sulfur dioxide (SO2) may be derived from natural sources or from industrial air pollution.
Major constituents of dry air, by volume[6]
Gas
Volume(A)
Name
Formula
in ppmv(B)
in %
Nitrogen N2 780,840 78.084
Oxygen O2 209,460 20.946
Argon Ar 9,340 0.9340
Carbon dioxide CO2 400 0.04[7]
Neon Ne 18.18 0.001818
Helium He 5.24 0.000524
Methane CH4 1.79 0.000179
Not included in above dry atmosphere:
Water vapor(C) H2O 10–50,000(D) 0.001%–5%(D)
notes:
(A) volume fraction is equal to mole fraction for ideal gas only,
also see volume (thermodynamics)
(B) ppmv: parts per million by volume
(C) Water vapor is about 0.25% by mass over full atmosphere
(D) Water vapor strongly varies locally[4]
The relative concentration of gasses remains constant until about 10,000 m (33,000 ft).[8]
Structure of the atmosphere
Earth's atmosphere Lower 4 layers of the atmosphere in 3 dimensions as seen diagonally from above the exobase. Layers drawn to scale, objects within the layers are not to scale. Aurorae shown here at the bottom of the thermosphere can actually form at any altitude in this atmospheric layer.
Principal layers
In general, air pressure and density decrease with altitude in the atmosphere. However, temperature has a more complicated profile with altitude, and may remain relatively constant or even increase with altitude in some regions (see the temperature section, below). Because the general pattern of the temperature/altitude profile is constant and measurable by means of instrumented balloon soundings, the temperature behavior provides a useful metric to distinguish atmospheric layers. In this way, Earth's atmosphere can be divided (called atmospheric stratification) into five main layers. Excluding the exosphere, the atmosphere has four primary layers, which are the troposphere, stratosphere, mesosphere, and thermosphere.[9] From highest to lowest, the five main layers are:
Exosphere: 700 to 10,000 km (440 to 6,200 miles)
Thermosphere: 80 to 700 km (50 to 440 miles)[10]
Mesosphere: 50 to 80 km (31 to 50 miles)
Stratosphere: 12 to 50 km (7 to 31 miles)
Troposphere: 0 to 12 km (0 to 7 miles)[11]
Exosphere
Main article: Exosphere
The exosphere is the outermost layer of Earth's atmosphere (i.e. the upper limit of the atmosphere). It extends from the exobase, which is located at the top of the thermosphere at an altitude of about 700 km above sea level, to about 10,000 km (6,200 mi; 33,000,000 ft) where it merges into the solar wind.
This layer is mainly composed of extremely low densities of hydrogen, helium and several heavier molecules including nitrogen, oxygen and carbon dioxide closer to the exobase. The atoms and molecules are so far apart that they can travel hundreds of kilometers without colliding with one another. Thus, the exosphere no longer behaves like a gas, and the particles constantly escape into space. These free-moving particles follow ballistic trajectories and may migrate in and out of the magnetosphere or the solar wind.
The exosphere is located too far above Earth for any meteorological phenomena to be possible. However, the aurora borealis and aurora australis sometimes occur in the lower part of the exosphere, where they overlap into the thermosphere. The exosphere contains most of the satellites orbiting Earth.
Thermosphere
Main article: Thermosphere
The thermosphere is the second-highest layer of Earth's atmosphere. It extends from the mesopause (which separates it from the mesosphere) at an altitude of about 80 km (50 mi; 260,000 ft) up to the thermopause at an altitude range of 500–1000 km (310–620 mi; 1,600,000–3,300,000 ft). The height of the thermopause varies considerably due to changes in solar activity.[10] Because the thermopause lies at the lower boundary of the exosphere, it is also referred to as the exobase. The lower part of the thermosphere, from 80 to 550 kilometres (50 to 342 mi) above Earth's surface, contains the ionosphere.
The temperature of the thermosphere gradually increases with height. Unlike the stratosphere beneath it, wherein a temperature inversion is due to the absorption of radiation by ozone, the inversion in the thermosphere occurs due to the extremely low density of its molecules. The temperature of this layer can rise as high as 1500 °C (2700 °F), though the gas molecules are so far apart that its temperature in the usual sense is not very meaningful. The air is so rarefied that an individual molecule (of oxygen, for example) travels an average of 1 kilometre (0.62 mi; 3300 ft) between collisions with other molecules.[12] Although the thermosphere has a high proportion of molecules with high energy, it would not feel hot to a human in direct contact, because its density is too low to conduct a significant amount of energy to or from the skin.
This layer is completely cloudless and free of water vapor. However, non-hydrometeorological phenomena such as the aurora borealis and aurora australis are occasionally seen in the thermosphere. The International Space Station orbits in this layer, between 350 and 420 km (220 and 260 mi).
Mesosphere
Main article: Mesosphere
The mesosphere is the third highest layer of Earth's atmosphere, occupying the region above the stratosphere and below the thermosphere. It extends from the stratopause at an altitude of about 50 km (31 mi; 160,000 ft) to the mesopause at 80–85 km (50–53 mi; 260,000–280,000 ft) above sea level.
Temperatures drop with increasing altitude to the mesopause that marks the top of this middle layer of the atmosphere. It is the coldest place on Earth and has an average temperature around −85 °C (−120 °F; 190 K).[13][14]
Just below the mesopause, the air is so cold that even the very scarce water vapor at this altitude can be sublimated into polar-mesospheric noctilucent clouds. These are the highest clouds in the atmosphere and may be visible to the naked eye if sunlight reflects off them about an hour or two after sunset or a similar length of time before sunrise. They are most readily visible when the Sun is around 4 to 16 degrees below the horizon. A type of lightning referred to as either sprites or ELVES occasionally forms far above tropospheric thunderclouds. The mesosphere is also the layer where most meteors burn up upon atmospheric entrance. It is too high above Earth to be accessible to jet-powered aircraft and balloons, and too low to permit orbital spacecraft. The mesosphere is mainly accessed by sounding rockets and rocket-powered aircraft.
Stratosphere
Main article: Stratosphere
The stratosphere is the second-lowest layer of Earth's atmosphere. It lies above the troposphere and is separated from it by the tropopause. This layer extends from the top of the troposphere at roughly 12 km (7.5 mi; 39,000 ft) above Earth's surface to the stratopause at an altitude of about 50 to 55 km (31 to 34 mi; 164,000 to 180,000 ft).
