Star Cycle Notes
... reduced. The force of gravity now pulls the star inward and the star becomes smaller (collapses). As the star collapses, the particles within the star (now mostly helium) heat up and get squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but ...
... reduced. The force of gravity now pulls the star inward and the star becomes smaller (collapses). As the star collapses, the particles within the star (now mostly helium) heat up and get squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but ...
The Lives of Stars
... Earth, but they have about as much mass as the sun. • Since a white dwarf has the same mass as the sun but only one millionth the volume, it is one million times as dense as the sun. A spoonful of material from a white dwarf has as much mass as a large truck. White dwarfs have no fuel, but they glow ...
... Earth, but they have about as much mass as the sun. • Since a white dwarf has the same mass as the sun but only one millionth the volume, it is one million times as dense as the sun. A spoonful of material from a white dwarf has as much mass as a large truck. White dwarfs have no fuel, but they glow ...
Notes - CH 12
... 1) Gravitational force causes clumps of matter to form in nebula 2) As they move closer, they move faster and heat up 3) As the clump contracts, it becomes spherical 4) When mass gets large enough it become a protostar 5) Temperature continues to increase and sphere becomes disk-like (elliptical) 6) ...
... 1) Gravitational force causes clumps of matter to form in nebula 2) As they move closer, they move faster and heat up 3) As the clump contracts, it becomes spherical 4) When mass gets large enough it become a protostar 5) Temperature continues to increase and sphere becomes disk-like (elliptical) 6) ...
Supernovae - Cloudfront.net
... the amount of energy created in a Type Ia Supernova is always about the same. Thus its luminosity is always the same. A Type Ia Supernova in another galaxy is thus a good standard candle to use to find the distance to the galaxy ...
... the amount of energy created in a Type Ia Supernova is always about the same. Thus its luminosity is always the same. A Type Ia Supernova in another galaxy is thus a good standard candle to use to find the distance to the galaxy ...
Life Cycle of a Star
... A supermassive black hole (SMBH) is the largest type of black hole, on the order of hundreds of thousands to billions of solar masses. Most—and possibly all—galaxies are inferred to contain a supermassive black hole at their centers. In the case of the Milky Way, the SMBH is believed to correspond w ...
... A supermassive black hole (SMBH) is the largest type of black hole, on the order of hundreds of thousands to billions of solar masses. Most—and possibly all—galaxies are inferred to contain a supermassive black hole at their centers. In the case of the Milky Way, the SMBH is believed to correspond w ...
Lifecycle of Stars - Mrs. Plante Science
... forming larger and larger balls of gas and dust molecules. • When the mass becomes large enough, gravitational contraction results in high pressure and temperature, and a protostar is formed. ...
... forming larger and larger balls of gas and dust molecules. • When the mass becomes large enough, gravitational contraction results in high pressure and temperature, and a protostar is formed. ...
Nebula – • The most abundant element in the universe is hydrogen
... A star is a sphere of super-hot gases, mostly hydrogen and helium that is held together by its own gravity. No two stars contain exactly the same elements in the same proportions. Stars are born by contraction of gasses inside a nebula. ...
... A star is a sphere of super-hot gases, mostly hydrogen and helium that is held together by its own gravity. No two stars contain exactly the same elements in the same proportions. Stars are born by contraction of gasses inside a nebula. ...
NOVAE and SUPERNOVAE
... Novae are repeat phenomena; WDs may explode many times. The explosion cycle is regulated by the rate at which matter is deposited onto the WD. More violent (and luminous) novae occur less frequently. Novae can ONLY occur in close binary star systems, where the possibility for mass transfer exist ...
... Novae are repeat phenomena; WDs may explode many times. The explosion cycle is regulated by the rate at which matter is deposited onto the WD. More violent (and luminous) novae occur less frequently. Novae can ONLY occur in close binary star systems, where the possibility for mass transfer exist ...
Stars and Light
... outward pressure from fusion. • Once the fusion stops, (H runs out) gravity will force the sun to collapse, which will increase the temperature so He can fuse (to form carbon). • When it does this, the outer layers “explode” and it becomes a Red Giant star. ...
... outward pressure from fusion. • Once the fusion stops, (H runs out) gravity will force the sun to collapse, which will increase the temperature so He can fuse (to form carbon). • When it does this, the outer layers “explode” and it becomes a Red Giant star. ...
Quiz Chapter 10 Answers
... The shockwave from a nearby supernova b) The shockwave from a newly formed high-mass star that is nearby c) The shockwave experienced by the cloud as it passes through a spiral arm d) All of the above X 10-11. Why does the core of a star contract during its time on the main sequence? a) The temperat ...
... The shockwave from a nearby supernova b) The shockwave from a newly formed high-mass star that is nearby c) The shockwave experienced by the cloud as it passes through a spiral arm d) All of the above X 10-11. Why does the core of a star contract during its time on the main sequence? a) The temperat ...
Astrophysics 12 - Stellar Evolution
... For stars with mass similar to the of the Sun, the carbon-oxygen core isn’t hot enough for fusion. The core continues to contract until electrons exert enough pressure to stop it collapsing further. ...
... For stars with mass similar to the of the Sun, the carbon-oxygen core isn’t hot enough for fusion. The core continues to contract until electrons exert enough pressure to stop it collapsing further. ...
Supernovae: Heavy Elements
... A Different Kind of Big Bang • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ...
... A Different Kind of Big Bang • The pressure of these neutrinos causes part of the imploding core to rebound • This rebound comes in the form of a shockwave, which rips through the still collapsing outer core • The collapsing outer shell is met by the shockwave and then by a rarefaction wave and is ...
The Life Cycle of a Star
... Stellar winds will peel away gases of the red giant and over time, its remnant will cool slowly and lose its brightness. It then becomes a white dwarf. ...
... Stellar winds will peel away gases of the red giant and over time, its remnant will cool slowly and lose its brightness. It then becomes a white dwarf. ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.