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Condition in thermodynamics
Radiative equilibrium is the condition where the total thermal radiation leaving an object is equal to the total thermal radiation entering it. It is
Radiative_equilibrium
Temperature of a planet when approximated as radiating as a black body
The planetary equilibrium temperature is a theoretical temperature that a planet would be if it were in radiative equilibrium, typically under the assumption
Planetary equilibrium temperature
Planetary_equilibrium_temperature
Meteorological concept
radiative-convective equilibrium (RCE) is a concept for the radiative balance of the atmosphere. It describes the balance between the net radiative longwave
Radiative-convective equilibrium
Radiative-convective_equilibrium
Concept for changes to the energy flows through a planetary atmosphere
radiative-dynamical equilibrium." Instantaneous radiative forcing: "if no change in stratospheric temperature is accounted for". Effective radiative forcing:
Radiative_forcing
State of no net thermal energy flow between two connected systems
until thermal equilibrium is reached and then they will have the same temperature.[citation needed] One form of thermal equilibrium is radiative exchange equilibrium
Thermal_equilibrium
Energy transfer in the form of electromagnetic radiation
scattering processes. The equation of radiative transfer describes these interactions mathematically. Equations of radiative transfer have application in a wide
Radiative_transfer
Physical systems that don't interact with other parts of the universe
example imagined by Planck. He was considering the internal thermal radiative equilibrium of a thermodynamic system in a cavity initially devoid of substance
Isolated_system
Idealised cavity in radiative equilibrium
space", "empty room", or "cavity") is a cavity whose walls are in radiative equilibrium with the radiant energy within the cavity. First proposed by Gustav
Hohlraum
Atmospheric heat retention
energy flows reduce radiative surface cooling (net upward radiative energy flow). Latent heat transport and thermals provide non-radiative surface cooling
Greenhouse_effect
Branch of thermodynamics
in radiative equilibrium in a cavity at the temperature of the matter of the 'cell'. Then it strictly obeys Kirchhoff's law of equality of radiative emissivity
Non-equilibrium thermodynamics
Non-equilibrium_thermodynamics
Climatic effect causing a planet's atmosphere to trap heat and prevent cooling
considers a grey stratosphere in radiative equilibrium. A grey stratosphere (or atmosphere) is an approach to modeling radiative transfer that does not take
Runaway_greenhouse_effect
Electromagnetic radiation generated by the thermal motion of particles
colleague of Pictet, introduced the concept of radiative equilibrium, wherein all objects both radiate and absorb heat. When an object is cooler than
Thermal_radiation
Phenomenon in solid-state physics of semiconductors
surface recombination. These decay channels can be separated into radiative and non-radiative. The latter occurs when the excess energy is converted into heat
Carrier generation and recombination
Carrier_generation_and_recombination
Concept for energy flows to and from Earth
incoming and outgoing energy fluxes are in balance, Earth is in radiative equilibrium and the climate system will be relatively stable. Global warming
Earth's_energy_budget
Mechanical equilibrium, the state in which the sum of the forces, and torque, on each particle of the system is zero Radiative equilibrium, the state
List_of_types_of_equilibrium
Chemical equilibrium of a reversible reaction
{k_{f}}{k_{b}}}\right)_{2}\times \cdots } Chemical equilibrium Equilibrium chemistry Mechanical equilibrium Radiative equilibrium Atkins, P.W.; de Paula, J. (2006). Physical
Dynamic_equilibrium
Physical quantity of hot and cold
Milne, E. A. (1928). "The effect of collisions on monochromatic radiative equilibrium". Monthly Notices of the Royal Astronomical Society. 88 (6): 493
Temperature
Brightest star in the constellation Lyra
reaction within the core region. The overlying atmosphere is in radiative equilibrium. This is in contrast to the Sun, which has a radiation zone centered
Vega
Path taken by pre-main-sequence stars in the Hertzsprung–Russell diagram
the 1950s showed that the pre-main-sequence star can remain in radiative equilibrium throughout some period of its contraction to the main sequence.
