I Can’t Sleep - Atmosphere | Gentle Reading to Help You Sleep

Episode Date: October 13, 2025

Relax with this calm bedtime reading about the atmosphere, perfect for easing insomnia and finding restful sleep. Drift off as Benjamin gently explores the layers, composition, and wonders of Earth’s protective air blanket. You’ll learn how the atmosphere sustains life, shields us from radiation, and creates the conditions that make our planet unique—all in a soothing, unhurried tone. Benjamin’s peaceful narration offers educational comfort without whispers or hypnosis, helping ease anxiety and promote relaxation for a better night’s rest. Press play, settle in, and let your mind float among the clouds. Happy sleeping! Read with permission from Atmosphere, Wikipedia (https://en.wikipedia.org/wiki/Atmosphere), licensed under CC BY-SA 4.0. Learn more about your ad choices. Visit megaphone.fm/adchoices

You're listening to a Glassbox Media podcast. What if I told you that most of the modern day self-help advice you've been hearing could actually make you worse? The key to a better life isn't about feel-good gimmicks that sound catchy. The Mentally Stronger Podcast gives you access to a licensed therapist who shares science-backed tools that will actually change your life. Hi, I'm Amy Morin, psychotherapist, mental strength trainer, and international best-selling author. In each episode, we cover research-back strategies, like how to stop relying on willpower and start creating habits for lasting change. And the five mental strength-building exercises you can do from your couch. I also speak to world-class experts like Dr. Nicole Kane, who shares how to permanently heal anxiety by addressing the root cause.

With over 200 episodes in our catalog, this podcast is for you if you're ready to crush self-doubt, conquer challenges, become stronger than ever with therapist-approved strategies that can change your life. Listen to Mentally Stronger with Therapist Amy Morin, wherever you get your podcasts. Welcome to the I Can't Sleep podcast where I help you drift off one fact at a time. I'm your host, Benjamin Boster, and today's episode is about atmospheres. An atmosphere is a layer of gases that envelop an astronomical object. held in place by the gravity of the object. The name originates from ancient Greek Atmos, vapor, steam, and spira, sphere.

An object acquires most of its atmosphere during its primordial epic, either by accretion of matter or by outgassing of volatiles. The chemical interaction of the atmosphere with the solid surface can change its fundamental composition, as can photochemical interaction with the sun. A planet retains an atmosphere for longer durations when the gravity is high and the temperature is low. The solar wind works to strip away a planet's outer atmosphere, although this process is slowed by a magnetosphere. The further a body is from the sun, the lower the rate of atmospheric stripping. All solar system Some planets, besides Mercury, have substantial atmospheres, as does the dwarf planet Pluto

and the moon Titan. The high gravity and low temperature of Jupiter and other gas giant planets allow them to retain massive atmospheres of mostly hydrogen and helium. Lower mass terrestrial planets orbit closer to the sun, and so mainly retain higher density the atmospheres made of carbon, nitrogen, and oxygen, with trace amounts of inner gas. Atmospheres have been detected around exoplanets, such as HD 209458B and Kepler 7B. A stellar atmosphere is the outer region of a star, which includes the layers above the opaque photosphere. Stars of a low temperature might have outer atmospheres containing compound molecules.

Other objects with atmospheres are brown dwarfs and active comets. In the nebular hypothesis, stars form during the gravitational collapse of a mass of gas and dust within an interstellar molecular cloud. This material forms a pancake-like rotating disk, with the mass concentrated at the center. The protostar is created at the central mass concentration, while the planets and satellites are formed in the disk through a process of accretion. Dust settles into the median disk plane, forming materials that can collide and accrete to create planetesimals. the star, these bodies grow and accumulate to form protoplanets, consisting primarily of refractory materials with few volatiles. Further from the star, planetary embryos are created from accumulation of volatiles, up to around 10 times the mass of the Earth or more. Masses of gas

are then acquired from the surrounding disk nebula, forming a gas giant around the embryo. Planetary satellites form in a similar fashion from the disk of material around the planets. The primary atmosphere of a planet is produced when the gravity is sufficient to retain accreted gas against escape processes. The latter can include collisions with other bodies

