Astrophysics (Index)About

energy

(physical state needed to do something)

The physics concept of energy is a type of measurable quality of an object or system that is needed to make something happen. The physics concept of energy is something that is permanent (conserved): its loss is merely its transfer it to something else or its transformation into some other kind of energy. For example, to lift an object of a certain mass from the ground to a certain height above ground requires a certain amount of energy. (The same amount of energy remains; afterward, the energy that lifted it remains inherent in the separation of the mass from the ground.) Among the forms of energy:

The physics term work is such transformation of energy, which is quantified by units of energy, i.e., the amount transformed. Energy as we know it everyday generally came from the Sun in the form of electromagnetic radiation (EMR), generally converted by plants into chemical energy, and by its heating effect on weather and climate. Numerous units are used to quantify energy in science and everyday life. Some of them:

joule SI unit
erg 10-7 joules
Planck energy a "natural unit", 1.9561 × 109 joules
electron volt 1.602176634 × 10-19 joule
Rydberg unit 2.1798723611035 × 10-18 joules
foe 1051 ergs or 1044 joules
calorie 4.184 joules
kilocalorie what is called a "calorie" regarding food, 4184 joules
kilowatt-hour 36×105 joules
BTU definition varies somewhat: one definition is 1055 joules
foot-pound 1.3558179483314004 joules

For context, a joule is very roughly the energy to lift (in Earth surface gravity) a pound weight 9 inches, or a kg weight 10 cm. Because of the relation between energy and mass (e=mc²), any unit of energy can be used as a unit of mass and vice-versa. Electron volts are perhaps used as measures of mass as much as they are of energy. The physics term for the rate at which energy is transformed (work is done) is power. Luminosity is basically power, but the term is used for measures of EMR emitted by a body, and for the extraction of nuclear energy used to produce that emission. Some units of power:

watt a joule per second
solar luminosity luminosity of the Sun, 3.828×1026 watts
horsepower definition varies somewhat: one definition is 730 watts

(physics)
Further reading:
https://en.wikipedia.org/wiki/Energy
https://en.wikipedia.org/wiki/Work_(physics)
https://en.wikipedia.org/wiki/Power_(physics)
https://en.wiktionary.org/wiki/energy
http://hyperphysics.phy-astr.gsu.edu/hbase/work.html
http://hyperphysics.phy-astr.gsu.edu/hbase/enecon.html
https://physics.info/energy/
https://www.britannica.com/science/energy