The atmospheric pressure at the top of the stratosphere is roughly 1/1000 the pressure at sea level. It contains the ozone layer, which is the part of Earth's atmosphere that contains relatively high concentrations of that gas. The stratosphere defines a layer in which temperatures rise with increasing altitude. This rise in temperature is caused by the absorption of ultraviolet radiation (UV) radiation from the Sun by the ozone layer, which restricts turbulence and mixing. Although the temperature may be −60 °C (−76 °F; 210 K) at the tropopause, the top of the stratosphere is much warmer, and may be near 0 °C.[15]
The stratospheric temperature profile creates very stable atmospheric conditions, so the stratosphere lacks the weather-producing air turbulence that is so prevalent in the troposphere. Consequently, the stratosphere is almost completely free of clouds and other forms of weather. However, polar stratospheric or nacreous clouds are occasionally seen in the lower part of this layer of the atmosphere where the air is coldest. The stratosphere is the highest layer that can be accessed by jet-powered aircraft.
Troposphere
Main article: Troposphere
The troposphere is the lowest layer of Earth's atmosphere. It extends from Earth's surface to an average height of about 12 km, although this altitude actually varies from about 9 km (30,000 ft) at the poles to 17 km (56,000 ft) at the equator,[11] with some variation due to weather. The troposphere is bounded above by the tropopause, a boundary marked in most places by a temperature inversion (i.e. a layer of relatively warm air above a colder one), and in others by a zone which is isothermal with height.[16][17]
Although variations do occur, the temperature usually declines with increasing altitude in the troposphere because the troposphere is mostly heated through energy transfer from the surface. Thus, the lowest part of the troposphere (i.e. Earth's surface) is typically the warmest section of the troposphere. This promotes vertical mixing (hence the origin of its name in the Greek word τρόπος, tropos, meaning "turn"). The troposphere contains roughly 80% of the mass of Earth's atmosphere.[18] The troposphere is denser than all its overlying atmospheric layers because a larger atmospheric weight sits on top of the troposphere and causes it to be most severely compressed. Fifty percent of the total mass of the atmosphere is located in the lower 5.6 km (18,000 ft) of the troposphere.
Nearly all atmospheric water vapor or moisture is found in the troposphere, so it is the layer where most of Earth's weather takes place. It has basically all the weather-associated cloud genus types generated by active wind circulation, although very tall cumulonimbus thunder clouds can penetrate the tropopause from below and rise into the lower part of the stratosphere. Most conventional aviation activity takes place in the troposphere, and it is the only layer that can be accessed by propeller-driven aircraft.
Space Shuttle Endeavour orbiting in the thermosphere. Because of the angle of the photo, it appears to straddle the stratosphere and mesosphere that actually lie more than 250 km below. The orange layer is the troposphere, which gives way to the whitish stratosphere and then the blue mesosphere.[19]
Other layers
Within the five principal layers that are largely determined by temperature, several secondary layers may be distinguished by other properties:
The ozone layer is contained within the stratosphere. In this layer ozone concentrations are about 2 to 8 parts per million, which is much higher than in the lower atmosphere but still very small compared to the main components of the atmosphere. It is mainly located in the lower portion of the stratosphere from about 15–35 km (9.3–21.7 mi; 49,000–115,000 ft), though the thickness varies seasonally and geographically. About 90% of the ozone in Earth's atmosphere is contained in the stratosphere.
The ionosphere is a region of the atmosphere that is ionized by solar radiation. It is responsible for auroras. During daytime hours, it stretches from 50 to 1,000 km (31 to 621 mi; 160,000 to 3,280,000 ft) and includes the mesosphere, thermosphere, and parts of the exosphere. However, ionization in the mesosphere largely ceases during the night, so auroras are normally seen only in the thermosphere and lower exosphere. The ionosphere forms the inner edge of the magnetosphere. It has practical importance because it influences, for example, radio propagation on Earth.
The homosphere and heterosphere are defined by whether the atmospheric gases are well mixed. The surface-based homosphere includes the troposphere, stratosphere, mesosphere, and the lowest part of the thermosphere, where the chemical composition of the atmosphere does not depend on molecular weight because the gases are mixed by turbulence.[20] This relatively homogeneous layer ends at the turbopause found at about 100 km (62 mi; 330,000 ft), the very edge of space itself as accepted by the FAI, which places it about 20 km (12 mi; 66,000 ft) above the mesopause.
Above this altitude lies the heterosphere, which includes the exosphere and most of the thermosphere. Here, the chemical composition varies with altitude. This is because the distance that particles can move without colliding with one another is large compared with the size of motions that cause mixing. This allows the gases to stratify by molecular weight, with the heavier ones, such as oxygen and nitrogen, present only near the bottom of the heterosphere. The upper part of the heterosphere is composed almost completely of hydrogen, the lightest element.[clarification needed]
The planetary boundary layer is the part of the troposphere that is closest to Earth's surface and is directly affected by it, mainly through turbulent diffusion. During the day the planetary boundary layer usually is well-mixed, whereas at night it becomes stably stratified with weak or intermittent mixing. The depth of the planetary boundary layer ranges from as little as about 100 metres (330 ft) on clear, calm nights to 3,000 m (9,800 ft) or more during the afternoon in dry regions.
The average temperature of the atmosphere at Earth's surface is 14 °C (57 °F; 287 K)[21] or 15 °C (59 °F; 288 K),[22] depending on the reference.[23][24][25]
Physical properties
Comparison of the 1962 US Standard Atmosphere graph of geometric altitude against air density, pressure, the speed of sound and temperature with approximate altitudes of various objects.[26]
Pressure and thickness
Main article: Atmospheric pressure
The average atmospheric pressure at sea level is defined by the International Standard Atmosphere as 101325 pascals (760.00 Torr; 14.6959 psi; 760.00 mmHg). This is sometimes referred to as a unit of standard atmospheres (atm). Total atmospheric mass is 5.1480×1018 kg (1.135×1019 lb),[27] about 2.5% less than would be inferred from the average sea level pressure and Earth's area of 51007.2 megahectares, this portion being displaced by Earth's mountainous terrain. Atmospheric pressure is the total weight of the air above unit area at the point where the pressure is measured. Thus air pressure varies with location and weather.
If the entire mass of the atmosphere had a uniform density from sea level, it would terminate abruptly at an altitude of 8.50 km (27,900 ft). It actually decreases exponentially with altitude, dropping by half every 5.6 km (18,000 ft) or by a factor of 1/e every 7.64 km (25,100 ft), the average scale height of the atmosphere below 70 km (43 mi; 230,000 ft). However, the atmosphere is more accurately modeled with a customized equation for each layer that takes gradients of temperature, molecular composition, solar radiation and gravity into account.
In summary, the mass of Earth's atmosphere is distributed approximately as follows:[28]
50% is below 5.6 km (18,000 ft).
90% is below 16 km (52,000 ft).
99.99997% is below 100 km (62 mi; 330,000 ft), the Kármán line. By international convention, this marks the beginning of space where human travelers are considered astronauts.