that impart sufficient energy for the gases to escape. For the terrestrial planets, the high temperatures generated by their initial bombardment results in the outgassing of volatiles, creating the secondary atmosphere. The original composition and thickness of the atmosphere is thus determined by the stellar nebula's chemistry and temperature, but can be modified by processes within the astronomical body that releases different atmospheric components. circumstellar disk will finally dissipate on timescales of about 10 to the 7th years, and the star will complete its contraction, then ignite hydrogen fusion at its core, in a time frame determined by its mass. For example, a star with the mass of the sun

will spend three times 10 to the 7th years contracting. The atmospheres of the planet's Venus and Mars are principally composed. of carbon dioxide, nitrogen, and argon. Because Venus has no oceans or rain to dissolve the carbon dioxide, large amounts of this greenhouse gas has remained in the atmosphere. The result is a dense atmosphere about 80 times the pressure of Earth's atmosphere. The planet's lack of a magnetic field and closer proximity to the sun resulted in the loss of its hydrogen in the form of water after two billion years.

Because Mars is small, cold, and lacks a magnetic field, it has retained only a sparse atmosphere. The surface air pressure of 0.6 kilopascals for Mars is only 0.6% of Earth's 101.3 kilopescales. The planet has probably lost at least 80 to 85% of its original water supply to space. However, the planet has retained significant deposits of frozen water and carbon dioxide. If all the frozen CO2 were de-sublimated, the air pressure could climb to 30 kilopascals. This is comparable to the air pressure on the top of Mount Everest.

The composition of Earth's atmosphere is determined by the byproducts of the life that it sustains. Dry air mixture of gases from Earth's atmosphere contains 78.08% nitrogen, 20.95% oxygen, 0.93% argon, 0.04% carbon dioxide, and traces of hydrogen, helium, and other noble gases by volume. But generally a variable amount of water vapor is also present, on average about 1% at sea level. Earth's persistent magnetosphere acts as the shield against atmospheric scavenging by the solar wind as it fends off the incoming plasma at a distance of about 10 Earth radii. The low temperatures and higher escape velocities of the solar system's giant planets,

Jupiter, Saturn, Uranus, and Neptune, allow them to readily retain gases with low molecular masses. These planets have reducing atmospheres of hydrogen and helium and trace amounts of other elements and more complex compounds. Unlike the terrestrial planets, The gas giants lack a well-defined surface. Instead, the atmosphere is maintained in hydrostatic equilibrium by intense pressure deep in the body.

The dynamic weather on these bodies only occurs in a relatively thin surface layer. Two satellites of the outer planets possess significant atmospheres. Titan, a moon of Saturn, and Triton, a moon of Neptune, have atmospheres mainly of nitrogen. When in the part of its orbit closest to the sun, Pluto has an atmosphere of nitrogen and methane similar to Tritons, but these gases are frozen when it's farther from the sun. Other bodies within the solar system have extremely thin atmospheres not in equilibrium.

These include the moon, sodium gas, noble gases, hydrogen, Mercury, sodium gas, colistow, carbon dioxide and oxygen, Europa, oxygen, I.O., sulfur dioxide, and Enceladus, water vapor. Planetary objects surround distant stars known as exoplanets span a more diverse range of physical properties than is found in the solar system. These targets provide an opportunity to study atmospheres around a broad span of objects and conditions. However, observations of these targets requires much more sensitive instrumentation. The methods used to analyze these remote atmospheres are transit spectroscopy, high-resolution Doppler spectroscopy, and direct imaging. Transit spectroscopy uses the transit of an exoplanet across its host star to detect its atmosphere.

By comparing the radius at different wavelengths, the presence of specific components can be detected. The first such detection was in 2002, when sodium was detected in the atmosphere of HD 209458B, A gas giant was a close orbit around a star in the constellation Pegasus. Its atmosphere is heated to temperatures over 1,000 Kelvin and is steadily escaping into space. Hydrogen, oxygen, and carbon have been detected in the planet's inflated atmosphere by Hubble observations. Since 2002, potassium has been detected in the atmosphere of XO2NB. and both sodium and potassium in HD189-733B's atmosphere.

Many of the discovered super-Earths have orbits close enough to their host star, but their surfaces are expected to be magma oceans. The secondary atmospheres of these lava planets most likely consist of materials that have been vaporized from the magma, such as sodium, potassium, oxygen, and silicon oxide. An atmosphere and hydrostatic equilibrium consists of a balance between the air pressure created by the motions of the molecules and the restraining force of gravity that prevents the molecules from escaping.