Referenced by pages:
AB system
absorption line
accretion
ACIS
Aditya-L1
Advanced Composition Explorer (ACE)
advection dominated accretion flow (ADAF)
air shower
airmass
alpha disk
AMS-02
anisotropy
anomalous cosmic rays (ACR)
anomalous X-ray pulsar (AXP)
antimatter
Ariel 5
astrophysical neutrino
asymptotic giant branch (AGB)
AT2018cow
ATHENA
atmosphere formation
atmospheric escape
atomic excitation
Auger effect
beam
BeppoSAX
binary SMBH (BSMBH)
binding energy
black body (BB)
black hole (BH)
black hole merger
black hole thermodynamics
black-body radiation
Blandford-Znajek mechanism (BZ process)
blastwave
Bohr model
bolometer
Boltzmann constant (k)
Boltzmann equation
Borexino
Bose-Einstein condensate (BEC)
Bose-Einstein statistics
bremsstrahlung
carbon dioxide (CO2)
carbon monoxide (CO)
CASA-MIA
CGS
Chandra X-ray Observatory (CXO)
chemical equilibrium (CE)
Cherenkov detector
Cherenkov Telescope Array (CTA)
chirp mass (Mc)
CO ladder
collisional broadening
Compton reflection
Compton scattering
Compton telescope
conservation law
continuous absorption
continuum
convection
convection zone
cooling flow
cooling function
core collapse
cosmic neutrino background (CNB)
cosmic rays (CR)
critical density (ρc)
Cryogenic Dark Matter Search (CDMS)
cyclotron radiation emission spectroscopy (CRES)
dark energy (Λ)
de Broglie wavelength
decoupling
degeneracy
degeneracy weight
density parameter
diffusion damping
dynamo
earthshine
Eddington approximation
electric dipole radiation
electromagnetic spectrum
electron (e-)
electron capture supernova
electron degeneracy
electron orbital
electron pressure
electron screening
electron shell
electron volt (eV)
emission coefficient (j)
emission line
endothermic reaction
energetic neutral atom (ENA)
energy density
entropy (S)
equation of radiative transfer (RTE)
erg
EUSO-SPB
evaporation
false vacuum
fast radio burst (FRB)
Fermi bubbles
Fermi sea
Fermi-Dirac statistics
filter
final parsec problem
fine structure
fluorescence
flux
Fly's Eye
foe
forbidden line
frequency (ν)
fusion
galaxy formation
galaxy SED
gamma-ray burst (GRB)
general relativity (GR)
Geroch-Bekenstein engine
giant star
globular cluster (GC)
GRAPES-3
gravitational collapse
gravitational potential (Φ)
gravitational potential well
gravitational wave (GW)
gravitationally bound
GRB-supernova (GRB-SN)
greenhouse effect
ground state
GW170817
GZK limit
Hamiltonian
HEAO-1
HEAO-2
HEASARC
HEGRA
helium 1083 nm line
helium rain
High Energy Stereoscopic System (HESS)
High Energy Transient Explorer (HETE)
high-energy astrophysics (HEA)
HII region (HII)
Hill stability
homologous collapse
hydrogen (H)
hyperfine structure
hyperon
HZE ion
IceCube
illumination
IMAGE­
IMAP
inflated radii
initial fluctuations
insolation
instability strip
intensity
International Cometary Explorer (ICE)
Interstellar Boundary Explorer (IBEX)
ionization potential
ionized carbon fine structure line ([CII])
ionized hydrogen (HII)
ionizing radiation
iron peak
irradiance
isothermal core
isotropy
Jeans length
joule (J)
K-line
kappa mechanism (κ-mechanism)
KATRIN
Kelvin-Helmholtz mechanism (KH mechanism)
Kelvin-Helmholtz timescale (KH timescale)
Kepler Telescope
kilonova (KN)
kinetic energy (KE)
KM3-230213A
KM3NeT (Cubic Kilometre Neutrino Telescope)
Kolmogorov spectrum
Kvant 1
Landau damping
Large Hadron Collider (LHC)
light cone
line blanketing
line broadening
luminosity (L)
Lyman break (LB)
Lyman-Werner photon
magma ocean
magnetar
magnetic dipole braking
magnetic dipole radiation
magnetic energy spectrum
maser
mass
mass shell
memorandum of understanding (MOU)
Messier 77 (M77)
metastable
microcalorimeter
muon (μ)
Navier-Stokes equations (NS equations)
neutrino (ν)
neutrinoless double beta decay
neutron scattering
neutron star (NS)
neutron star merger
neutron-star black-hole merger (NSBH merger)
nuclear energy generation rate (ε)
nuclear statistical equilibrium (NSE)
nuclide
NuSTAR
Oh-My-God Particle
one dimensional climate model
OSO 8
pair production
pair telescope
partial ionization zone
particle
partition function (Z)
Penrose Compton scattering (PCS)
Penrose process
phase transition
photochemistry
photodissociation
photoevaporation
photoionization
photomultiplier tube (PMT)
photon
photon energy
PICO experiment (PICO)
Pierre Auger Observatory (PAO)
Planck constant (h)
Planck units
planet structure
plasmon
post-AGB star (pAGB)
potential energy (PE)
Poynting vector (S)
pre-main-sequence star (PMS)
proportional counter
protogalaxy
pulsating star
Q factor
quantum
quantum fluctuations
quantum mechanics (QM)
quantum number
radiance
radiant flux
radiation belt
radiation pressure
radiation zone
radiative flux
radiative transfer (RT)
radiative transfer code (RT code)
radioactive heating
radioactivity
radiolysis
recombination
red giant
red-giant branch (RGB)
reheating
relativistic energy
RMS
RXTE
Rydberg constant (RH)
Rydberg unit
Sachs-Wolfe effect (SWE)
Saha equation
SAMPEX
Satech-01
scattering
Schönberg-Chandrasekhar limit
scintillator
SELENE
self-absorption
shock wave
SI
Small Astronomy Satellite 3 (SAS 3)
SMBH formation
solar constant
solar neutrino
solar neutrino unit (SNU)
specific intensity
spectral class
spectral density
spectral energy distribution (SED)
spectral index (α)
spectral line
spectral line designation
spectral line energy distribution (SLED)
spectral power distribution (SPD)
spectral temperature
spin (ms)
spin-down luminosity
standard candle
standard model of a flare
star
star formation feedback
starburst galaxy
state of excitation
Stefan-Boltzmann constant (σ)
stellar flare
stellar model atmosphere
stellar structure
stimulated emission
STMAG system
Strömgren sphere
Sunyaev-Zel'dovich effect (SZ effect)
superluminous supernova (SLSN)
supermassive black hole (SMBH)
supernova (SN)
superradiance
supershell
suprathermal
Swordy plot
synchrotron self-Compton (SSC)
T-Tauri star (TTS)
TAMBO
tau (τ)
Telescope Array Project (TA)
temperature
thermodynamics
Thomson scattering
three dimensional model
tidal force
tidal Q
timescale (t)
tired light
trans-iron element
Trinity
ultra-high-energy gamma rays (UHEGR)
Ulysses
Urca process
valley of beta stability
vegetation red edge (VRE)
very-high-energy gamma rays (VHEGR)
VHE
viscous dissipation
Voyager
watt (W)
wave-particle duality
wavelength (λ)
white dwarf (WD)
Wien approximation
Wien's displacement law
Zeeman effect
Zeeman-Doppler imaging (ZDI)

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