Astronomy Chapter 13 Name
... D. A type of binary star in which the spectrum lines exhibit a changing Doppler shift as a result of the orbital motion of one star around the other ...
... D. A type of binary star in which the spectrum lines exhibit a changing Doppler shift as a result of the orbital motion of one star around the other ...
Stars - HMXEarthScience
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
... 1. Large clouds of dust and gas are pulled together by gravity (these clouds are called nebulae) 2. Gases in the nebula contract due to gravity, resulting in the formation of a protostar. 3. Pressure and temperature increase until the gases “ignite” and nuclear fusion begins 4. Once the star has ful ...
Week 11 Answers
... The more massive stars have shorter lifetimes. Also, the more mass that a main sequence star has, the higher its surface temperature. Cluster D has main sequence stars with surface temperatures all the way up to 20,000 degrees and more. These are stars that do not live for very long as main sequence ...
... The more massive stars have shorter lifetimes. Also, the more mass that a main sequence star has, the higher its surface temperature. Cluster D has main sequence stars with surface temperatures all the way up to 20,000 degrees and more. These are stars that do not live for very long as main sequence ...
Theoretical Modeling of Massive Stars Mr. Russell University of Delaware
... 10 M_sun Bipolar Nebula enshrouds star(s) from 1840’s “Giant Eruption” Very close so lots of data Data predicts system is actually a binary system with one star ~90 M_sun and the other ~30 M_sun Think it is in last stages of life before big star undergoes a supernova ...
... 10 M_sun Bipolar Nebula enshrouds star(s) from 1840’s “Giant Eruption” Very close so lots of data Data predicts system is actually a binary system with one star ~90 M_sun and the other ~30 M_sun Think it is in last stages of life before big star undergoes a supernova ...
Starry Starry Night Vocabulary
... Artist: A person who creates art such as paintings, drawings or sculpture. Astronomy: The study of objects outside the earth’s atmosphere, including planets and stars. Author: A person who writes a story or a book. Aztecs: An ancient civilization in Mexico. Aztecs studies the stars, noticed that the ...
... Artist: A person who creates art such as paintings, drawings or sculpture. Astronomy: The study of objects outside the earth’s atmosphere, including planets and stars. Author: A person who writes a story or a book. Aztecs: An ancient civilization in Mexico. Aztecs studies the stars, noticed that the ...
the lab handout here
... According to the HR diagram, a massive star with a surface temperature of 20,000 K that is nearly a million times brighter than the sun would mostly likely be classified as a ...
... According to the HR diagram, a massive star with a surface temperature of 20,000 K that is nearly a million times brighter than the sun would mostly likely be classified as a ...
Document
... • Stars don’t live forever. Stars expand as it grows old. After the hydrogen (fuel) is used up, the star will begin to die. The core contracts and the outer layers expand, cool, and become less bright. It then becomes a red giant star. • Helium is now being used, and the core begins to shrink, and o ...
... • Stars don’t live forever. Stars expand as it grows old. After the hydrogen (fuel) is used up, the star will begin to die. The core contracts and the outer layers expand, cool, and become less bright. It then becomes a red giant star. • Helium is now being used, and the core begins to shrink, and o ...
The Life Cycle of Stars Webquest
... 1. The nuclear reactions inside a star, such as our sun, convert hydrogen into helium by means of a process known as. 2. What gives a star its energy? 3. How many protons does a standard hydrogen atom have in its nucleus? ...
... 1. The nuclear reactions inside a star, such as our sun, convert hydrogen into helium by means of a process known as. 2. What gives a star its energy? 3. How many protons does a standard hydrogen atom have in its nucleus? ...
Astronomy Study Guide #2
... 23. What is the ``Doppler Effect" and how does it apply to light? And to stars? 24. Why are the Balmer lines of hydrogen important? What are they and how are they formed? (Hint: We saw these in the spectral tube demonstrations.) 25. How will stars less massive than 1.5 M_0 end their Post-Main Seque ...
... 23. What is the ``Doppler Effect" and how does it apply to light? And to stars? 24. Why are the Balmer lines of hydrogen important? What are they and how are they formed? (Hint: We saw these in the spectral tube demonstrations.) 25. How will stars less massive than 1.5 M_0 end their Post-Main Seque ...
What have we learned?
... • How does a star’s mass affect nuclear fusion? – A star’s mass determines its core pressure and temperature and therefore determines its fusion rate. – Higher mass stars have hotter cores, faster fusion rates, greater luminosities, and shorter ...
... • How does a star’s mass affect nuclear fusion? – A star’s mass determines its core pressure and temperature and therefore determines its fusion rate. – Higher mass stars have hotter cores, faster fusion rates, greater luminosities, and shorter ...
Brock physics - Brock University
... (a) Fusion of two 3 He nuclei into a 4 He nucleus. (b) Fusion of hydrogen and deuterium into 3 He. (c) Fusion of two protons into deuterium with a release of a positron, a neutrino and energy. (d) [None of the above.] 38. When four hydrogen nuclei fuse to form a helium nucleus, the total mass at the ...
... (a) Fusion of two 3 He nuclei into a 4 He nucleus. (b) Fusion of hydrogen and deuterium into 3 He. (c) Fusion of two protons into deuterium with a release of a positron, a neutrino and energy. (d) [None of the above.] 38. When four hydrogen nuclei fuse to form a helium nucleus, the total mass at the ...
Page 1 Astronomy 110 Homework #08 Assigned: 03/13/2007 Due
... A) to dim and redden distant stars by preferentially scattering their blue light. B) to scatter the red light from stars preferentially, making them appear more blue than expected. C) almost nonexistent, because light does not interact with dust. D) to make stars appear less bright than expected by ...
... A) to dim and redden distant stars by preferentially scattering their blue light. B) to scatter the red light from stars preferentially, making them appear more blue than expected. C) almost nonexistent, because light does not interact with dust. D) to make stars appear less bright than expected by ...
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.