Faster access than browser!Similarities between Stellar evolution and Supernova
Stellar evolution and Supernova have 48 things in common (in Unionpedia): Accretion (astrophysics), Black hole, Blue supergiant star, Carbon, Carbon-burning process, Chandrasekhar limit, Convection, Degenerate matter, Electron capture, Electron degeneracy pressure, Gravitational collapse, Gravitational energy, Helium, Hydrogen, Infrared, International Astronomical Union, Iron, Kelvin, Kinetic energy, Luminosity, Luminous blue variable, Main sequence, Metallicity, Milky Way, Molecular cloud, Nebula, Neutrino, Neutron, Neutron star, Nova, ..., Nuclear fusion, Nucleosynthesis, Oxygen, Pair-instability supernova, Photodisintegration, Planet, Pulsar, Red giant, Shock wave, Silicon, SN 1987A, Solar System, Supergiant star, Type Ia supernova, Type II supernova, Uranium, White dwarf, Wolf–Rayet star. Expand index (18 more) »
Accretion (astrophysics)
In astrophysics, accretion is the accumulation of particles into a massive object by gravitationally attracting more matter, typically gaseous matter, in an accretion disk.
Accretion (astrophysics) and Stellar evolution · Accretion (astrophysics) and Supernova ·
Black hole
A black hole is a region of spacetime exhibiting such strong gravitational effects that nothing—not even particles and electromagnetic radiation such as light—can escape from inside it.
Black hole and Stellar evolution · Black hole and Supernova ·
Blue supergiant star
Blue supergiant stars are hot luminous stars, referred to scientifically as OB supergiants.
Blue supergiant star and Stellar evolution · Blue supergiant star and Supernova ·
Carbon
Carbon (from carbo "coal") is a chemical element with symbol C and atomic number 6.
Carbon and Stellar evolution · Carbon and Supernova ·
Carbon-burning process
The carbon-burning process or carbon fusion is a set of nuclear fusion reactions that take place in the cores of massive stars (at least 8 \beginsmallmatrixM_\odot\endsmallmatrix at birth) that combines carbon into other elements.
Carbon-burning process and Stellar evolution · Carbon-burning process and Supernova ·
Chandrasekhar limit
The Chandrasekhar limit is the maximum mass of a stable white dwarf star.
Chandrasekhar limit and Stellar evolution · Chandrasekhar limit and Supernova ·
Convection
Convection is the heat transfer due to bulk movement of molecules within fluids such as gases and liquids, including molten rock (rheid).
Convection and Stellar evolution · Convection and Supernova ·
Degenerate matter
Degenerate matter is a highly dense state of matter in which particles must occupy high states of kinetic energy in order to satisfy the Pauli exclusion principle.
Degenerate matter and Stellar evolution · Degenerate matter and Supernova ·
Electron capture
Electron capture (K-electron capture, also K-capture, or L-electron capture, L-capture) is a process in which the proton-rich nucleus of an electrically neutral atom absorbs an inner atomic electron, usually from the K or L electron shell.
Electron capture and Stellar evolution · Electron capture and Supernova ·
Electron degeneracy pressure
Electron degeneracy pressure is a particular manifestation of the more general phenomenon of quantum degeneracy pressure.
Electron degeneracy pressure and Stellar evolution · Electron degeneracy pressure and Supernova ·
Gravitational collapse
Gravitational collapse is the contraction of an astronomical object due to the influence of its own gravity, which tends to draw matter inward toward the center of gravity.
Gravitational collapse and Stellar evolution · Gravitational collapse and Supernova ·
Gravitational energy
Gravitational energy is the potential energy a body with mass has in relation to another massive object due to gravity.
Gravitational energy and Stellar evolution · Gravitational energy and Supernova ·
Helium
Helium (from lit) is a chemical element with symbol He and atomic number 2.
Helium and Stellar evolution · Helium and Supernova ·
Hydrogen
Hydrogen is a chemical element with symbol H and atomic number 1.
Hydrogen and Stellar evolution · Hydrogen and Supernova ·
Infrared
Infrared radiation (IR) is electromagnetic radiation (EMR) with longer wavelengths than those of visible light, and is therefore generally invisible to the human eye (although IR at wavelengths up to 1050 nm from specially pulsed lasers can be seen by humans under certain conditions). It is sometimes called infrared light.
Infrared and Stellar evolution · Infrared and Supernova ·
International Astronomical Union
The International Astronomical Union (IAU; Union astronomique internationale, UAI) is an international association of professional astronomers, at the PhD level and beyond, active in professional research and education in astronomy.
International Astronomical Union and Stellar evolution · International Astronomical Union and Supernova ·
Iron
Iron is a chemical element with symbol Fe (from ferrum) and atomic number 26.
Iron and Stellar evolution · Iron and Supernova ·
Kelvin
The Kelvin scale is an absolute thermodynamic temperature scale using as its null point absolute zero, the temperature at which all thermal motion ceases in the classical description of thermodynamics.
Kelvin and Stellar evolution · Kelvin and Supernova ·
Kinetic energy
In physics, the kinetic energy of an object is the energy that it possesses due to its motion.
Kinetic energy and Stellar evolution · Kinetic energy and Supernova ·
Luminosity
In astronomy, luminosity is the total amount of energy emitted per unit of time by a star, galaxy, or other astronomical object.
