Amie Bickert - ColonialAcademyScience
... Protostar- earliest stage of a stars life White dwarf: blue-white core of the star that is left behind cools forms this. Supernovas: an explosion of a suergiant Neutron star: the remains of high-mass stars. Black holes- an object with gravity so strong that nothing, not even light, can esc ...
... Protostar- earliest stage of a stars life White dwarf: blue-white core of the star that is left behind cools forms this. Supernovas: an explosion of a suergiant Neutron star: the remains of high-mass stars. Black holes- an object with gravity so strong that nothing, not even light, can esc ...
So why are more massive stars more luminous?
... with TAs by sending them e-mail, starting now. The first 50 will be signed up for March 7. If there are more then 50 people they will be signed up for ...
... with TAs by sending them e-mail, starting now. The first 50 will be signed up for March 7. If there are more then 50 people they will be signed up for ...
Lecture21 - UCSB Physics
... • A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it • B) Higher temperatures inhibit star formation • C) Higher temperatures help star formation • D) Star formation is independent of the temperature of the cloud ...
... • A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it • B) Higher temperatures inhibit star formation • C) Higher temperatures help star formation • D) Star formation is independent of the temperature of the cloud ...
Formation of Stars
... Gravity works to compress a cloud. As an interstellar cloud collapses, it heats up. The rise in internal temperature and pressure works to counter gravity and stop the compression. ...
... Gravity works to compress a cloud. As an interstellar cloud collapses, it heats up. The rise in internal temperature and pressure works to counter gravity and stop the compression. ...
Questions for this book (Word format)
... 1. When Eddington suggested in 1926 that stars were powered by hydrogen fusion, why did most physicists quite reasonably reject this suggestion? Explain the phenomenon, unknown in 1926, that allows hydrogen fusion to occur in the cores of stars. Briefly summarise, with a time-line, the historical st ...
... 1. When Eddington suggested in 1926 that stars were powered by hydrogen fusion, why did most physicists quite reasonably reject this suggestion? Explain the phenomenon, unknown in 1926, that allows hydrogen fusion to occur in the cores of stars. Briefly summarise, with a time-line, the historical st ...
Option: Astrophysics Objects in the Universe: Asteroid: a small rocky
... 2. All planets have orbital planes that are inclined by less than 6° 3. Terrestrial planets are dense, rocky and small; Jovian planets are gaseous and ...
... 2. All planets have orbital planes that are inclined by less than 6° 3. Terrestrial planets are dense, rocky and small; Jovian planets are gaseous and ...
Instrumentation for Cosmology
... The spiral arms are an illusion. They trace the passage of a ‘sound wave’ through the disk of the galaxy ...
... The spiral arms are an illusion. They trace the passage of a ‘sound wave’ through the disk of the galaxy ...
THE LIFE CYCLE OF A STAR
... A star is a luminous globe of gas producing its own heat and light by nuclear reactions (nuclear fusion). They are born from nebulae and consist mostly of hydrogen and helium gas. Surface temperatures range from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brighte ...
... A star is a luminous globe of gas producing its own heat and light by nuclear reactions (nuclear fusion). They are born from nebulae and consist mostly of hydrogen and helium gas. Surface temperatures range from 2000C to above 30,000C, and the corresponding colors from red to blue-white. The brighte ...
01 - Ionia Public Schools
... _____ 28. After the supergiant stage, massive stars contract with a gravitational force that is a. a much less than that of small-mass stars. b. much greater than that of large-mass stars. c. much less than that of white dwarf stars. d. much greater than that of small mass stars. 29. What happens wh ...
... _____ 28. After the supergiant stage, massive stars contract with a gravitational force that is a. a much less than that of small-mass stars. b. much greater than that of large-mass stars. c. much less than that of white dwarf stars. d. much greater than that of small mass stars. 29. What happens wh ...
Evolution of Stars and Galaxies
... After core uses up He, contracts more Outer layer escapes into space Leaves behind a hot, dense core (about the size of Earth) Eventually will cool and stop giving off light ...