By comparison, the summit of Mt. Everest is at 8,848 m (29,029 ft); commercial airliners typically cruise between 10 km (33,000 ft) and 13 km (43,000 ft) where the thinner air improves fuel economy; weather balloons reach 30.4 km (100,000 ft) and above; and the highest X-15 flight in 1963 reached 108.0 km (354,300 ft).
Even above the Kármán line, significant atmospheric effects such as auroras still occur. Meteors begin to glow in this region, though the larger ones may not burn up until they penetrate more deeply. The various layers of Earth's ionosphere, important to HF radio propagation, begin below 100 km and extend beyond 500 km. By comparison, the International Space Station and Space Shuttle typically orbit at 350–400 km, within the F-layer of the ionosphere where they encounter enough atmospheric drag to require reboosts every few months. Depending on solar activity, satellites can experience noticeable atmospheric drag at altitudes as high as 700–800 km.
Temperature and speed of sound
Main articles: Atmospheric temperature and Speed of sound
Temperature trends in two thick layers of the atmosphere as measured between January 1979 and December 2005 by Microwave Sounding Units and Advanced Microwave Sounding Units on NOAA weather satellites. The instruments record microwaves emitted from oxygen molecules in the atmosphere. Source:[29]
The division of the atmosphere into layers mostly by reference to temperature is discussed above. Temperature decreases with altitude starting at sea level, but variations in this trend begin above 11 km, where the temperature stabilizes through a large vertical distance through the rest of the troposphere. In the stratosphere, starting above about 20 km, the temperature increases with height, due to heating within the ozone layer caused by capture of significant ultraviolet radiation from the Sun by the dioxygen and ozone gas in this region. Still another region of increasing temperature with altitude occurs at very high altitudes, in the aptly-named thermosphere above 90 km.
Because in an ideal gas of constant composition the speed of sound depends only on temperature and not on the gas pressure or density, the speed of sound in the atmosphere with altitude takes on the form of the complicated temperature profile (see illustration to the right), and does not mirror altitudinal changes in density or pressure.
Density and mass
Temperature and mass density against altitude from the NRLMSISE-00 standard atmosphere model (the eight dotted lines in each "decade" are at the eight cubes 8, 27, 64, ..., 729)
Main article: Density of air
The density of air at sea level is about 1.2 kg/m3 (1.2 g/L, 0.0012 g/cm3). Density is not measured directly but is calculated from measurements of temperature, pressure and humidity using the equation of state for air (a form of the ideal gas law). Atmospheric density decreases as the altitude increases. This variation can be approximately modeled using the barometric formula. More sophisticated models are used to predict orbital decay of satellites.
The average mass of the atmosphere is about 5 quadrillion (5×1015) tonnes or 1/1,200,000 the mass of Earth. According to the American National Center for Atmospheric Research, "The total mean mass of the atmosphere is 5.1480×1018 kg with an annual range due to water vapor of 1.2 or 1.5×1015 kg, depending on whether surface pressure or water vapor data are used; somewhat smaller than the previous estimate. The mean mass of water vapor is estimated as 1.27×1016 kg and the dry air mass as 5.1352 ±0.0003×1018 kg."
Optical properties
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See also: Sunlight
Solar radiation (or sunlight) is the energy Earth receives from the Sun. Earth also emits radiation back into space, but at longer wavelengths that we cannot see. Part of the incoming and emitted radiation is absorbed or reflected by the atmosphere. In May 2017, glints of light, seen as twinkling from an orbiting satellite a million miles away, were found to be reflected light from ice crystals in the atmosphere.[30][31]
Scattering
Main article: Scattering
When light passes through Earth's atmosphere, photons interact with it through scattering. If the light does not interact with the atmosphere, it is called direct radiation and is what you see if you were to look directly at the Sun. Indirect radiation is light that has been scattered in the atmosphere. For example, on an overcast day when you cannot see your shadow there is no direct radiation reaching you, it has all been scattered. As another example, due to a phenomenon called Rayleigh scattering, shorter (blue) wavelengths scatter more easily than longer (red) wavelengths. This is why the sky looks blue; you are seeing scattered blue light. This is also why sunsets are red. Because the Sun is close to the horizon, the Sun's rays pass through more atmosphere than normal to reach your eye. Much of the blue light has been scattered out, leaving the red light in a sunset.
Absorption
Main article: Absorption (electromagnetic radiation)
Rough plot of Earth's atmospheric transmittance (or opacity) to various wavelengths of electromagnetic radiation, including visible light.
Different molecules absorb different wavelengths of radiation. For example, O2 and O3 absorb almost all wavelengths shorter than 300 nanometers. Water (H2O) absorbs many wavelengths above 700 nm. When a molecule absorbs a photon, it increases the energy of the molecule. This heats the atmosphere, but the atmosphere also cools by emitting radiation, as discussed below.
The combined absorption spectra of the gases in the atmosphere leave "windows" of low opacity, allowing the transmission of only certain bands of light. The optical window runs from around 300 nm (ultraviolet-C) up into the range humans can see, the visible spectrum (commonly called light), at roughly 400–700 nm and continues to the infrared to around 1100 nm. There are also infrared and radio windows that transmit some infrared and radio waves at longer wavelengths. For example, the radio window runs from about one centimeter to about eleven-meter waves.
Emission
Main article: Emission (electromagnetic radiation)
Emission is the opposite of absorption, it is when an object emits radiation. Objects tend to emit amounts and wavelengths of radiation depending on their "black body" emission curves, therefore hotter objects tend to emit more radiation, with shorter wavelengths. Colder objects emit less radiation, with longer wavelengths. For example, the Sun is approximately 6,000 K (5,730 °C; 10,340 °F), its radiation peaks near 500 nm, and is visible to the human eye. Earth is approximately 290 K (17 °C; 62 °F), so its radiation peaks near 10,000 nm, and is much too long to be visible to humans.
Because of its temperature, the atmosphere emits infrared radiation. For example, on clear nights Earth's surface cools down faster than on cloudy nights. This is because clouds (H2O) are strong absorbers and emitters of infrared radiation. This is also why it becomes colder at night at higher elevations.
The greenhouse effect is directly related to this absorption and emission effect. Some gases in the atmosphere absorb and emit infrared radiation, but do not interact with sunlight in the visible spectrum. Common examples of these are CO2 and H2O.
Refractive index
See also: Scintillation (astronomy)
The refractive index of air is close to, but just greater than 1. Systematic variations in refractive index can lead to the bending of light rays over long optical paths. One example is that, under some circumstances, observers onboard ships can see other vessels just over the horizon because light is refracted in the same direction as the curvature of Earth's surface.
The refractive index of air depends on temperature, giving rise to refraction effects when the temperature gradient is large. An example of such effects is the mirage.
