Star Formation/Llfe Cycle Notes
... c. Known as Protostar of YSO, before it reaches main sequence d. Center of protostar gets dense enough and therefore hot enough (3000K+) to become luminous, however not visible due to exterior of gas and dust surrounding it. 3) Phophids- YSO’s starting to disk a. start to get charged particles 4) Ea ...
... c. Known as Protostar of YSO, before it reaches main sequence d. Center of protostar gets dense enough and therefore hot enough (3000K+) to become luminous, however not visible due to exterior of gas and dust surrounding it. 3) Phophids- YSO’s starting to disk a. start to get charged particles 4) Ea ...
Elements from Stardust
... With the high pressure and hot temperature in the sun, nuclei of atoms are squeezed together and they collide. Nuclear fusion combines smaller nuclei into larger nuclei—making bigger and heavier atoms. ...
... With the high pressure and hot temperature in the sun, nuclei of atoms are squeezed together and they collide. Nuclear fusion combines smaller nuclei into larger nuclei—making bigger and heavier atoms. ...
3 - MrFuglestad
... White Dwarf – Earth sized star that is stable with no nuclear reactions and is made of helium or carbon depending on the mass. Less massive than our Sun = Helium. There can be other elements present such as Oxygen, etc. Often the White Dwarf stars are surrounded by nebula. Black Dwarf – This star is ...
... White Dwarf – Earth sized star that is stable with no nuclear reactions and is made of helium or carbon depending on the mass. Less massive than our Sun = Helium. There can be other elements present such as Oxygen, etc. Often the White Dwarf stars are surrounded by nebula. Black Dwarf – This star is ...
01 - cloudfront.net
... the H-R diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. 6. A 7. C 8. Dense regions of matter build up within the nebula. 9. a shrinking, spinning region that begins to flatten into a disk with a central concentration of matter 10. Gravit ...
... the H-R diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. 6. A 7. C 8. Dense regions of matter build up within the nebula. 9. a shrinking, spinning region that begins to flatten into a disk with a central concentration of matter 10. Gravit ...
Protostar, Initial mass, Main Sequence
... Red dwarf stars with less than half a solar mass do not achieve red giant status they begin to fade as soon as their hydrogen fuel is exhausted. White dwarfs, planetary nebulae Our Sun, and any star with similar mass, will fuse to carbon and, possibly, oxygen and neon before shrinking to become a wh ...
... Red dwarf stars with less than half a solar mass do not achieve red giant status they begin to fade as soon as their hydrogen fuel is exhausted. White dwarfs, planetary nebulae Our Sun, and any star with similar mass, will fuse to carbon and, possibly, oxygen and neon before shrinking to become a wh ...
Astrobiology 101
... The heaviest elements are created in supernovae, the fantastic death of supergiant stars. As the core of the supergiant becomes saturated with iron, its pressure and temperature increase. Eventually, the blackbody radiation from the core produces gamma rays powerful enough to break apart the iron a ...
... The heaviest elements are created in supernovae, the fantastic death of supergiant stars. As the core of the supergiant becomes saturated with iron, its pressure and temperature increase. Eventually, the blackbody radiation from the core produces gamma rays powerful enough to break apart the iron a ...
Introduction to Astrophysics Tutorial 4: Supernovae
... • Mass loss plays an important role (the higher the mass, the greater the mass loss), but is poorly ...
... • Mass loss plays an important role (the higher the mass, the greater the mass loss), but is poorly ...
20.1 Notes
... the outer layers will _________________ becoming a _________ ________________. The star is red because it is _____________, but the core is still hot enough to convert helium into __________________ and ___________________. ...
... the outer layers will _________________ becoming a _________ ________________. The star is red because it is _____________, but the core is still hot enough to convert helium into __________________ and ___________________. ...
Stellar evolution
... in the core of the star. The star is stable as the pressure of the expanding gas counteracts gravity. As the helium core grows, hydrogen fusion moves out into the star, and the size increases. The star eventually runs out of hydrogen it can fuse, and collapses. If the star is big enough, the collaps ...
... in the core of the star. The star is stable as the pressure of the expanding gas counteracts gravity. As the helium core grows, hydrogen fusion moves out into the star, and the size increases. The star eventually runs out of hydrogen it can fuse, and collapses. If the star is big enough, the collaps ...