Henyey_track
State of thermodynamic systems where no net flow of matter or energy occurs
thermodynamic equilibrium are simultaneously in mutual thermal, mechanical, chemical, and radiative equilibria. Systems can be in one kind of mutual equilibrium, while
Thermodynamic_equilibrium
Concept in climate science
measure of how much temperature change a given amount of radiative forcing will cause. Radiative forcings are generally quantified as Watts per square meter
Climate_sensitivity
Model of the potential energy of a diatomic molecule
empirical values for physical parameters such as the dissociation energy, equilibrium bond length, and long-range constants. Cases of particular note include:
Morse/Long-range_potential
German physicist (1873–1916)
concept of radiative equilibrium between convection inside the Sun and thermal radiation at the surface. He developed an equation for radiative transfer
Karl_Schwarzschild
Region of a star
A radiative zone is a layer of a star's interior where energy is primarily transported toward the exterior by means of radiative diffusion and thermal
Radiative_zone
Layer of gases surrounding an astronomical body held by gravity
out by the planetary albedo. When a planet is in radiative equilibrium, it has a planetary equilibrium temperature. This differs from the global mean temperature
Atmosphere
1967 influential scientific article on climate
Nadir; Held, Isaac; Ramaswamy, V. (November 2022). "Manabe's Radiative–Convective Equilibrium". Bulletin of the American Meteorological Society. 103 (11):
Thermal Equilibrium of the Atmosphere with a Given Distribution of Relative Humidity
Thermal_Equilibrium_of_the_Atmosphere_with_a_Given_Distribution_of_Relative_Humidity
Concentration of water vapour in the air
This is the biggest non-radiative cooling effect at the surface. It compensates for roughly 70% of the average net radiative warming at the surface. Second
Humidity
Capacity of an object to radiate electromagnetic energy
used in single-use reentry capsules. Passive daytime radiative cooling Daytime passive radiative coolers use the extremely cold temperature of outer space
Emissivity
Subfield of astronomy
233. JSTOR 6491. PMID 17747682. Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Astrophysics
Quantitative methods used to simulate climate
simplifications of the atmospheric radiative transfer on the basis of atmospheric radiative transfer codes, and cloud microphysics. Radiative parametrizations are important
Climate_model
Idealized physical body that absorbs all incident electromagnetic radiation
body in thermal equilibrium has two main properties: It is an ideal emitter: at every frequency, it emits as much or more thermal radiative energy as any
Black_body
Energy transfer mechanism which enables planetary cooling
space, i.e., the only way the planet cools itself. Radiative heating from absorbed sunlight, and radiative cooling to space via OLR power the heat engine
Outgoing_longwave_radiation
Law of wavelength-specific emission and absorption
wavelength-specific radiative emission and absorption by a material body in thermodynamic equilibrium, including radiative exchange equilibrium. It is a special
Kirchhoff's law of thermal radiation
Kirchhoff's_law_of_thermal_radiation
Topics referred to by the same term
temperature Earth's Energy Imbalance, a measurable change in the planet's radiative equilibrium which quantifies its heating (or cooling) rate Global Warming (Pitbull
Global warming (disambiguation)
Global_warming_(disambiguation)
Mathematical estimate of planetary temperatures
long-term, the planet's thermal inertia is surmounted and a new radiative equilibrium is reached when all energy arriving on the planet is leaving again
Idealized_greenhouse_model
Thermal electromagnetic radiation
absolutely stable distribution of radiative intensity that can persist in thermodynamic equilibrium inside a cavity. In equilibrium, for each frequency, the intensity
Black-body_radiation
plane-parallel atmosphere geometry. The atmosphere is in a thermal radiative equilibrium. This set of assumptions leads directly to the mean intensity and
Grey_atmosphere
Optical effect seen in stars
Press, New York. Bibcode:1966gtsc.book.....B. Milne, E.A. (1921). "Radiative Equilibrium in the Outer Layers of a Star: the Temperature Distribution and
Limb_darkening
Reaction that combines atomic nuclei
2022. Retrieved 25 March 2020. Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Nuclear_fusion
