
Name: Notes – #45 The Diverse Sizes of Stars 1. A Hertzsprung
... 6. Super giants tend to have surface temperatures cooler than the sun but emit 104 time or more energy than the Sun. Why is this true? 7. The size of the star Betelgeuse in the constellation Orion is approximately the same size as ____________’s orbit around the Sun. 8. What stars have the same temp ...
... 6. Super giants tend to have surface temperatures cooler than the sun but emit 104 time or more energy than the Sun. Why is this true? 7. The size of the star Betelgeuse in the constellation Orion is approximately the same size as ____________’s orbit around the Sun. 8. What stars have the same temp ...
Review_game_and_answers
... 7- How are all galaxies moving in relation to every other galaxy? Away from each other ...
... 7- How are all galaxies moving in relation to every other galaxy? Away from each other ...
22 Stellar Remnant/HR Diagram
... Red giant • Large radius • High luminosity • Fairly cool (red) • Left over core • Small radius (Earth) • Low luminosity • Really hot (blue/white) ...
... Red giant • Large radius • High luminosity • Fairly cool (red) • Left over core • Small radius (Earth) • Low luminosity • Really hot (blue/white) ...
Supernovae, Neutron Stars, Black Holes
... the supernova explosion of SN 1987A. ---- a 1028 megaton bomb (i.e., a few octillion nuclear warheads). ...
... the supernova explosion of SN 1987A. ---- a 1028 megaton bomb (i.e., a few octillion nuclear warheads). ...
Chapter 29 Notes
... • Parallax is used to find the distance to stars • Constellations: Groups of stars in the same part of the sky • Clusters: groups of stars bound together by gravity • Binaries: two stars that orbit a common center of mass ...
... • Parallax is used to find the distance to stars • Constellations: Groups of stars in the same part of the sky • Clusters: groups of stars bound together by gravity • Binaries: two stars that orbit a common center of mass ...
File - Mr. Goodyear Astronomy
... moves back toward main sequence area of H-R diagram. - Star fluctuates on and off main sequence. Gravity tries to contact star creating other elements in star increasing fusion process. - This increase energy causes an explosion-like occurrence. This cause star to lose large quantities of mass. - Al ...
... moves back toward main sequence area of H-R diagram. - Star fluctuates on and off main sequence. Gravity tries to contact star creating other elements in star increasing fusion process. - This increase energy causes an explosion-like occurrence. This cause star to lose large quantities of mass. - Al ...
Giant Stars
... • Three helium nuclei can fuse into one carbon nucleus. – Temperature over 108 K (100 million) – High density to collide within 10-8 s photon ...
... • Three helium nuclei can fuse into one carbon nucleus. – Temperature over 108 K (100 million) – High density to collide within 10-8 s photon ...
Homework, August 29, 2002 AST110-6
... 1. If nuclear fusion of hydrogen in the core of the Sun were to stop now, what would we see on the surface of the Sun tomorrow? Why? Will we be able to tell that hydrogen burning in the core has stopped? How? (20pt) (Hint: What particles that are generated by the fusion of hydrogen can escape from t ...
... 1. If nuclear fusion of hydrogen in the core of the Sun were to stop now, what would we see on the surface of the Sun tomorrow? Why? Will we be able to tell that hydrogen burning in the core has stopped? How? (20pt) (Hint: What particles that are generated by the fusion of hydrogen can escape from t ...
SNC1PL The Life Cycle of Stars
... After 10 billion years, a main sequence star (like the Sun) has converted most of its hydrogen into helium. With less energy pushing outwards, the helium center starts to contract. This contraction causes the core to heat up. Heat from the core causes any remaining hydrogen in the outer layers to fu ...
... After 10 billion years, a main sequence star (like the Sun) has converted most of its hydrogen into helium. With less energy pushing outwards, the helium center starts to contract. This contraction causes the core to heat up. Heat from the core causes any remaining hydrogen in the outer layers to fu ...
LT 9: I can describe how a protostar becomes a star.
... Variable stars: vary in brightness over regular cycles – Pulsating stars: change in brightness as they expand (cool, dim) and contract (hot, bright) – Cepheid variables: the longer their cycle is the larger their absolute magnitude is – Eclipsing binary: 2 stars of unequal brightness that revolve ar ...
... Variable stars: vary in brightness over regular cycles – Pulsating stars: change in brightness as they expand (cool, dim) and contract (hot, bright) – Cepheid variables: the longer their cycle is the larger their absolute magnitude is – Eclipsing binary: 2 stars of unequal brightness that revolve ar ...
Life Cycle of Stars - Lab Science Schedule
... Galaxies contain nebulae (huge clouds of gas and dust), which is the birthplace of stars. Some of the hydrogen gas in the nebula is clumped together by gravity & the hydrogen atoms form a spinning cloud. More and more hydrogen gas is pulled into the cloud over millions of years. Collisions between h ...
... Galaxies contain nebulae (huge clouds of gas and dust), which is the birthplace of stars. Some of the hydrogen gas in the nebula is clumped together by gravity & the hydrogen atoms form a spinning cloud. More and more hydrogen gas is pulled into the cloud over millions of years. Collisions between h ...
Star Life Guided Notes
... determines the fate of a star. gravityand _____ fusion The two forces acting on a star are ____ When a star reaches the end of its life it begins to helium and it ______. fuse ______ swells planetary When fusion stops a typical star will producenebula a __ white dwarf and become a ______ _____. Even ...
... determines the fate of a star. gravityand _____ fusion The two forces acting on a star are ____ When a star reaches the end of its life it begins to helium and it ______. fuse ______ swells planetary When fusion stops a typical star will producenebula a __ white dwarf and become a ______ _____. Even ...
Unit_Phys_2_nuclear_fusion__fission
... a) Nuclear fusion is the joining of two atomic nuclei to form a larger one. b) Nuclear fusion is the process by which energy is released in stars. c) Stars form when enough dust and gas from space is pulled together by gravitational attraction. Smaller masses may also form and be attracted by a larg ...
... a) Nuclear fusion is the joining of two atomic nuclei to form a larger one. b) Nuclear fusion is the process by which energy is released in stars. c) Stars form when enough dust and gas from space is pulled together by gravitational attraction. Smaller masses may also form and be attracted by a larg ...
Chapter 8 lesson 4 Notes
... Stars form when matter comes together and starts to give off energy. ...
... Stars form when matter comes together and starts to give off energy. ...
High Mass Stellar Evolution
... High mass stars (> 8 Msolar) have more fuel but they use it up much more quickly than low mass stars (higher luminosity). ...
... High mass stars (> 8 Msolar) have more fuel but they use it up much more quickly than low mass stars (higher luminosity). ...
lecture22
... becomes denser (and heats up!) Eventually, the electrons are forced to be too close together. A quantum mechanical law called the Pauli Exclusion Principle restricts electrons from being in the same state (i.e., keeps them from being too close together). The resulting outward pressure which keeps th ...
... becomes denser (and heats up!) Eventually, the electrons are forced to be too close together. A quantum mechanical law called the Pauli Exclusion Principle restricts electrons from being in the same state (i.e., keeps them from being too close together). The resulting outward pressure which keeps th ...
Lecture 15 (pdf from the powerpoint)
... • The core of a red giant star is very dense, and can get to very high temperatures – If the temperature is high enough, helium fuses into Beryllium, and then fuses with another helium nuclei to form carbon. ...
... • The core of a red giant star is very dense, and can get to very high temperatures – If the temperature is high enough, helium fuses into Beryllium, and then fuses with another helium nuclei to form carbon. ...
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.