The pressure decreases in altitude, producing a pressure-gradient force. Atmospheric pressure is the force per unit area perpendicular to a unit area of planetary surface, as determined by the weight of the vertical column of atmospheric gases. In said atmospheric model, the atmospheric pressure, the weight of the mass of the gas, decreases at high altitude because of the diminishing mass of the gas above the point of barometric measurement. Air pressure varies by place in time due to meteorological conditions and atmospheric waves. Units of air pressure are based upon the standard atmosphere, ATM, which is 101,325 Pascal's, equivalent to 760 Tor, or 14.6.66 PSI.

For an ideal gas atmosphere, the weight at which the atmospheric pressure declines by a factor of E, the base of the natural logarithm, is called the scale height, H. For an atmosphere of uniform temperature, the scale height is proportional to the atmospheric temperature and is inversely proportional to the product of the mean molecular mass of dry air. and the local acceleration of gravity at the point of barometric measurement. The temperature of the atmosphere is determined by an energy budget, which balances the heating from the incoming solar energy against the heat radiated back into space. The incoming energy is determined by the distance from the sun, and the energy reflected back out by the planetary albedo. When a planet is in radiative equilibrium, it has a planetary equilibrium,

it has a planetary equilibrium temperature. This differs from the global mean temperature, which may be warmer than the equilibrium temperature due to the atmospheric greenhouse effect. For example, Venus has a surface temperature of almost 460 degrees Celsius compared to an equilibrium temperature of negative 40 degrees Celsius. Planetary atmospheres are composed of layers

with different properties. such as specific gases compounds, temperature gradients, and pressure. For Earth, Mars, and Venus, the lowest level of the atmosphere is the troposphere, or most of the planet's clouds and weather are found. This extends from the group up to 65 kilometers on Venus, 40 kilometers on Mars, and 17 kilometers on Earth. The troposphere contains the bulk of the atmosphere,

possessing 80% and 98% of the total atmospheric mass. Temperature varies by altitude according to the lapse rate, as thermal energy from the ground is transported upward via convection. Infrared radiation becomes trapped by molecules of gas and water vapor. For the Earth, the next line is. This layer is the stratosphere, which is a region of temperature increasing with altitude, creating a temperature inversion. This region contains the UV-absorbing ozone layer, at an altitude between 15 kilometers and

35 kilometers, which is responsible for the temperature rise. Energy transport in this region occurs through radiation processes. blocking an oxygenated atmosphere to generate a significant layer of ozone, neither Mars nor Venus have a stratosphere. Above the troposphere stratosphere, the next layer of the atmosphere is termed a mesosphere. In this region, the water vapor and carbon dioxide serves as a heat sinks that radiates energy in the infrared. As a result, the temperature of the mesosphere decreases with altitude. altitude, reaching the coldest layer of the atmosphere at the top. Both Venus and Mars have an altitude range in the Mesosphere, where the temperature is nearly

isothermal. For Mars, this is above 120 kilometers, while for Venus it is between 63 and 75 kilometers altitude. In the lower regions of the atmosphere, turbulent mixing causes the atmospheric constituents to be evenly distributed. Above a transition layer called the homopause, molecular diffusion dominates. This results in diffuse separation of the constituents by atomic weight. That is, lower mass components diffuse upward, leaving higher mass molecules near the bottom.

The homopause is at an altitude of 100 to 110 kilometers for the years. 115 to 130 kilometers for Mars and 135 to 150 kilometers for Venus. Beyond the mesosphere is a region of the atmosphere called the thermosphere that absorbs x-rays and extreme UV from the Sun, causing temperature to rise with altitude. The thermal properties of this layer varied daily and with solar activity cycles. The atmospheric region from the ground through the thermosphere is referred to as the barrosphere, since the barometric law holds around.