Star Factories: Nuclear Fusion and the Creation of the Elements
... The R-Process When the supernova explodes, large numbers of neutrons are shot out of the interior of the star at high velocities. Think of these like pellets in a shot gun shell that has been fired. These neutrons pass through the outer regions of the star, colliding with the atoms already there (m ...
... The R-Process When the supernova explodes, large numbers of neutrons are shot out of the interior of the star at high velocities. Think of these like pellets in a shot gun shell that has been fired. These neutrons pass through the outer regions of the star, colliding with the atoms already there (m ...
Interstellar clouds
... • Luminosity is determined by the amount of fuel that it is burning. • Our sun fuses 4 billion kilograms of hydrogen per second. • In some 5 billion years from now the sun’s life will come to an end. • The more massive a star the shorter its life time, since increasing the mass/gravity increases the ...
... • Luminosity is determined by the amount of fuel that it is burning. • Our sun fuses 4 billion kilograms of hydrogen per second. • In some 5 billion years from now the sun’s life will come to an end. • The more massive a star the shorter its life time, since increasing the mass/gravity increases the ...
No Slide Title
... IIs, yet! Too hard to calibrate • Instead we use Type Ia • Type Ia come from binary star systems that have one member that is a white dwarf (WD). • The WD is less than 1.4 solar masses ...
... IIs, yet! Too hard to calibrate • Instead we use Type Ia • Type Ia come from binary star systems that have one member that is a white dwarf (WD). • The WD is less than 1.4 solar masses ...
Life and Death of a Star – video questions
... 9. __________ is the fundamental thing that drives the life history of stars. _______________ stars live their lives faster. 10. The size of a star influences how it ______________. 11. what will gravity do to the sun when fusion is over? ...
... 9. __________ is the fundamental thing that drives the life history of stars. _______________ stars live their lives faster. 10. The size of a star influences how it ______________. 11. what will gravity do to the sun when fusion is over? ...
PowerPoint File
... • So, massive stars run out of fuel sooner. The more massive, the shorter their Main Sequence lifetime ...
... • So, massive stars run out of fuel sooner. The more massive, the shorter their Main Sequence lifetime ...
The Lifecycle of Stars
... When A Star Dies Supernova Some massive stars may explode in a large, bright display called a Supernova Supernova occur when a massive star collapses and throws its outer layers into space. This explosion is so powerful that it can be brighter than an entire galaxy for several days!! ...
... When A Star Dies Supernova Some massive stars may explode in a large, bright display called a Supernova Supernova occur when a massive star collapses and throws its outer layers into space. This explosion is so powerful that it can be brighter than an entire galaxy for several days!! ...
Astronomy Galaxies & The Universe
... brightest are ≤ 1 faintest are ≥ 6 absolute magnitude – expresses luminosity of stars as if they were all seen 32.6 lightyears from Earth (our sun = 4.8) ...
... brightest are ≤ 1 faintest are ≥ 6 absolute magnitude – expresses luminosity of stars as if they were all seen 32.6 lightyears from Earth (our sun = 4.8) ...
The big bang left the universe with its first atoms
... The heaviest elements are created in supernovae, the fantastic death of supergiant stars. As the core of the supergiant becomes saturated with iron, its pressure and temperature increase. Eventually, the blackbody radiation from the core produces gamma rays powerful enough to break apart the iron a ...
... The heaviest elements are created in supernovae, the fantastic death of supergiant stars. As the core of the supergiant becomes saturated with iron, its pressure and temperature increase. Eventually, the blackbody radiation from the core produces gamma rays powerful enough to break apart the iron a ...
Linking Asteroids and Meteorites through Reflectance
... • A star-forming cloud is called a molecular cloud because low temperatures allow Hydrogen to form Hydrogen molecules (H2) • Temperatures like 10-50 K ...
... • A star-forming cloud is called a molecular cloud because low temperatures allow Hydrogen to form Hydrogen molecules (H2) • Temperatures like 10-50 K ...
Death of Stars
... temperatures to start fusion, so they will remain red hot for billions of years. • Low mass stars end as white dwarfs ...
... temperatures to start fusion, so they will remain red hot for billions of years. • Low mass stars end as white dwarfs ...
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.