Circulation
Main article: Atmospheric circulation
An idealised view of three large circulation cells.
Atmospheric circulation is the large-scale movement of air through the troposphere, and the means (with ocean circulation) by which heat is distributed around Earth. The large-scale structure of the atmospheric circulation varies from year to year, but the basic structure remains fairly constant because it is determined by Earth's rotation rate and the difference in solar radiation between the equator and poles.
Evolution of Earth's atmosphere
See also: History of Earth and Paleoclimatology
Earliest atmosphere
The first atmosphere consisted of gases in the solar nebula, primarily hydrogen. There were probably simple hydrides such as those now found in the gas giants (Jupiter and Saturn), notably water vapor, methane and ammonia. As the solar nebula dissipated, these gases escaped, partly driven off by the solar wind.[32]
Second atmosphere
Outgassing from volcanism, supplemented by gases produced during the late heavy bombardment of Earth by huge asteroids, produced the next atmosphere, consisting largely of nitrogen plus carbon dioxide and inert gases.[32] A major part of carbon-dioxide emissions soon dissolved in water and built up carbonate sediments.[clarification needed]
Researchers have found water-related sediments dating from as early as 3.8 billion years ago.[33] About 3.4 billion years ago, nitrogen formed the major part of the then stable "second atmosphere". An influence of life has to be taken into account rather soon in the history of the atmosphere, because hints of early life-forms appear as early as 3.5 billion years ago.[34] How Earth at that time maintained a climate warm enough for liquid water and life, if the early Sun put out 30% lower solar radiance than today, is a puzzle known as the "faint young Sun paradox".
The geological record however shows a continually relatively warm surface during the complete early temperature record of Earth - with the exception of one cold glacial phase about 2.4 billion years ago. In the late Archean Eon an oxygen-containing atmosphere began to develop, apparently produced by photosynthesizing cyanobacteria (see Great Oxygenation Event), which have been found as stromatolite fossils from 2.7 billion years ago. The early basic carbon isotopy (isotope ratio proportions) strongly suggests conditions similar to the current, and that the fundamental features of the carbon cycle became established as early as 4 billion years ago.
Ancient sediments in the Gabon dating from between about 2,150 and 2,080 million years ago provide a record of Earth's dynamic oxygenation evolution. These fluctuations in oxygenation were likely driven by the Lomagundi carbon isotope excursion.[35]
Third atmosphere
Oxygen content of the atmosphere over the last billion years[36][37]
The constant re-arrangement of continents by plate tectonics influences the long-term evolution of the atmosphere by transferring carbon dioxide to and from large continental carbonate stores. Free oxygen did not exist in the atmosphere until about 2.4 billion years ago during the Great Oxygenation Event and its appearance is indicated by the end of the banded iron formations.
Before this time, any oxygen produced by photosynthesis was consumed by oxidation of reduced materials, notably iron. Molecules of free oxygen did not start to accumulate in the atmosphere until the rate of production of oxygen began to exceed the availability of reducing materials that removed oxygen. This point signifies a shift from a reducing atmosphere to an oxidizing atmosphere. O2 showed major variations until reaching a steady state of more than 15% by the end of the Precambrian.[38] The following time span from 541 million years ago to the present day is the Phanerozoic Eon, during the earliest period of which, the Cambrian, oxygen-requiring metazoan life forms began to appear.
The amount of oxygen in the atmosphere has fluctuated over the last 600 million years, reaching a peak of about 30% around 280 million years ago, significantly higher than today's 21%. Two main processes govern changes in the atmosphere: Plants use carbon dioxide from the atmosphere, releasing oxygen. Breakdown of pyrite and volcanic eruptions release sulfur into the atmosphere, which oxidizes and hence reduces the amount of oxygen in the atmosphere. However, volcanic eruptions also release carbon dioxide, which plants can convert to oxygen. The exact cause of the variation of the amount of oxygen in the atmosphere is not known. Periods with much oxygen in the atmosphere are associated with rapid development of animals. Today's atmosphere contains 21% oxygen, which is high enough for this rapid development of animals.[39]
Play media
Animation shows the buildup of tropospheric CO2 in the Northern Hemisphere with a maximum around May. The maximum in the vegetation cycle follows in the late summer. Following the peak in vegetation, the drawdown of atmospheric CO2 due to photosynthesis is apparent, particularly over the boreal forests.
The scientific consensus is that the anthropogenic greenhouse gases currently accumulating in the atmosphere are the main cause of global warming.[40]
Air pollution
Main article: Air pollution
Air pollution is the introduction into the atmosphere of chemicals, particulate matter or biological materials that cause harm or discomfort to organisms.[41] Stratospheric ozone depletion is caused by air pollution, chiefly from chlorofluorocarbons and other ozone-depleting substances.
Images from space
On October 19, 2015 NASA started a website containing daily images of the full sunlit side of Earth on http://epic.gsfc.nasa.gov/. The images are taken from the Deep Space Climate Observatory (DSCOVR) and show Earth as it rotates during a day.[42]
Blue light is scattered more than other wavelengths by the gases in the atmosphere, giving Earth a blue halo when seen from space.
The geomagnetic storms cause beautiful displays of aurora across the atmosphere.
Limb view, of Earth's atmosphere. Colors roughly denote the layers of the atmosphere.
This image shows the Moon at the centre, with the limb of Earth near the bottom transitioning into the orange-colored troposphere. The troposphere ends abruptly at the tropopause, which appears in the image as the sharp boundary between the orange- and blue-colored atmosphere. The silvery-blue noctilucent clouds extend far above Earth's troposphere.
Earth's atmosphere backlit by the Sun in an eclipse observed from deep space onboard Apollo 12 in 1969.
See also
Aerial perspective
Air (classical element)
Air glow
Airshed
Atmosphere (on atmospheres in general)
Atmospheric dispersion modeling
Atmospheric electricity
Atmospheric models
Atmospheric Radiation Measurement (ARM) (in the U.S.)
Atmospheric stratification
Aviation
Biosphere
Carbon dioxide in Earth's atmosphere
Compressed air
COSPAR international reference atmosphere (CIRA)
Environmental impact of aviation
Global dimming
Historical temperature record
Hydrosphere
Hypermobility (travel)
Kyoto Protocol
Leaching (agriculture)
Lithosphere
Standard Dry Air
U.S. Standard Atmosphere
Warm period
Water vapor in Earth's atmosphere
Ozone layer
Atmosphere portal
Environment portal
References
Jump up ^ Zimmer, Carl (3 October 2013). "Earth's Oxygen: A Mystery Easy to Take for Granted". New York Times. Retrieved 3 October 2013.
