ASTR 300 Stars and Stellar Systems Spring 2011
... Solving for M2 we find M2 = 60.7/3.875 = 15.7 M⊙, and then M1 = 60.7 − 15.7 = 45 M⊙. (c) If instead, the orbit is inclined at an angle of 45 degrees, what are the true velocities of the stars? In this case, what is their separation? What is the total mass and the individual masses? If the orbit is i ...
... Solving for M2 we find M2 = 60.7/3.875 = 15.7 M⊙, and then M1 = 60.7 − 15.7 = 45 M⊙. (c) If instead, the orbit is inclined at an angle of 45 degrees, what are the true velocities of the stars? In this case, what is their separation? What is the total mass and the individual masses? If the orbit is i ...
What is a star? A star is a giant ball of gases held together by gravity
... much energy. Smaller stars become white dwarfs as they get older, and large stars explode as supernovae which burn brightly and quickly. The material that explodes from a supernova becomes the gases and dust that creates new stars. ...
... much energy. Smaller stars become white dwarfs as they get older, and large stars explode as supernovae which burn brightly and quickly. The material that explodes from a supernova becomes the gases and dust that creates new stars. ...
1. Star A has a distance of 3 parsecs. What is its parallax angle? 1a
... The -4 magntude star has a greater luminosity by a factor 2.51210 . Star I is of spectral type O2 and star II is of spectral type O3. Which star is hotter? Star I. Which of the following stars is the most massive: a) G2V b) K8V c) O1V? c) because its the hottest and hence brightest and hence most lu ...
... The -4 magntude star has a greater luminosity by a factor 2.51210 . Star I is of spectral type O2 and star II is of spectral type O3. Which star is hotter? Star I. Which of the following stars is the most massive: a) G2V b) K8V c) O1V? c) because its the hottest and hence brightest and hence most lu ...
Stars - cmamath
... White dwarf: remains of low/medium mass stars after nuclear fusion has completely stopped. After the white dwarf has completely cooled, it becomes a black dwarf which is a dead star that no longer shines. ...
... White dwarf: remains of low/medium mass stars after nuclear fusion has completely stopped. After the white dwarf has completely cooled, it becomes a black dwarf which is a dead star that no longer shines. ...
www.NewYorkScienceTeacher.org/review
... shorter or longer, the observer can determine if the star is moving toward or away from Earth. These shifts are called blueshifts and redshifts. The larger the shift, the higher the speed of motion. The shifts in spectral lines can also be used to detect binary stars as they orbit around their cente ...
... shorter or longer, the observer can determine if the star is moving toward or away from Earth. These shifts are called blueshifts and redshifts. The larger the shift, the higher the speed of motion. The shifts in spectral lines can also be used to detect binary stars as they orbit around their cente ...
Practice questions for Stars File
... 1. Describe the difference in the stages of the life cycle for a large and massive star compared to an average star 2. Describe the fuel use changes from birth to death for a black hole 3. Describe the fuel use changes from birth to death for a neutron star 4. Explain how the energy changes are invo ...
... 1. Describe the difference in the stages of the life cycle for a large and massive star compared to an average star 2. Describe the fuel use changes from birth to death for a black hole 3. Describe the fuel use changes from birth to death for a neutron star 4. Explain how the energy changes are invo ...
chapter6
... Just by analyzing the light received from a star, astronomers can retrieve information about a star’s ...
... Just by analyzing the light received from a star, astronomers can retrieve information about a star’s ...
A Star is Born – Worksheet and Key – Ben Kwok
... What causes them to form? Gravitational forces pulling dust particles and gas together How do stars created energy? Nuclear fusion How long does a main sequence star live for? 10 billion years What marks the start of the death of a star? When the star can no longer fuse hydrgen What does the term re ...
... What causes them to form? Gravitational forces pulling dust particles and gas together How do stars created energy? Nuclear fusion How long does a main sequence star live for? 10 billion years What marks the start of the death of a star? When the star can no longer fuse hydrgen What does the term re ...
Stars
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
... • Begin their lives as clouds of dust and gas called nebulae • Gravity may cause the nebula to contract • Matter in the gas cloud will begin to condense into a dense region called a protostar • The protostar continues to condense, it heats up. Eventually, it reaches a critical mass and nuclear fusio ...
Name Physics 130 Astronomy Exam 2 August 2, 2004 Multiple Choice
... d.) The product (ash) nucleus contains fewer protons than the original (fuel) nucleus, since these protons have been converted into energy. 38. _____ The core collapse phase at the end of the life of a massive star is triggered when a.) nuclear fusion has produced a significant amount of iron in its ...
... d.) The product (ash) nucleus contains fewer protons than the original (fuel) nucleus, since these protons have been converted into energy. 38. _____ The core collapse phase at the end of the life of a massive star is triggered when a.) nuclear fusion has produced a significant amount of iron in its ...
Star Formation
... If the star-forming region is too hot, the elements (HII, dust, etc.) are moving too fast for gravity to overcome Sometimes one big star gets started before its neighbors, and it heats the region up so no other stars can form – However, if the first stars to turn on aren’t too hot, their solar winds ...
... If the star-forming region is too hot, the elements (HII, dust, etc.) are moving too fast for gravity to overcome Sometimes one big star gets started before its neighbors, and it heats the region up so no other stars can form – However, if the first stars to turn on aren’t too hot, their solar winds ...
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.