Spectral density of light emitted by a black body
conductive heat transfer and radiative heat transfer. Radiative heat transfer can be filtered to pass only a definite band of radiative frequencies. It is generally
Planck's_law
series of 26 papers in The Astrophysical Journal titled On the Radiative Equilibrium of a Stellar Atmosphere from 1944 to 1948. In the 10th paper, he
Chandrasekhar_polarization
Field of physics that studies atomic interactions
Bibcode:1920SciMo..11..297E. JSTOR 6491. Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Nuclear_physics
1957 paper on stellar origins of elements
1920), pp. 297–303 JSTOR 6491 Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
B2FH_paper
British astrophysicist (1882–1944)
1920), pp. 297–303 JSTOR 6491 Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Arthur_Eddington
Scatter plot of stars showing the relationship of luminosity to stellar classification
233. JSTOR 6491. PMID 17747682. Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Hertzsprung–Russell_diagram
Luminosity–temperature relationship in stars
between 0.5 and 3 M☉ develop a radiative zone prior to reaching the main sequence. Stars between 3 and 10 M☉ are fully radiative at the beginning of the pre-main-sequence
Hayashi_track
English astronomer
independently of him. He constructed a model of star with a convective core and radiative envelope, named the Cowling model by Chandrasekhar. He also studied magnetic
Thomas_Cowling
Passage of an object through the gases of an atmosphere from outer space
and radiative heating increase, but at different rates. At very high speeds, radiative heating will dominate the convective heat fluxes, as radiative heating
Atmospheric_entry
Formula for radiative heat transfer
used to calculate radiative transfer (energy transfer via electromagnetic radiation) through a medium in local thermodynamic equilibrium that both absorbs
Schwarzschild's equation for radiative transfer
Schwarzschild's_equation_for_radiative_transfer
Physical law for entropy and heat
cannot decrease, as they always tend toward a state of thermodynamic equilibrium where the entropy is highest at the given internal energy. An increase
Second_law_of_thermodynamics
Swiss physicist (1751–1839)
physico-mecaniques sur la chaleur, and Essai sur le calorique rayonnant. Radiative equilibrium Prevost, Pierre (April 1791). "Mémoire sur l'équilibre du feu".
Pierre_Prevost_(physicist)
Soviet Armenian astrophysicist (1908–1996)
1978. His undergraduate thesis was "devoted to a study of radiative transfer radiative equilibrium." He completed his postgraduate studies at the Pulkovo
Viktor_Ambartsumian
Possible fate of the universe
language of physics, this is when the universe reaches thermodynamic equilibrium. If the curvature of the universe is hyperbolic or flat, or if dark energy
Heat_death_of_the_universe
Concept in astrophysics regarding radiation transparency
frequency ( κ ν = κ {\displaystyle \kappa _{\nu }=\kappa } ). Under radiative equilibrium, the local physical temperature T {\displaystyle T} at a given optical
Optical_depth_(astrophysics)
Tropical atmospheric circulation feature
difference in potential temperature between the equator and the pole in radiative equilibrium, H t {\displaystyle H_{t}} is the height of the tropopause, Ω {\displaystyle
Hadley_cell
Physics of heat, work, and temperature
thermodynamics which primarily studies systems in thermodynamic equilibrium. Non-equilibrium thermodynamics is often treated as an extension of the classical
Thermodynamics
Property of an object or substance that is impervious to light
electromagnetic or other kinds of radiation, especially visible light. In radiative transfer, it describes the absorption and scattering of radiation in a
Opacity
James Mercer, proved Mercer's theorem. Edward Milne, the study of radiative equilibrium, the structure of stellar atmospheres, theory of relativity and
List of University of Manchester people
List_of_University_of_Manchester_people
Heat-trapping gas in an atmosphere
radiation with the surface and limit radiative heat flow away from it, which reduces the overall rate of upward radiative heat transfer. The increased concentration
Greenhouse_gas
Vertical rate of change of temperature in atmosphere
and all cooling is radiative. Within the troposphere, the lapse rate is essentially the consequence of a balance between (a) radiative cooling of the air
Lapse_rate