... After core uses up He, contracts more Outer layer escapes into space Leaves behind a hot, dense core (about the size of Earth) Eventually will cool and stop giving off light ...
Final Exam Practice Part I
... 4. What caused its shape to become a disk? 5. Today’s planets formed from dust and gases that clumped together. What caused this clumping into actual planets? 6. The inner planets of our solar system are rocky, while the outer planets are “gas giants.” Why are the inner and outer planets different? ...
... 4. What caused its shape to become a disk? 5. Today’s planets formed from dust and gases that clumped together. What caused this clumping into actual planets? 6. The inner planets of our solar system are rocky, while the outer planets are “gas giants.” Why are the inner and outer planets different? ...
Chapter 12
... shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star produces a Red Giant ...
... shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star produces a Red Giant ...
Outline 8: History of the Universe and Solar System
... Why the apparent older age? Consider the following example: Travel at 100 mph for 2 hours = 200 miles Travel at 60 mph for 3 hours = 180 miles Total time is 5 hours. Total distance is 380 miles. If you were observed traveling at 60 mph and had covered 380 miles, the assumption would be made that you ...
... Why the apparent older age? Consider the following example: Travel at 100 mph for 2 hours = 200 miles Travel at 60 mph for 3 hours = 180 miles Total time is 5 hours. Total distance is 380 miles. If you were observed traveling at 60 mph and had covered 380 miles, the assumption would be made that you ...
Slayt 1
... into the interstellar medium. • Even higher elements like gold, uranium etc are formed during the SN explosion. • Now the interstellar medium is richer with heavy elements. • …but how did these elements in the interstellar medium came to our body? ...
... into the interstellar medium. • Even higher elements like gold, uranium etc are formed during the SN explosion. • Now the interstellar medium is richer with heavy elements. • …but how did these elements in the interstellar medium came to our body? ...
Type II supernova
A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star. A star must have at least 8 times, and no more than 40–50 times, the mass of the Sun (M☉) for this type of explosion. It is distinguished from other types of supernovae by the presence of hydrogen in its spectrum. Type II supernovae are mainly observed in the spiral arms of galaxies and in H II regions, but not in elliptical galaxies.Stars generate energy by the nuclear fusion of elements. Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans. The degeneracy pressure of electrons and the energy generated by these fusion reactions are sufficient to counter the force of gravity and prevent the star from collapsing, maintaining stellar equilibrium. The star fuses increasingly higher mass elements, starting with hydrogen and then helium, progressing up through the periodic table until a core of iron and nickel is produced. Fusion of iron or nickel produces no net energy output, so no further fusion can take place, leaving the nickel-iron core inert. Due to the lack of energy output allowing outward pressure, equilibrium is broken.When the mass of the inert core exceeds the Chandrasekhar limit of about 1.4 M☉, electron degeneracy alone is no longer sufficient to counter gravity and maintain stellar equilibrium. A cataclysmic implosion takes place within seconds, in which the outer core reaches an inward velocity of up to 23% of the speed of light and the inner core reaches temperatures of up to 100 billion kelvin. Neutrons and neutrinos are formed via reversed beta-decay, releasing about 1046 joules (100 foes) in a ten-second burst. The collapse is halted by neutron degeneracy, causing the implosion to rebound and bounce outward. The energy of this expanding shock wave is sufficient to accelerate the surrounding stellar material to escape velocity, forming a supernova explosion, while the shock wave and extremely high temperature and pressure briefly allow for theproduction of elements heavier than iron. Depending on initial size of the star, the remnants of the core form a neutron star or a black hole. Because of the underlying mechanism, the resulting nova is also described as a core-collapse supernova.There exist several categories of Type II supernova explosions, which are categorized based on the resulting light curve—a graph of luminosity versus time—following the explosion. Type II-L supernovae show a steady (linear) decline of the light curve following the explosion, whereas Type II-P display a period of slower decline (a plateau) in their light curve followed by a normal decay. Type Ib and Ic supernovae are a type of core-collapse supernova for a massive star that has shed its outer envelope of hydrogen and (for Type Ic) helium. As a result, they appear to be lacking in these elements.