Svoboda, PPTX, 14 MB
... 2. What energy resolution is required to see scientifically interesting features? What would be the scientific loss if resolution were 30% versus 10% versus 3%? Note that time, money, and engineering effort to achieve such precise energy information is decidedly non-linear in the required precision. ...
... 2. What energy resolution is required to see scientifically interesting features? What would be the scientific loss if resolution were 30% versus 10% versus 3%? Note that time, money, and engineering effort to achieve such precise energy information is decidedly non-linear in the required precision. ...
1 - Physics
... • B) both take the same length of time to form • C) mass of the sun • D) the formation rates will depend on the rotation of the gas clouds 7. Of the following, which is the most important factor that causes fusion in the cores of stars to be highly dependant on the temperature of the core? • A) beca ...
... • B) both take the same length of time to form • C) mass of the sun • D) the formation rates will depend on the rotation of the gas clouds 7. Of the following, which is the most important factor that causes fusion in the cores of stars to be highly dependant on the temperature of the core? • A) beca ...
Astronomy Club
... nearly half of what is predicted from standard stellar physics. This thirty-year mystery persists in the deficit of about a half in the numbers of neutrinos detected compared to expectations, the socalled "Solar Neutrino Problem". All kinds of ideas came up to explain this puzzle and perhaps more th ...
... nearly half of what is predicted from standard stellar physics. This thirty-year mystery persists in the deficit of about a half in the numbers of neutrinos detected compared to expectations, the socalled "Solar Neutrino Problem". All kinds of ideas came up to explain this puzzle and perhaps more th ...
astronomy - Mr. Barnard
... (2) neutron star (4) white dwarf ____5. The explosion of a massive star near the end of its life is known as a (1) nebula (3) nova (2) supernova (4) pulsar ____6. According to our present theories of stellar evolution, our sun will change next into (1) a white dwarf (3) a red giant (2) a black hole ...
... (2) neutron star (4) white dwarf ____5. The explosion of a massive star near the end of its life is known as a (1) nebula (3) nova (2) supernova (4) pulsar ____6. According to our present theories of stellar evolution, our sun will change next into (1) a white dwarf (3) a red giant (2) a black hole ...
The Science of Sunshine
... together. The released energy travels upwards from the core until it eventually escapes the Sun’s surface. It is a long journey, about 700,000 km, or almost twice the distance from the Earth to the Moon. Once it leaves the Sun’s surface most of it shines outwards into empty space but after a journey ...
... together. The released energy travels upwards from the core until it eventually escapes the Sun’s surface. It is a long journey, about 700,000 km, or almost twice the distance from the Earth to the Moon. Once it leaves the Sun’s surface most of it shines outwards into empty space but after a journey ...
What Are Sunspots?
... coal gives us energy for our cars and heating our homes. But the sun's energy doesn't come from burning fuels. The sun's energy comes from nuclear fusion. The nuclei (plural form of nucleus) of different atoms of gases in the sun fuse or join together. Most of the sun's fusion happens when atoms of ...
... coal gives us energy for our cars and heating our homes. But the sun's energy doesn't come from burning fuels. The sun's energy comes from nuclear fusion. The nuclei (plural form of nucleus) of different atoms of gases in the sun fuse or join together. Most of the sun's fusion happens when atoms of ...
Lecture 15 - Deaths of Stars, Supernovae
... • Star burns up rest of hydrogen • Nothing remains but degenerate core of Oxygen and Carbon • “White dwarf” cools but does not contract because core is degenerate • No energy from fusion, no energy from gravitational contraction • White dwarf slowly fades away… ...
... • Star burns up rest of hydrogen • Nothing remains but degenerate core of Oxygen and Carbon • “White dwarf” cools but does not contract because core is degenerate • No energy from fusion, no energy from gravitational contraction • White dwarf slowly fades away… ...
The Future Sun
... stars than Pleiades. b. Most stars are one the main sequence. c. Perseus has small range of luminosity d. Some clusters have giants. ...
... stars than Pleiades. b. Most stars are one the main sequence. c. Perseus has small range of luminosity d. Some clusters have giants. ...
Powerpoint
... represents the transition of an ordinary star into a neutron star consisting mainly of neutrons. Such a star may possess a very small radius and an extremely high density. As neutrons can be packed much more closely than ordinary nuclei and electrons, the gravitational packing energy in a cold neutr ...
... represents the transition of an ordinary star into a neutron star consisting mainly of neutrons. Such a star may possess a very small radius and an extremely high density. As neutrons can be packed much more closely than ordinary nuclei and electrons, the gravitational packing energy in a cold neutr ...
Great Migrations & other natural history tales
... to with a factor of 10) from the equations governing the structure of a star. These equations are typically ODEs (ordinary differential eqs.) that contain terms like dP/dr This derivative can be estimated as dP/dr ~ [P(R) - P(0)]/(R - 0) Notice that this would be an exact expression for the derivati ...
... to with a factor of 10) from the equations governing the structure of a star. These equations are typically ODEs (ordinary differential eqs.) that contain terms like dP/dr This derivative can be estimated as dP/dr ~ [P(R) - P(0)]/(R - 0) Notice that this would be an exact expression for the derivati ...
AND STARS! The Sun s Source of Energy E= m c
... to expand. The energy would eventually be radiated off into space and the Sun would return to normal size. 4) The injected energy would heat the core, causing the Sun to expand. The Sun would find a new equilibrium with the gravitational pressure and end up being larger in size. ...
... to expand. The energy would eventually be radiated off into space and the Sun would return to normal size. 4) The injected energy would heat the core, causing the Sun to expand. The Sun would find a new equilibrium with the gravitational pressure and end up being larger in size. ...
Timescales of stellar evolution 1. Dynamical time scale Measure of
... fuel if it keeps burning it at the current rate: Energy release from fusing one gram of hydrogen to helium is 6 x 1018 erg, so: ...
... fuel if it keeps burning it at the current rate: Energy release from fusing one gram of hydrogen to helium is 6 x 1018 erg, so: ...
Winning Entries in this week’s Galaxy
... • Further H, He falls in at specified rate. • Follow evolution of individual elements C, for the getH,aHe, feel N, O, Ne, Mg, Si, S, Ar, Ca and Fe. problem. ...
... • Further H, He falls in at specified rate. • Follow evolution of individual elements C, for the getH,aHe, feel N, O, Ne, Mg, Si, S, Ar, Ca and Fe. problem. ...
1_Introduction
... That’s 4.5 million times what you’d get by burning the hydrogen. Sun’s hydrogen supply adequate for billions, not thousands, of years. ...
... That’s 4.5 million times what you’d get by burning the hydrogen. Sun’s hydrogen supply adequate for billions, not thousands, of years. ...
Document
... Total luminosity is about 4 × 1026 W—the equivalent of 10 billion 1-megaton nuclear bombs per second. ...
... Total luminosity is about 4 × 1026 W—the equivalent of 10 billion 1-megaton nuclear bombs per second. ...