The outermost layer of a planetary atmosphere is termed the exosphere. Here the air pressure is so low at this altitude that the distance traveled between molecule collisions, the mean free path, is greater than the atmospheric scale height. In this region, lower mass components with a thermal velocity, exceeding the escape velocity, can escape into space. For the Earth, the exosphere is at an altitude of 500 kilometers, while it is around 210 kilometers for Venus and Mars. On Earth, the exosphere extends to roughly 10,000 kilometers, where it interacts with the

magnetosphere of Earth. All three planets have an ionosphere, which is an ionized region of the upper atmosphere. The ionosphere for Mars and Venus are closer to the surface and less dense than on the Earth. The density of the Earth's ionosphere is greater at short distances from the planetary surface in the daytime and decreases as the ionosphere rises at night time, thereby allowing a greater range of radio frequencies to travel greater distances. Gas giants are primarily composed of hydrogen and helium with traces of other elements, giving the planets a low bulk density. Many of the molecules observed in the outer atmosphere are hydrides, and most of these, with the exception of H2O and H2S,

are photochemically destroyed by solar UV in the stratosphere of Jupiter and Saturn. These compounds get recreated by thermochemical reactions within the hotter, lower regions of the atmosphere. Complex organic compounds are recycled back to methane by the highly reducing atmosphere. The high gravity of these planets combined with their distance from the sun means that mass loss from their exosphires is negligible, so they form closed systems. A common feature of the gas giant planets are cloud layers that form where the combination of temperature and pressure are appropriate

for condensing a particular volatile. For Jupiter and Saturn, the uttermost cloud layer consists of ice particles of ammonia, NH3. with an underlying layer of ammonium hydrosulfide, NH4SH, then a deep layer of water clouds, H2O. For Uranus and Neptune, the top layer is a methane-CH4 layer of ice particles, followed by the same cloud layers as Jupiter and Saturn. One difference for Uranus and Neptune is a hydrogen sulfide H2S mixes at the same level as the condensensens. pneumonia. These cloud layers are optically thick, absorbing light at all wavelengths. The result is a shallower scale hide for the outer atmosphere. All four gas giants experience

lightning activity in the water clouds, and this is generally much more powerful than terrestrial lightning. Lightning has been observed on Jupiter, but has not been optically detected on Saturn, Uranus or Neptune, most likely because of their depth. All of the gas giants have internal heat sources and radiate more heat than they receive from the sun. Models for the interiors of Jupiter and Saturn suggest that at a certain depth, the hydrogen undergoes a phase change to a metallic hydrogen fluid

mixed with ice. There is probably a diffuse of solid core of more massive elements. For Uranus and Neptune, there is no metallic hydrogen. Instead, there are interior layers of ice, placing these worlds in the subcategory of ice giants. As sufficient depths, the ice may transition to a supercritical fluid. Within the solar system, gas giant planets formed beyond the frost line,

where the temperature from the young sun was low enough for varieg. volatiles to condense into solid grains. In some star systems, dynamic processes in the protoplanetary disk can cause a gas giant to migrate much closer to the central star, creating a hot Jupiter. A prototype example is 51 Pegas I.B. Through gravitational interaction, the orbit of the planet becomes circularized, and it is tidily locked into a synchronous, rotation with one side constantly facing the star. The heated side becomes swollen, and high-velocity winds distribute the thermal energy around the planet. The atmosphere may eventually be stripped away by the star's gravity, leaving behind a super-Earth. At the upper mass extreme of gas giants

is a class of objects known as brown dwarfs. There is no universal consensus. on how to distinguish a brown dwarf from a gas giant. Although a commonly used criteria is the ability to fuse deuterium at around 13 times the mass of Jupiter. Once the initial deuterium burning phase of a brown dwarf is concluded, the internal store of heat gradually makes its way to the surface, then is radiated away over time. Convection occurs around the core,

and possibly at the surface, surface if the brown dwarf is receiving energy from a nearby star. Radiative energy transfer occurs throughout the remainder of the brown dwarf. Chemistry can occur throughout the atmosphere, which depending on the chemical species, can change the opacity to radiative energy transfer. As with gas giants, in the cooler outer regions of a brown dwarf, some molecules can condense to form clouds. The circulation of the atmosphere occurs due to thermal differences when convection becomes a more efficient

transporter of heat than thermal radiation. On planets where the primary heat source is solar radiation, excess heat in the tropics is transported to higher latitudes. When a planet generates a significant amount of heat internally, such as is the case for Jupiter, convection in the atmosphere can transport thermal energy from the higher temperature interior up to the surface. The thermally driven meridional circulation of Earths, Mars, and Venus are dominated by the Hadley cell. This is created by rising air in the warmest region of the planet, accompanied by descending air when it is cooler. However, there are significant differences in the circulation patterns between the three planets.

