Educator`s Guide for Dark Star Adventure
... 2. Have children practice drawing what they see out toward the horizon from the horizon up to their zenith. Then have children practice doing night sky observational drawing in the classroom; have them pick an area of the room and draw what they see from the “horizon” (the floor) and up, including t ...
... 2. Have children practice drawing what they see out toward the horizon from the horizon up to their zenith. Then have children practice doing night sky observational drawing in the classroom; have them pick an area of the room and draw what they see from the “horizon” (the floor) and up, including t ...
Astro 204: Practice Questions Some of these questions are a bit
... 19. A bright star is observed to orbit a supermassive black hole in a circular orbit with a period of 20 years. The orbital plane is inclined with respect to the plane of the sky by 30◦ . Observations of various lines in the stellar spectrum show that the maximum line-of-sight velocity exhibited by ...
... 19. A bright star is observed to orbit a supermassive black hole in a circular orbit with a period of 20 years. The orbital plane is inclined with respect to the plane of the sky by 30◦ . Observations of various lines in the stellar spectrum show that the maximum line-of-sight velocity exhibited by ...
Stellar Evolution
... than the Sun A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate Its path across the H-R diagram is essentially a straight line It stays at just about the same luminosity as it cools off Eventually the star dies in a violent explosion ...
... than the Sun A star of more than 8 solar masses can fuse elements far beyond carbon in its core, leading to a very different fate Its path across the H-R diagram is essentially a straight line It stays at just about the same luminosity as it cools off Eventually the star dies in a violent explosion ...
RTFS Test - 2017 BCS Cobra
... 70. Review the spectral types of some of the main sequence stars in the table below: Which star is: Star Spectral Type mv Q1: Brightest in apparent A G2 V ...
... 70. Review the spectral types of some of the main sequence stars in the table below: Which star is: Star Spectral Type mv Q1: Brightest in apparent A G2 V ...
Understanding the H-R Diagram
... temperature. They range in temperature from super hot bluewhite stars (over 20,000°C) to cool red stars (2,500°C + to 3,000°C). Look at the chart below and you will see that our Sun is a medium yellow star. A star's color is determined by its temperature. Red stars are cooler and blue stars are hott ...
... temperature. They range in temperature from super hot bluewhite stars (over 20,000°C) to cool red stars (2,500°C + to 3,000°C). Look at the chart below and you will see that our Sun is a medium yellow star. A star's color is determined by its temperature. Red stars are cooler and blue stars are hott ...
chapter14Sol
... neutrinos failed to find the predicted number. Down by a factor of three. This experiment was done deep underground only neutrinos could penetrate that far. Cl was transformed to Ar when a neutron was transformed into a proton and an electron by the absorption of a neutrino. http://en.wikipedia.org/ ...
... neutrinos failed to find the predicted number. Down by a factor of three. This experiment was done deep underground only neutrinos could penetrate that far. Cl was transformed to Ar when a neutron was transformed into a proton and an electron by the absorption of a neutrino. http://en.wikipedia.org/ ...
Collapse of an unstable Neutron Star to a Black Hole
... star merger process a new supramassive or hypermassive neutron star is formed, which could be stable for longer times or collapse almost immediately to a black hole. During this process a short gamma ray burst is emitted, releasing in less than one second the energy emitted by our Galaxy over one ye ...
... star merger process a new supramassive or hypermassive neutron star is formed, which could be stable for longer times or collapse almost immediately to a black hole. During this process a short gamma ray burst is emitted, releasing in less than one second the energy emitted by our Galaxy over one ye ...
Stellar Astrophysics: Introduction Q. Daniel Wang Astronomy Department University of Massachusetts
... where M is any constant. We then obtain, for example, M αr −1 ...
... where M is any constant. We then obtain, for example, M αr −1 ...
The galactic metallicity gradient Martín Hernández, Nieves Leticia
... in the life of a star is called main sequence. Once the supply of hydrogen is exhausted, the star becomes cooler, larger, and more luminous. Stars like our Sun will eventually eject their outer layers, creating planetary nebulae, and contract to become a white dwarf; highmass stars will die violentl ...
... in the life of a star is called main sequence. Once the supply of hydrogen is exhausted, the star becomes cooler, larger, and more luminous. Stars like our Sun will eventually eject their outer layers, creating planetary nebulae, and contract to become a white dwarf; highmass stars will die violentl ...
X-Ray Binaries
... companion (neutron star, black hole, [white dwarf ]) • traditionally two main classes: high-mass X-ray binaries (HMXBs; M2 > ∼ 10 M¯) and low-mass X-ray binaries (LMXBs; M2 < ∼ 1.5 M¯) . missing intermediate-mass systems? . probably not: most systems classified as LMXBs almost certainly originate fr ...
... companion (neutron star, black hole, [white dwarf ]) • traditionally two main classes: high-mass X-ray binaries (HMXBs; M2 > ∼ 10 M¯) and low-mass X-ray binaries (LMXBs; M2 < ∼ 1.5 M¯) . missing intermediate-mass systems? . probably not: most systems classified as LMXBs almost certainly originate fr ...
5 – Stellar Structure I
... It can thus withstand greater compression without deviating from an ideal gas. Note that an ideal gas demands that the distances between the particles are much greater than their sizes, and nuclear dimension is 10-15 m compared to atomic dimension of 10-10 m Lets revisit the issue of radiation vs ga ...
... It can thus withstand greater compression without deviating from an ideal gas. Note that an ideal gas demands that the distances between the particles are much greater than their sizes, and nuclear dimension is 10-15 m compared to atomic dimension of 10-10 m Lets revisit the issue of radiation vs ga ...
Astronomy 112: The Physics of Stars Class 15 Notes: Stars Before
... the one I just showed can be made. In addition to this molecular line, there are many more that we can use, involving both different transitions of CO and of other molecules – thousands have been detected. These clouds are extremely cold, typically around 10 K, mainly because the CO molecules are v ...
... the one I just showed can be made. In addition to this molecular line, there are many more that we can use, involving both different transitions of CO and of other molecules – thousands have been detected. These clouds are extremely cold, typically around 10 K, mainly because the CO molecules are v ...
Introduction
... in spectrographs were to resolve that line into three lines. One corresponded to hydrogen but the other two remained unknown and it was thought that these two lines originated from a new element, nebulium. The identification of both lines came much later (∼1930), they were from [O III ]. Nowadays, s ...
... in spectrographs were to resolve that line into three lines. One corresponded to hydrogen but the other two remained unknown and it was thought that these two lines originated from a new element, nebulium. The identification of both lines came much later (∼1930), they were from [O III ]. Nowadays, s ...
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.