Luminosity and Stellar evolution · Luminosity and Supernova ·
Luminous blue variable
Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in both their spectra and brightness.
Luminous blue variable and Stellar evolution · Luminous blue variable and Supernova ·
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appear on plots of stellar color versus brightness.
Main sequence and Stellar evolution · Main sequence and Supernova ·
Metallicity
In astronomy, metallicity is used to describe the abundance of elements present in an object that are heavier than hydrogen or helium.
Metallicity and Stellar evolution · Metallicity and Supernova ·
Milky Way
The Milky Way is the galaxy that contains our Solar System.
Milky Way and Stellar evolution · Milky Way and Supernova ·
Molecular cloud
A molecular cloud, sometimes called a stellar nursery (if star formation is occurring within), is a type of interstellar cloud, the density and size of which permit the formation of molecules, most commonly molecular hydrogen (H2).
Molecular cloud and Stellar evolution · Molecular cloud and Supernova ·
Nebula
A nebula (Latin for "cloud" or "fog"; pl. nebulae, nebulæ, or nebulas) is an interstellar cloud of dust, hydrogen, helium and other ionized gases.
Nebula and Stellar evolution · Nebula and Supernova ·
Neutrino
A neutrino (denoted by the Greek letter ν) is a fermion (an elementary particle with half-integer spin) that interacts only via the weak subatomic force and gravity.
Neutrino and Stellar evolution · Neutrino and Supernova ·
Neutron
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Neutron and Stellar evolution · Neutron and Supernova ·
Neutron star
A neutron star is the collapsed core of a large star which before collapse had a total of between 10 and 29 solar masses.
Neutron star and Stellar evolution · Neutron star and Supernova ·
Nova
A nova (plural novae or novas) or classical nova (CN, plural CNe) is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star, that slowly fades over several weeks or many months.
Nova and Stellar evolution · Nova and Supernova ·
Nuclear fusion
In nuclear physics, nuclear fusion is a reaction in which two or more atomic nuclei come close enough to form one or more different atomic nuclei and subatomic particles (neutrons or protons).
Nuclear fusion and Stellar evolution · Nuclear fusion and Supernova ·
Nucleosynthesis
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons.
Nucleosynthesis and Stellar evolution · Nucleosynthesis and Supernova ·
Oxygen
Oxygen is a chemical element with symbol O and atomic number 8.
Oxygen and Stellar evolution · Oxygen and Supernova ·
Pair-instability supernova
A pair-instability supernova occurs when pair production, the production of free electrons and positrons in the collision between atomic nuclei and energetic gamma rays, temporarily reduces the internal pressure supporting a supermassive star's core against gravitational collapse.
Pair-instability supernova and Stellar evolution · Pair-instability supernova and Supernova ·
Photodisintegration
Photodisintegration (also called phototransmutation) is a nuclear process in which an atomic nucleus absorbs a high-energy gamma ray, enters an excited state, and immediately decays by emitting a subatomic particle.
Photodisintegration and Stellar evolution · Photodisintegration and Supernova ·
Planet
A planet is an astronomical body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.
Planet and Stellar evolution · Planet and Supernova ·
Pulsar
A pulsar (from pulse and -ar as in quasar) is a highly magnetized rotating neutron star or white dwarf that emits a beam of electromagnetic radiation.
Pulsar and Stellar evolution · Pulsar and Supernova ·
Red giant
A red giant is a luminous giant star of low or intermediate mass (roughly 0.3–8 solar masses) in a late phase of stellar evolution.
Red giant and Stellar evolution · Red giant and Supernova ·
Shock wave
In physics, a shock wave (also spelled shockwave), or shock, is a type of propagating disturbance.
Shock wave and Stellar evolution · Shock wave and Supernova ·
Silicon
Silicon is a chemical element with symbol Si and atomic number 14.
Silicon and Stellar evolution · Silicon and Supernova ·
SN 1987A
SN 1987A was a peculiar type II supernova in the Large Magellanic Cloud, a dwarf galaxy satellite of the Milky Way.
SN 1987A and Stellar evolution · SN 1987A and Supernova ·
Solar System
The Solar SystemCapitalization of the name varies.
Solar System and Stellar evolution · Solar System and Supernova ·
Supergiant star
Supergiants are among the most massive and most luminous stars.
Stellar evolution and Supergiant star · Supergiant star and Supernova ·
Type Ia supernova
A type Ia supernova (read "type one-a") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf.
Stellar evolution and Type Ia supernova · Supernova and Type Ia supernova ·
Type II supernova
A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star.
Stellar evolution and Type II supernova · Supernova and Type II supernova ·
Uranium
Uranium is a chemical element with symbol U and atomic number 92.
Stellar evolution and Uranium · Supernova and Uranium ·
White dwarf
A white dwarf, also called a degenerate dwarf, is a stellar core remnant composed mostly of electron-degenerate matter.
Stellar evolution and White dwarf · Supernova and White dwarf ·
Wolf–Rayet star
Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of highly ionised helium and nitrogen or carbon.
Stellar evolution and Wolf–Rayet star · Supernova and Wolf–Rayet star ·
The list above answers the following questions
- What Stellar evolution and Supernova have in common
- What are the similarities between Stellar evolution and Supernova
Stellar evolution and Supernova Comparison
Stellar evolution has 138 relations, while Supernova has 257. As they have in common 48, the Jaccard index is 12.15% = 48 / (138 + 257).
References
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