Jump up ^ Lide, David R. Handbook of Chemistry and Physics. Boca Raton, FL: CRC, 1996: 14-7
Jump up ^ [1] Ultraviolet radiation in the solar system By Manuel Vázquez, Arnold Hanslmeier
^ Jump up to: a b Wallace, John M. and Peter V. Hobbs. Atmospheric Science; An Introductory Survey.Elsevier. Second Edition, 2006. ISBN 978-0-12-732951-2. Chapter 1
Jump up ^ "Trace Gases". Ace.mmu.ac.uk. Archived from the original on 9 October 2010. Retrieved 2010-10-16.
Jump up ^ Source for figures: Carbon dioxide, NOAA Earth System Research Laboratory, (updated 2013-03). Methane, IPCC TAR table 6.1 Archived 2007-06-15 at the Wayback Machine., (updated to 1998). The NASA total was 17 ppmv over 100%, and CO2 was increased here by 15 ppmv. To normalize, N2 should be reduced by about 25 ppmv and O2 by about 7 ppmv.
Jump up ^ Vaughan, Adam (2015-05-06). "Global carbon dioxide levels break 400ppm milestone". The Guardian. ISSN 0261-3077. Retrieved 2016-12-25.
Jump up ^ "Air Composition". The Engineering ToolBox. Retrieved 2017-07-04. The composition of air is unchanged until elevation of approximately 10.000 m
Jump up ^ Zell, Holly (2015-03-02). "Earth's Upper Atmosphere". NASA. Retrieved 2017-02-20.
^ Jump up to: a b Randy Russell (2008). "The Thermosphere". Retrieved 2013-10-18.
^ Jump up to: a b "The height of the tropopause". Das.uwyo.edu. Retrieved 2012-04-18.
Jump up ^ Ahrens, C. Donald. Essentials of Meteorology. Published by Thomson Brooks/Cole, 2005.
Jump up ^ States, Robert J.; Gardner, Chester S. (January 2000). "Thermal Structure of the Mesopause Region (80–105 km) at 40°N Latitude. Part I: Seasonal Variations". Journal of the Atmospheric Sciences 2000. 57: 66–77. Bibcode:2000JAtS...57...66S. doi:10.1175/1520-0469(2000)057<0066:TSOTMR>2.0.CO;2.
Jump up ^ Joe Buchdahl. "Atmosphere, Climate & Environment Information Programme". Ace.mmu.ac.uk. Archived from the original on 2010-07-01. Retrieved 2012-04-18.
Jump up ^ Journal of the Atmospheric Sciences (1993). "stratopause". Retrieved 2013-10-18.
Jump up ^ Barry, R.G. & Chorley R.J. (1971). Atmosphere, Weather and Climate. London, Menthuen & Co Ltd., p. 65
Jump up ^ Tyson, P.D., Preston-Whyte, R.A. (2013). The Weather and Climate of Southern Africa. (Second Edition). Oxford, Oxford University Press. p. 4.
Jump up ^ McGraw-Hill Concise Encyclopedia of Science & Technology. (1984). Troposphere. "It contains about four-fifths of the mass of the whole atmosphere."
Jump up ^ "ISS022-E-062672 caption". NASA. Retrieved 21 September 2012.
Jump up ^ "''homosphere''—AMS Glossary". Amsglossary.allenpress.com. Archived from the original on 14 September 2010. Retrieved 2010-10-16.
Jump up ^ "Earth's Atmosphere". Archived from the original on 2009-06-14.
Jump up ^ "NASA — Earth Fact Sheet". Nssdc.gsfc.nasa.gov. Archived from the original on 30 October 2010. Retrieved 2010-10-16.
Jump up ^ "Global Surface Temperature Anomalies". Archived from the original on 2009-03-03.
Jump up ^ "Earth's Radiation Balance and Oceanic Heat Fluxes". Archived from the original on 2005-03-03.
Jump up ^ "Coupled Model Intercomparison Project Control Run" (PDF). Archived from the original (PDF) on 2008-05-28.
Jump up ^ Geometric altitude vs. temperature, pressure, density, and the speed of sound derived from the 1962 U.S. Standard Atmosphere.
Jump up ^ "The Mass of the Atmosphere: A Constraint on Global Analyses". Ams.allenpress.com. 1970-01-01. Retrieved 2010-10-16.
Jump up ^ Lutgens, Frederick K. and Edward J. Tarbuck (1995) The Atmosphere, Prentice Hall, 6th ed., pp14-17, ISBN 0-13-350612-6
Jump up ^ "Atmospheric Temperature Trends, 1979-2005 : Image of the Day". Earthobservatory.nasa.gov. 2000-01-01. Retrieved 2014-06-10.
Jump up ^ St. Fleur, Nicholas (19 May 2017). "Spotting Mysterious Twinkles on Earth From a Million Miles Away". New York Times. Retrieved 20 May 2017.
Jump up ^ Marshak, Alexander; Várnai, Tamás; Kostinski, Alexander (15 May 2017). "Terrestrial glint seen from deep space: oriented ice crystals detected from the Lagrangian point". Geophysical Research Letters. Bibcode:2017GeoRL..44.5197M. doi:10.1002/2017GL073248. Retrieved 20 May 2017.
^ Jump up to: a b Zahnle, K.; Schaefer, L.; Fegley, B. (2010). "Earth's Earliest Atmospheres". Cold Spring Harbor Perspectives in Biology. 2 (10): a004895. doi:10.1101/cshperspect.a004895. PMC 2944365  . PMID 20573713.
Jump up ^ B. Windley: The Evolving Continents. Wiley Press, New York 1984
Jump up ^ J. Schopf: Earth's Earliest Biosphere: Its Origin and Evolution. Princeton University Press, Princeton, N.J., 1983
Jump up ^ Timothy W. Lyons, Christopher T. Reinhard & Noah J. Planavsky (2014). "Atmospheric oxygenation three billion years ago". Nature. 506 (7488): 307–15. Bibcode:2014Natur.506..307L. doi:10.1038/nature13068. PMID 24553238.
Jump up ^ Martin, Daniel; McKenna, Helen; Livina, Valerie. "The human physiological impact of global deoxygenation". The Journal of Physiological Sciences. 67 (1): 97–106. doi:10.1007/s12576-016-0501-0. ISSN 1880-6546. Retrieved 2017-09-05.
Jump up ^ http://www.nap.edu/openbook/0309100615/gifmid/30.gif
Jump up ^ Christopher R. Scotese, Back to Earth History : Summary Chart for the Precambrian, Paleomar Project
Jump up ^ Peter Ward:[2] Out of Thin Air: Dinosaurs, Birds, and Earth's Ancient Atmosphere
Jump up ^ "Summary for Policymakers" (PDF). Climate Change 2007: The Physical Science Basis. Contribution of Working Group I to the Fourth Assessment Report of the Intergovernmental Panel on Climate Change. Intergovernmental Panel on Climate Change. 5 February 2007.