1920), pp. 297–303 JSTOR 6491 Eddington, A. S. (1916). "On the radiative equilibrium of the stars". Monthly Notices of the Royal Astronomical Society
Timeline of gravitational physics and relativity
Timeline_of_gravitational_physics_and_relativity
Model in computational physics
the energy is distributed before the radiative process sets in. In a coronal picture the timescale of the radiative process is small compared to the collisions
Plasma_modeling
Astrophysics concept
arise in accretion disks. Zeipel, Edvard Hugo von (1924). "The radiative equilibrium of a rotating system of gaseous masses". Monthly Notices of the
Von_Zeipel_theorem
Structure of stars
refer to Radiative transfer. Different layers of the stars transport heat up and outwards in different ways, primarily convection and radiative transfer
Stellar_structure
inter-comparison of far-infrared line-by-line radiative transfer models", Journal of Quantitative Spectroscopy and Radiative Transfer, v. 90, iss. 3–4, p. 323-341
FUTBOLIN
trapping Radiational cooling Radiative cooling Radiative equilibrium Radiative heat transfer Radiative process Radiative transfer Radio-frequency induction
Index_of_physics_articles_(R)
Cosmological epoch c. 370,000 years after the Big Bang
photons on the 2s–1s transition. This requires solving a time-dependent radiative transfer equation. In addition, one needs to account for higher-order
Recombination_(cosmology)
Feedback between climate change and the effect of clouds on radiation
conditions, is described as the cloud radiative effect (CRE). This is also sometimes referred to as cloud radiative forcing (CRF). However, since cloud
Cloud_feedback
Indian-American astrophysicist (1910–1995)
stochastic process, radiative transfer, the quantum theory of the hydrogen anion, hydrodynamic and hydromagnetic stability, turbulence, equilibrium and the stability
Subrahmanyan_Chandrasekhar
Red dwarf star in the constellation Cygnus
from the original on 24 August 2017. Retrieved 29 February 2012. "Radiating Equilibrium Temperature". University of Wisconsin Marathon County - Department
Kepler-42
Classical physics prediction that black body radiation grows unbounded with frequency
early 20th century classical physics that an ideal black body at thermal equilibrium would emit an unbounded quantity of energy as wavelength decreased into
Ultraviolet_catastrophe
Super-Earth exoplanet orbiting Kepler-22
atmosphere, its equilibrium temperature, assuming an Earth-like albedo, would be about 279 K (6 °C; 43 °F), slightly higher than Earth's equilibrium temperature
Kepler-22b
Process whose direction can be reversed
the system is in thermodynamic equilibrium, both physical and chemical, and nearly in pressure and temperature equilibrium with its surroundings. This prevents
Reversible process (thermodynamics)
Reversible_process_(thermodynamics)
Topics referred to by the same term
warming Earth's Energy Imbalance, a measurable change in the planet's radiative equilibrium which quantifies its cooling (or heating) rate Generally, cooling
Global cooling (disambiguation)
Global_cooling_(disambiguation)
When a system has more excited-state members than ground-state
1960). A three-level system could also have a radiative transition between level 3 and 2, and a non-radiative transition between 2 and 1. In this case, the
Population_inversion
Star at the centre of the Solar System
200 kg/m3) between 0.25 solar radii and 0.7 radii, the top of the radiative zone. The radiative zone and the convective zone are separated by a transition layer
Sun
Fields Astronomy Workplaces University of Wisconsin–Madison Thesis Radiative equilibrium in an atmosphere in which pure scattering and pure absorption both
Arthur_Code
Type of energy transfer
transfer is entirely due to disordered, microscopic action, including radiative transfer. A mathematical definition can be formulated for small increments
Heat
Stellar phenomenon
Chayer, P.; Fontaine, G.; Wesemael, F. (1995). "Radiative Levitation in Hot White Dwarfs: Equilibrium Theory". The Astrophysical Journal Supplement Series
Radiative_levitation
Quantity in oceanography
determining the sea surface temperature (SST). Since the skin layer is in radiative equilibrium with the atmosphere and the sun, its temperature underlies a daily
Sea_surface_skin_temperature
Compression of an electrically conducting filament by magnetic forces