For Venus, the lower atmosphere has two symmetrical equator to the near-pole circulation cells, with a higher altitude subsolar to anti-solar circulation cell. On Earth, Hadley cells exist on each side of the equator, but these vary seasonally due to the planet. planet's obliquity. Mars is similar to the Earth in this respect, but it displays greater seasonality due to its thinner atmosphere. It has two Hadley cells during equinox, but a single cell at solstice. The Earth has multiple counter-rotating convection cells, with the Hadley cell on either side of the equator, an intermediate feral cell along the mid-latitude.

and polar cells at each pole. The planet's rotation induces a coriolis force that creates a curvature in the north-south convection flow. As air moves toward a pole, the latitudinal flow remains steady, but the distance needed to encircle the planet grows shorter, creating a curved pass along the surface. These flows create the prevailing winds along the planet's surface.

Near the equator, the air flow creates the trade winds, which flow from east to west. At the mid-latitudes, the Westerlies brings the air flow from the west into the United States and Europe. Finally, the polar easterlies moves polar air from east to west. Both Jupiter and Saturn display banded cloud formations. These are associated with alternating jets known as zonal flows that follow latitudinal lines. The bands alternate in direction, with the equatorial jet moving eastward at 150 kilometers per second on Jupiter and 300 kilometers per second on Saturn.

It remains unclear whether these flows occur in the shallow layers around the clouds, extend much deeper into the atmosphere. Observations of Neptune show a similar zonal flow structure. This planet displays the largest range of differential rotation in the solar system. Surface gravity differs significantly among the planets. For example, the large gravitational force of the giant planet Jupiter retains light gases such as hydrogen and helium that escape from a large gravitational force of the giant planet Jupiter retains light gases, such as hydrogen and helium, it escaped from objects with lower gravity. Secondly, the distance from the sun determines the energy available to heat atmospheric gas to the point where some fraction of its molecule's thermal motion exceed the planet's escape

velocity, allowing those to escape a planet's gravitational grasp. Thus, distant and cold Titan, Triton and Pluto are able to retain components of their original atmospheres, despite the relatively low gravities. Since a collection of gas molecules may be moving at a wide range of velocities, there will always be some fast enough to produce a slow leakage of gas into space. Lighter molecules move faster than heavier ones, with the same thermokinetic energy, and so gases of low molecular weight are lost more rapidly, than those of high molecular weight.

It is thought that Venus and Mars may have lost much of their water when after being photo-dissociated into hydrogen and oxygen by solar ultraviolet radiation, the hydrogen escaped. Earth's magnetic field helps to prevent this, as normally the solar wind would greatly enhance the escape of hydrogen. However, over the past 3 billion years, Earth may have lost gases through the magnetic polar regions due to auroral activity, including a net 2% of its atmospheric oxygen. The net effect, taking the most important escape processes into account, is that an intrinsic magnetic field does not protect a planet from atmospheric escape, and that for some magnetizations, the present. presence of a magnetic field works to increase the escape rate.

Planets around small M-type main sequence stars may be particularly prone to atmospheric loss. The star will spend an extended period as a superluminous pre-main sequence star, then experience high levels of activity. The strong stellar magnetic field will tend to reduce the size of planetary magnetospheres, leading to greater erosion from the stellar wind.

Planets around older M-type stars may become tidily locked in synchronous orbit, leading to the atmosphere being permanently frozen on the dark face. Other mechanisms that can cause atmosphere depletion or solar wind-induced sputtering, impact erosion, weathering, and sequestration, sometimes referred to as freezing out, into the regalus and polar caps. An extreme example of the latter is a comet, which is a small body that forms beyond the frost line

and the protoplanetary disk. These objects contain many types of frozen volatiles, including water, carbon dioxide, ammonia, and formaldehyde. As these objects approach the sun, the thermal radiation causes the volatiles to sublimate, creating a diffuse, dusty atmosphere around the comet, the coma. However, the gravitational potential of the comet is insufficient to retain this atmosphere. The solar system contains a large number of bodies that are now practically airless,

such as Mercury and the Moon. These objects have only an exosphere layer with particles that are essentially collisionless. In this environment, atoms and molecules are released from the surface by various means, including particle sputtering and micro-mediorite impact. When the release velocity of these particles exceed the escape velocity, they are lost to space. Higher mass particles have a greater chance to be returned to the surface,

which creates a chemical alteration of the surface over time.