Jump up ^ Starting from [3] Pollution—Definition from the Merriam-Webster Online Dictionary
Jump up ^ Northon, Karen. "Daily Views of Earth Available on New NASA Website". NASA. Retrieved 2015-10-21.
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text:
Bachelor in Paradise (season 1)
From Wikipedia, the free encyclopedia
Jump to: navigation, search
Bachelor in Paradise (season 1)
Country of origin
United States
No. of episodes
7
Release
Original network
ABC
Original release
August 4 (2014-08-04) – September 8, 2014 (2014-09-08)
Season chronology
Next →
Season 2
The first season of Bachelor in Paradise premiered on August 4, 2014, a week after season ten of The Bachelorette, with the season finale airing on September 8, 2014. Chris Harrison reprised his role from The Bachelor and The Bachelorette as the host of the show.
Contents
[hide]
1 Production
2 Contestants
2.1 Elimination Table
2.2 Key
3 Episodes
3.1 Episode 1
3.2 Episode 2
3.3 Episode 3
3.4 Episode 4
3.5 Episode 5
3.6 Episode 6
3.7 Episode 7
4 Post Show
5 References
6 External links
Production[edit]
In March 2013, ABC canceled Bachelor Pad after three seasons. ABC then announced a new spin-off series, Bachelor In Paradise. The season was filmed in Tulum, Mexico.[1][2]
Contestants[edit]
The first batch of contestants were revealed on June 4, 2014, but only 14 contestants were confirmed. On July 14, 2014, an additional 11 contestants were revealed, resulting in 25 contestants.[1][3][4][5][6][7][8][9]
Name
Age
Occupation
Residence
From
Arrived
Eliminated
Lacy Faddoul 26 Nursing Home Owner La Jolla, CA The Bachelor, Season 18 Week 1 Engaged
Marcus Grodd 26 Sports Medicine Manager Dallas, TX The Bachelorette, Season 10 Week 1 Engaged
Michelle Money 33 Hairstylist Salt Lake City, UT The Bachelor, Season 15 Week 1 Relationship
Cody Sattler 28 Personal Trainer Chicago, IL The Bachelorette, Season 10 Week 4 Relationship
Robert Graham 31 Advertising Entrepreneur Los Angeles, CA The Bachelorette, Season 9 Week 1 Split Week 7
Sarah Herron 27 Art Director Marina del Ray, CA The Bachelor, Season 17 Week 1 Split Week 7
Zack Kalter 29 Book Publisher Los Angeles, CA The Bachelorette, Season 9 Week 2 Split Week 7
Jackie Parr 26 Cosmetics Consultant Boca Raton, FL The Bachelor, Season 17 Week 3 Split Week 7
Christy Hansen 25 Hairstylist Chicago, IL The Bachelor, Season 18 Week 5 Split Week 7
Tasos Hernandez 30 Wedding Event Coordinator Denver, CO The Bachelorette, Season 10 Week 6 Split Week 7
Graham Bunn 35 Entrepreneur New York, NY The Bachelorette, Season 4 Week 1 Split Week 7
AshLee Frazier 33 Personal Organizer Houston, TX The Bachelor, Season 17 Week 1 Split Week 7
Brooks Forester 29 Entrepreneur Salt Lake City, UT The Bachelorette, Season 9 Week 6 Week 6
Jesse Kovacs 32 Winemaker San Diego, CA The Bachelorette, Season 5 Week 4 Week 6 (Quit)
Lucy Aragon 25 Free Spirit Santa Barbara, CA The Bachelor, Season 18 Week 5 Week 5
Clare Crawley 33 Hairstylist Sacramento, CA The Bachelor, Season 18 Week 1 Week 5 (Quit)
Kalon McMahon 29 Entrepreneur Houston, TX The Bachelorette, Season 8 Week 4 Week 4
Marquel Martin 27 Sponsorship Salesman Las Vegas, NV The Bachelorette, Season 10 Week 1 Week 4
Danielle Ronco 26 Psychiatric Nurse St. Louis, MO The Bachelor, Season 18 Week 3 Week 3
Elise Mosca 28 Bartender Los Angeles, CA The Bachelor, Season 18 Week 1 Week 3 (Quit)
Chris Bukowski 27 Entrepreneur Washington, D.C. The Bachelorette, Season 8 Week 2 Week 3 (Quit)
Dylan Petitt 26 Accountant Boston, MA The Bachelorette, Season 10 Week 1 Week 2
Ben Scott 30 Sales Representative Dallas, TX The Bachelorette, Season 9 Week 1 Week 2 (Quit)
Daniella McBride 26 Commercial Casting Associate San Francisco, CA The Bachelor, Season 17 Week 1 Week 1
Michelle Kujawa 30 Sales Anaheim, CA The Bachelor, Season 14 Week 1 Week 1 (Quit)
Elimination Table[edit]
Place
Contestant
Week
1
2
3
4
5
6
7
1-4 Lacy Date (Robert) Date (Marcus) In Date (Marcus) In Date (Marcus) In Stay (Marcus)
Marcus Date (Sarah) Date (Lacy) In Date (Lacy) In Date (Lacy) In Stay (Lacy)
Michelle M. Date (Marquel) In Last In Date (Cody) In In Stay (Cody)
Cody Wait In Date (Michelle M.) In In Stay (Michelle M.)
5-6 Sarah Last (Marcus) Date (Dylan) In Date (Robert) Date (Robert) In In Split (Robert)
Robert Date (Lacy/Clare) Last In Date (Sarah) Date (Sarah) In In Split (Sarah)
7-12 Jackie Wait Date (Marquel) Date (Jesse) In Date (Brooks/Zack) Split (Zack)
Zack Wait Date (Clare) In In In Last (Jackie) Split (Jackie)
Christy Wait Last (Jesse) Date (Tasos) Split (Tasos)
Tasos Wait Date (Christy) Split (Christy)
AshLee In In Date (Graham) In Date (Graham) In Split (Graham)
Graham In In Date (AshLee) In Date (AshLee) In Split (AshLee)
13 Brooks Wait Out (Jackie)
14 Jesse Wait Last (Jackie) Date (Christy/Lucy) Quit
15 Lucy Wait Out (Jesse)
16 Clare Date (Robert) Date (Chris/Zack) In In Quit
17-18 Kalon Wait Out (Kalon)
Marquel Date (Michelle M.) In Date (Danielle/Jackie) Out
19 Danielle Wait Out (Marquel)
20-21 Elise In In Quit (Chris)
Chris Wait Date (Clare) Quit (Elise)
22 Dylan In Out (Sarah)
23 Ben In Quit
24 Daniella Out
25 Michelle K. Quit
Key[edit]
The contestant is male.