deuterium pinch. In 1957 Pease and Braginskii independently predicted radiative collapse in a Z-pinch under pressure balance when in hydrogen the current
Pinch_(plasma_physics)
Theory of cloud radiation emission
hypothesis is a physical hypothesis that describes the response of cloud radiative properties to rising surface temperatures. It presumes that the temperature
Fixed anvil temperature hypothesis
Fixed_anvil_temperature_hypothesis
Contraction of an astronomical object due to the influence of its gravity
state of thermodynamic equilibrium. During the star's evolution a star might collapse again and reach several new states of equilibrium. An interstellar cloud
Gravitational_collapse
Thermal engineering discipline concerning transfer of heat in physical systems
dioxide determines the radiative balance of Earth's atmosphere, carbon dioxide removal techniques can be applied to reduce the radiative forcing. Solar radiation
Heat_transfer
Law of thermodynamics establishing the conservation of energy
quantities (increments of internal energy, quantities of emitted or absorbed radiative energy). In 1907, George H. Bryan wrote about systems between which there
First_law_of_thermodynamics
In astronomy and in astrophysics, for radiative losses of the solar corona, it is meant the energy flux radiated from the external atmosphere of the Sun
Coronal_radiative_losses
Model approximation of atmospheric temperature
If the planet's atmosphere is in radiative equilibrium, then the uppermost of these opaque layers should radiate infrared radiation upwards with a flux
Skin_temperature_(atmosphere)
entropy production extremal principles are ideas developed within non-equilibrium thermodynamics that attempt to predict the likely steady states and dynamical
Extremal principles in non-equilibrium thermodynamics
Extremal_principles_in_non-equilibrium_thermodynamics
Concept in physics of one-way time
the probability for initial conditions that produce a radiative wave. In fact, normally a radiative wave increases entropy, while a convergent wave decreases
Arrow_of_time
Physical law on the emissive power of black body
ISBN 0-19-505134-3. Grainger, R. G. (2020). "A Primer on Atmospheric Radiative Transfer: Chapter 3. Radiometric Basics" (PDF). Earth Observation Data
Stefan–Boltzmann_law
Measurement of electromagnetic radiation
passive daytime radiative cooling surface has been estimated at ~100-150 W/m2. Insolation is the primary variable affecting equilibrium temperature in
Solar_irradiance
Central region of the Sun
to current models, random scattering from free electrons in the solar radiative zone (the zone within 75% of the solar radius, where heat transfer is
Solar_core
Speed that exceeds five times the speed of sound (Mach 5 and above)
dissociation and ionization of molecules resulting in convective and radiative heat-flux.[citation needed] Although "subsonic" and "supersonic" usually
Hypersonic_speed
Value in astrophysics
of a star for a given mass. When a star is fully within hydrostatic equilibrium—a condition where the inward force of gravity is matched by the outward
Hayashi_limit
Physical property of matter
such systems have equal temperatures, they are at thermal equilibrium. However, this equilibrium is stable only if the systems have positive heat capacities
Heat_capacity
Supplementary feature of clouds
radiative effects as they evolve. There are a couple of ideas as to how radiation can cause mammatus to form. One is that, because clouds radiatively
Mammatus_cloud
Russian physicist
studying atmospheric circulation. She developed a complete theory of radiative equilibrium in the atmosphere. She examined the wave-like disturbances in the
Ekaterina_Nikitichna_Blinova
Layer of the Sun's atmosphere
ionized, so that it radiates energy very effectively; above, it becomes fully ionized. This has a profound effect on the equilibrium temperature (see below)
Solar_transition_region
Maximum energy available for use
as it achieves equilibrium with its environment. Exergy is also known as "availability". Exergy is non-zero when there is dis-equilibrium between the system
Exergy
Distinctive narrow spectral feature of chemical species
(due to spontaneous radiative decay or the Auger process) with the uncertainty of its energy. Some authors use the term "radiative broadening" to refer
Spectral_line
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RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
RADIATIVE EQUILIBRIUM
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