Wavelength
... • Eventually, the outer parts grow larger and drift out into space creating a planetary nebula. ...
... • Eventually, the outer parts grow larger and drift out into space creating a planetary nebula. ...
Galactic Address/Stars/Constellations
... Size of Stars • Stars can be as small as Earth or as large as the orbit of Jupiter. • https://www.youtube.com/watch?v=HEheh1BH34Q ...
... Size of Stars • Stars can be as small as Earth or as large as the orbit of Jupiter. • https://www.youtube.com/watch?v=HEheh1BH34Q ...
Supernovae
... inverse b-decay Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
... inverse b-decay Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
Foundations III The Stars
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements ...
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements ...
Star Facts - Dr. Noha MH Elnagdi
... Some look red (like Betelgeuse), some look more yellow (like the Sun), and some look blue or blue-white (like Sirius) ...
... Some look red (like Betelgeuse), some look more yellow (like the Sun), and some look blue or blue-white (like Sirius) ...
Regents Earth Science – Unit 5: Astronomy
... the Sun produces energy by the process of nuclear fusion in its core the sun’s outer atmosphere “the corona” can be seen during a total solar eclipse the Sun has sunspots (cooler, dark in color) - spots associated with the its magnetic field these increase and decrease in a cyclic pattern the sun al ...
... the Sun produces energy by the process of nuclear fusion in its core the sun’s outer atmosphere “the corona” can be seen during a total solar eclipse the Sun has sunspots (cooler, dark in color) - spots associated with the its magnetic field these increase and decrease in a cyclic pattern the sun al ...
Internet Space Scavenger Hunt
... 28.What determines how large a star will become? The amount of matter that is available for star formation in the nebula determines how large a star becomes. 29.Will a star’s lifecycle be shorter or longer if its mass is greater? Shorter 30.Black holes have an enormous ________________ pull. Gravita ...
... 28.What determines how large a star will become? The amount of matter that is available for star formation in the nebula determines how large a star becomes. 29.Will a star’s lifecycle be shorter or longer if its mass is greater? Shorter 30.Black holes have an enormous ________________ pull. Gravita ...
The Sun and other Stars
... the same time, but independently of each other. H-R Diagram – ____________________________ Most stars lie along a diagonal line called the ______ ...
... the same time, but independently of each other. H-R Diagram – ____________________________ Most stars lie along a diagonal line called the ______ ...
Star formation Stars form out of dense, cold, often dusty, molecular
... Free-fall†timescale for a cloud of this density is: ...
... Free-fall†timescale for a cloud of this density is: ...
Devil physics The baddest class on campus IB Physics
... quantum state Pauli exclusion principle says they will acquire large kinetic energy which allows the star to resist gravitational pressure to collapse ...
... quantum state Pauli exclusion principle says they will acquire large kinetic energy which allows the star to resist gravitational pressure to collapse ...
BV Color Index and Temperature - The University of Texas at Dallas
... of a sample of 50,000 known asteroids. The color indicates accuracy of the detection - the separation on the sky between the observed position of Gaia's detection and the expected position of PHYS-3380 each asteroid.The regions showing lower accuracy (red) of ...
... of a sample of 50,000 known asteroids. The color indicates accuracy of the detection - the separation on the sky between the observed position of Gaia's detection and the expected position of PHYS-3380 each asteroid.The regions showing lower accuracy (red) of ...
AST301.Ch22.NeutGammBH - University of Texas Astronomy
... Observed as pulsars (discovered 1967). Each pulsar has different pulse period (0.03 to 0.3 sec for most) but most are very stable. (Fig. ...
... Observed as pulsars (discovered 1967). Each pulsar has different pulse period (0.03 to 0.3 sec for most) but most are very stable. (Fig. ...
1.3 Lifecycle of stars
... Evolution of a Sun-Like Star The helium flash: The pressure within the helium core is almost totally due to “electron degeneracy”—two electrons cannot be in the same quantum state, so the core cannot contract beyond a certain point. This pressure is almost independent of temperature— when the heliu ...
... Evolution of a Sun-Like Star The helium flash: The pressure within the helium core is almost totally due to “electron degeneracy”—two electrons cannot be in the same quantum state, so the core cannot contract beyond a certain point. This pressure is almost independent of temperature— when the heliu ...
Stars, Galaxies, and the Universe
... Black hole: The remains of an extremely massive star pulled into a small volume by the force of gravity. ...
... Black hole: The remains of an extremely massive star pulled into a small volume by the force of gravity. ...
Fate of Stars
... For heavy white dwarves with a companion star • Acquire mass, if becomes > 1.4 M(Sun) ...
... For heavy white dwarves with a companion star • Acquire mass, if becomes > 1.4 M(Sun) ...
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.