The contestant is female.
Date The contestant had a date and gave out a rose at the rose ceremony.
Date The contestant went on a date and got a rose at the rose ceremony.
In The contestant gave or received a rose at the rose ceremony, thus remaining in the competition.
Last The contestant received the last rose.
Last The contestant went on a date and received the last rose.
Out The contestant went on a date and rejected a rose and ended up getting eliminated.
Out The contestant went on a date and was eliminated.
Out The contestant was eliminated.
Quit The contestant had a date and voluntarily left the show
Quit The contestant voluntarily left the show.
Quit The contestant quit the show after being in a relationship back home.
Quit The contestant quit due to injury.
Split The couple broke up and was eliminated.
Stay The couple decided to stay together and won the competition.
Wait The contestant had to wait to appear in paradise.
Episodes[edit]
Episode 1[edit]
Airdate: August 4, 2014
Arrival Order: Clare, Marcus, Sarah, Marquel, Daniella, Graham, Lacy, Ben, Michelle K., Robert, Dylan, Elise and AshLee.
Chris Harrison asked everyone if they were single and Michelle K. said "maybe". Throughout the first day, Lacy went into the ocean with Robert and Marcus in an 8-hour span. She went into the ocean while Marcus went in there by himself feeling rejected over bachelorette Andi Dorfman.
Clare's date: Clare initially wanted to take Graham on the date, but AshLee "claimed" Graham at the start, which made Clare go on a date with Robert. Clare and Robert went to the ruins; while climbing the ruins, Robert got attacked by fire ants.
Sarah's date: Sarah took Marcus on a date and went cliff diving. During the date, Michelle Money joined the cast in Mexico.
Michelle M.'s date: Michelle M. arrived with a date card and took Marquel, they went horseback riding on a beach in Playa del Carmen.
Lacy's date: Lacy took Robert on a date and they had dinner on a beach.
Rose ceremony: The rose ceremony came after a cocktail party. Before the first rose was handed out Michelle K. stepped out and left because she never had any feelings for a guy. In order Marquel gave his rose to Michelle M., Graham gave his rose to AshLee, Dylan gave his rose to Elise, Marcus gave his rose to Lacy which upset Robert who then gave his rose to Clare, Ben had the final rose which he gave to Sarah over Daniella eliminating her.
Episode 2[edit]
Airdate: August 11, 2014
Chris's Date: Chris showed up with a date card and he took Clare to Papaya Playa on a trip to a spa. During the date Dylan tells Elise to talk to other men in paradise.
Marcus's Date: Marcus took Lacy on a date and they had dinner in Zcaret. During the date Elise did what Dylan requested which was hooking up with Chris in the ocean, they had a conversation about this the next day and Dylan told Elise if she offered him a rose, he would reject it.
Zack's Date: Zack showed up with a date card and took Clare to the city to explore, then went swimming in the ocean.
Dylan's Date: Dylan took Sarah on a date and had dinner.
Before the Rose Ceremony, Marcus and Marquel confronted Ben upon finding a love letter in his backpack from a girl back home. Ben admitted to being in love with her, upsetting everyone especially Michelle, and decided to go home.
Rose Ceremony Lacy gives her rose to Marcus, Ashlee gives hers to Graham, Clare to Zack, Michelle to Marquel, Elise gives hers to Dylan but he declines, so she gives it to Chris instead, Sarah gives her rose to Robert over Dylan, eliminating him.
Episode 3[edit]
Airdate: August 18, 2014
Elise's Date: Elise asked Chris out. Before the date began, Chris sprained his knee. He decided to go through with the date, despite being in great pain. Immediately after the date he went to the hospital for treatment.
Danielle: Danielle showed up at the bachelor house with a date. She asked Marquel to go on the date and they went swimming.
At the house, Michelle and Clare decided to take Zack and Robert on a mini double date. Sarah was pretty upset about this.
Jackie: Jackie showed up with a date card. She decided to take Marquel as well for his second date this week. Danielle and Michelle were a little upset about this. They went the Campeche Mexico and explored. They shared a kiss after Marquel and Jackie both said they don't usually kiss on the first date.
Sarah and the others expressed their concern to Elise about being careful with Chris and not getting too serious too fast.
AshLee: Ashlee asked Graham to go on her date with her. They went to dinner. AshLee started talking about living together and Graham asked her to not put pressure on forever anymore. They got a card from Chris Harrison with two room keys. Graham wanted to use both rooms, but Ashlee wanted to share a room. They ended up using both rooms.
Rose Ceremony: Graham gave his rose to Ashlee. Zack gave his rose to Clare. Marcus gave his rose to Lacy. Marquel gave his rose to Jackie. Robert gave his rose to Sarah. Chris asked Elise to come forward. He told Elise that he could not give her the rose, because he had decided to leave the show due to his knee injury. Instead, he asked Elise to leave along with him so they could continue to pursue their relationship back home, and she accepted. Chris decided to give his rose to Michelle so she could continue her journey of true love. Danielle was eliminated.
Episode 4[edit]
Airdate: August 25, 2014
Robert: Robert gets the first date and decides to take Sarah. They go sailing and swimming in the ocean.
Cody's Date Card: Cody arrived with a date card. He asks Clare, but she decided to pass on the date because of Zack. Cody then decided to pass it to his friend Marcus, so he could have more time to get to know the people in the house. Many of the women thought that was a very nice gesture. Marcus takes Lacy.
Kalon's Date: Kalon arrived with a date card. He asked Michelle and she accepted, but then she cancelled on him. He asked a few other girls, but none of the women would go out with him (recalling how badly he had upset Emily Maynard in The Bachelorette (season 8). Feeling certain that he would be eliminated later at the Rose Ceremony, he decided to go by himself and enjoy it rather than pass the card, creating the show's first "one on none" date.
Jesse: Jesse shows up with a date card and he invites Jackie to go out with him. She accepts and Marquel is kind of upset. They go to an ancient Mayan Cave. The date is a little awkward at first, but gets better toward the end. Andrew Ripp performs.
Before the Rose Ceremony, AshLee said disrespectful things about Clare to Zack and her remarks were caught on camera. Word got back to Clare and she confronted AshLee about it. Michelle informed Graham about the situation right before the Rose Ceremony began. Graham started to have second thoughts about AshLee.
Rose Ceremony: Lacy gives her rose to Marcus. Clare gives her rose to Zack. AshLee asked Graham to come forward. At that point Graham turned and left the room. Michelle followed after him. AshLee continued to stand in the Rose Ceremony room and did not follow Graham. After seeing a medic, Graham returned and accepted the rose from AshLee. Then Lacy became ill and departed in an ambulance, accompanied by Marcus. The rose ceremony continued. Michelle gave her rose to Cody. Sarah gave her rose to Robert. Jackie gave her rose to Jesse. Kalon and Marquel were eliminated at the Rose Ceremony.
Episode 5[edit]
Airdate: August 26, 2014
Christy: Christy shows up with a date card and asks Zack to go with her, but he turns her down. Christy then asks Jesse to join her on the date. They go shopping in Mexico.
Lacy and Marcus return from the hospital.
Sarah: Sarah got a date card and asked Robert to join her. They go out to dinner and go swimming. They share a kiss.
Clare was still upset about the disrespectful comments from AshLee. She came to Zack to let him know that she had decided to quit.
Lucy's Date: Lucy arrived with a date card. She asked Jesse out and they went to some ruins.
Michelle's Date: Michelle asked Cody out and they had their 'engagement' photos taken on the beach, even though it was their first date.
AshLee's Date: She asked Graham out and they drove sports cars on a road course.
Christy began to feel insecure about her status with Jesse. She spoke to him and was reassured. They started to make out in private and were joined by Lucy.
Rose Ceremony: Sarah accepts Robert's rose. AshLee accepts Graham's rose. Cody gives his rose to Michelle. Lacy accepted Marcus' rose with a very long kiss. Zack gives his rose to Jackie. Jesse chose Christy over Lucy, so Lucy was eliminated.
Episode 6[edit]
Airdate: September 1, 2014
Marcus's Date: Marcus took Lacy on a date exploring in a cave. Lacy told Marcus she was falling in love with him.
Brooks' Date: Sarah was hoping that Brooks would ask her out, and Brooks wanted to do it, but Robert informed Brooks that he and Sarah were a couple and Brooks should pick someone else. Brooks asked Jackie out.
Tasos's Date: Tasos arrived with a date card. Tasos pulled Michelle aside first and told him he should take Christy. Tasos told her how great of a guy Cody was. Tasos asked Christy on the date and Jesse wasn't happy because he doesn't want to leave Paradise. On the date, Tasos and Christy go swimming in a lazy river.
Zack's Date: Zack asked Jackie on the date, and Brooks wasn't too thrilled. AshLee was also upset it wasn't Graham who got the date card. Zack and Jackie went swimming in a cave. They kissed.
Before the Rose Ceremony, Jesse had a talk with Christy and realized that he would not be getting a rose from her. He decided to quit at that point rather than be eliminated later. Before he could depart, Christy came to the car and told him all of the reasons that she was angry with him. Jesse didn't seem concerned by this, saying later that he had fun and he knew there would be lots of emails and party invitations waiting for him when he got home.
Rose Ceremony: Lacy gave her rose to Marcus. AshLee gave her rose to Graham. Sarah gave her rose to Robert. Michelle gave her rose to Cody. Christy to Tasos. Jackie gave her rose to Zack. Brooks was eliminated. Then Chris Harrison announced that there would be no more newcomers; the final episode would be a test of their new relationships.
Episode 7[edit]
Airdate: September 8, 2014
Chris Harrison asked each of the couples to have a serious talk with each other and decide whether to continue or go home. AshLee and Graham decided to split up after some prompting by Michelle. Zack, Jackie, Tasos and Christy all decided to break up. That left three couples: Sarah and Robert, Michelle and Cody, and Lacy and Marcus.
The three couples went on romantic overnight dates in fantasy suites. Lacy and Marcus and Michelle and Cody came back convinced that they should remain as couples. However, Sarah complained that there was little intimacy on their date. She confronted Robert about this and he just apologized and left with no explanation.
The two remaining couples were joined by three couples (Jason/Molly Mesnick, Sean/Catherine Lowe and Desiree Hartsock/Chris Seigfried) who had found love on the show in the past. They agreed that the two remaining couples had a good chance of making it work.
Rose Ceremony: Michelle and Cody exchanged roses and left as a couple. Marcus proposed to Lacy and she accepted.
In the epilogue, it was revealed that Chris and Elise broke up after less than two weeks. Michelle and Cody were still in a relationship at the time. Clare was still in Sacramento searching for her soulmate.
Post Show[edit]
In December 2014, Michelle and Cody announced that they decided to end their relationship, and got back together in June 2015, but later broke up again. In 2016 they appeared on Marriage Boot Camp, where they broke up again.
Marcus and Lacy were wed by Chris Harrison on the season premiere of season 2 of Bachelor in Paradise.[10] However, in July 2016 Marcus admitted that the two were never legally married and have since broken up.[11]
Clare returned to Paradise for season 2. She was eliminated in week 3.
References[edit]
^ Jump up to: a b Wong, Derek (July 14, 2014). "Bachelor in Paradise - Full Cast Announcement". ABC. Retrieved July 15, 2014.
Jump up ^ Bricker, Tierney (July 15, 2014). "Why You'll Want to Move Into the Bachelor in Paradise House and Never Leave". E! Online. Retrieved July 19, 2014.
Jump up ^ Nahas, Aili (June 4, 2014). "Bachelor in Paradise: Meet the Cast". People. Retrieved July 10, 2014.
Jump up ^ Nahas, Aili (June 18, 2014). "Michelle Money and Marquel Martin Join the Cast of Bachelor in Paradise". People. Retrieved July 10, 2014.
Jump up ^ Chiu, Melody (June 25, 2014). "Cody Sattler Joins the Cast of Bachelor in Paradise". People. Retrieved July 10, 2014.
Jump up ^ Kwiatkowski, Elizabeth (July 9, 2014). "'Bachelor in Paradise's final contestant formally revealed". Reality TV World. Retrieved July 10, 2014.
Jump up ^ Pierce, Scott (July 14, 2014). "2 Utahns will look for love on 'Bachelor in Paradise'". Salt Lake Tribune. Retrieved July 19, 2014.
Jump up ^ Duren, Rand (July 14, 2014). "‘Bachelorette’ Dallasites Ben Scott and Marcus Grodd will be on messy spinoff ‘Bachelor in Paradise’". Dallas News. Retrieved August 4, 2014.
Jump up ^ Spera, Rebecca (August 4, 2014). "Houstonians reveal secrets from 'Bachelor In Paradise'". ABC 13. Retrieved August 10, 2014.
Jump up ^ "Inside Marcus Grodd and Lacy Faddoul's 'Intimate' Bachelor in Paradise Wedding". People Magazine. August 3, 2017.
Jump up ^ "Bachelor in Paradise's Marcus Reveals His 'Embarrassment' About Messy Split From Lacy: 'I Feel Played'". Us Weekly. July 15, 2016. .
External links[edit]
Official website
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