mass-luminosity relationship
... 2) If m1 is much larger than m2, what is the total kinetic energy of the system and which mass has all the kinetic energy? Since K = ½mv2 and m ~ m2, K = ½m2v2 and the smaller mass has all the kinetic energy (it is the only thing moving) ...
... 2) If m1 is much larger than m2, what is the total kinetic energy of the system and which mass has all the kinetic energy? Since K = ½mv2 and m ~ m2, K = ½m2v2 and the smaller mass has all the kinetic energy (it is the only thing moving) ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
... the star, but in the extreme conditions that are now present in the core, the stellar material becomes opaque even to neutrinos, and these may give a push to the shock wave such that it gains momentum and continues outward. The shock wave eventually reaches the stellar surface after a few hours, at ...
... the star, but in the extreme conditions that are now present in the core, the stellar material becomes opaque even to neutrinos, and these may give a push to the shock wave such that it gains momentum and continues outward. The shock wave eventually reaches the stellar surface after a few hours, at ...
The Science of Life in the Universe (Chap 2
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
Page R63 - ClassZone
... The Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram is a graph that shows stars plotted according to brightness and surface temperature. Most stars fall within a diagonal band called the main sequence. In the mainsequence stage of a star’s life cycle, brightness is closely related ...
... The Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram is a graph that shows stars plotted according to brightness and surface temperature. Most stars fall within a diagonal band called the main sequence. In the mainsequence stage of a star’s life cycle, brightness is closely related ...
Stellar Metamorphosis
... gases (Hydrogen, Helium, Methane ) its atmosphere starts thinning and also evaporation causes loss of surface liquids by this process. There was more water on earth in earlier phases than now and the earth’s water constantly recirculates through its atmosphere via evaporation. During this cooling p ...
... gases (Hydrogen, Helium, Methane ) its atmosphere starts thinning and also evaporation causes loss of surface liquids by this process. There was more water on earth in earlier phases than now and the earth’s water constantly recirculates through its atmosphere via evaporation. During this cooling p ...
The Science of Life in the Universe (Chap 2
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
Stars
... distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
... distance of each star from the center of mass yields the ratio of the masses. •The ratio and sum provide each mass individually. ...
Chapter 3 Notes
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
... thermostat from 300 Kelvin to 1200 Kelvin, how much more energy will be required to heat the chamber? A 64 times B 256 times C 4 times D 81 times E 16 times ...
The First Stars in the Universe - Scientific American
... cannot cool the gas below 200 kelvins, making this a lower limit to the temperature of the first star-forming clumps. Another is that the cooling from molecular hydrogen becomes inefficient at the higher densities encountered when the clumps begin to collapse. At these densities the hydrogen molecul ...
... cannot cool the gas below 200 kelvins, making this a lower limit to the temperature of the first star-forming clumps. Another is that the cooling from molecular hydrogen becomes inefficient at the higher densities encountered when the clumps begin to collapse. At these densities the hydrogen molecul ...
Earth
... •To produce elements heavier than Fe, enormous amounts of energy are needed which is thought to derive solely from the cataclysmic explosions of supernovae. •In the supernova explosion, a large flux of energetic neutrons is produced and nuclei bombarded by these neutrons build up mass one unit at a ...
... •To produce elements heavier than Fe, enormous amounts of energy are needed which is thought to derive solely from the cataclysmic explosions of supernovae. •In the supernova explosion, a large flux of energetic neutrons is produced and nuclei bombarded by these neutrons build up mass one unit at a ...
Exercises
... i. Summarize your results for the questions above by computing the nuclear, thermal and dynamical timescales for a 1, 10 and 25 M main-sequence star. Put your answers in tabular form. ii. For each of the following evolutionary stages indicate on which timescale they occur: premain sequence contract ...
... i. Summarize your results for the questions above by computing the nuclear, thermal and dynamical timescales for a 1, 10 and 25 M main-sequence star. Put your answers in tabular form. ii. For each of the following evolutionary stages indicate on which timescale they occur: premain sequence contract ...
Answers to Coursebook questions – Chapter E5
... A one solar mass star would evolve to become a red giant. As the star expands in size into the red giant stage, nuclear reactions inside the core of the star are able to produce heavier elements than helium because the temperature of the core is sufficiently high. The red giant star will explode as ...
... A one solar mass star would evolve to become a red giant. As the star expands in size into the red giant stage, nuclear reactions inside the core of the star are able to produce heavier elements than helium because the temperature of the core is sufficiently high. The red giant star will explode as ...
Answers
... like star has become a red giant. In a sun-like star, fusion stops at this point once the 4He has been exhausted, leaving a high temperature, degenerate core as a white dwarf star. The timescale of helium fusion in a sun-like star is about 10% of the hydrogen burning phase, for the sun about 109 yea ...
... like star has become a red giant. In a sun-like star, fusion stops at this point once the 4He has been exhausted, leaving a high temperature, degenerate core as a white dwarf star. The timescale of helium fusion in a sun-like star is about 10% of the hydrogen burning phase, for the sun about 109 yea ...
Name Physics 130 Astronomy Exam 2 August 2, 2004 Multiple Choice
... b.) We don’t know, since their lifetimes are longer than the age of the universe. c.) They explode d.) They gradually shrink to the size of the Earth. 28. _____ The major source of energy in the pre-main-sequence life of the Sun was a.) nuclear fusion. b.) gravitational c.) nuclear fusion d.) burnin ...
... b.) We don’t know, since their lifetimes are longer than the age of the universe. c.) They explode d.) They gradually shrink to the size of the Earth. 28. _____ The major source of energy in the pre-main-sequence life of the Sun was a.) nuclear fusion. b.) gravitational c.) nuclear fusion d.) burnin ...
Galaxies
... to label galaxy types. • E: elliptical galaxy; the number indicates how stretched out the shape is. • S (or SA): regular spiral galaxy; SB: barred spiral galaxy; the small letter indicates how spread out the arms are. ...
... to label galaxy types. • E: elliptical galaxy; the number indicates how stretched out the shape is. • S (or SA): regular spiral galaxy; SB: barred spiral galaxy; the small letter indicates how spread out the arms are. ...
Death of Stars notes
... • The SOFIA finding demonstrates that supernovas not only produce dust, but that the dust can survive the explosion to become raw material for the formation of other stars—and planets. • This result supports the notion that most of the dust observed in distant young galaxies may have been made by su ...
... • The SOFIA finding demonstrates that supernovas not only produce dust, but that the dust can survive the explosion to become raw material for the formation of other stars—and planets. • This result supports the notion that most of the dust observed in distant young galaxies may have been made by su ...
How is a Star`s Color Related to Its temperature?
... On a clear night you have surely noticed that some stars are brighter than cthers. But stars also have different colors. Rigel is blue. and Betelgense is red. Capella and ore" Sun are yellow, in this activity you will make your own Hertzsprung-Russell diagram. You will see how star brightness, color ...
... On a clear night you have surely noticed that some stars are brighter than cthers. But stars also have different colors. Rigel is blue. and Betelgense is red. Capella and ore" Sun are yellow, in this activity you will make your own Hertzsprung-Russell diagram. You will see how star brightness, color ...
PDF of story and photos
... picture of star formation. In stellar nurseries, many stars often form in the same cloud of gas and dust. The biggest stars begin producing light before the smaller stars. This means that the energy released by the biggest stars can affect the smaller, still-forming stars that are near the big stars ...
... picture of star formation. In stellar nurseries, many stars often form in the same cloud of gas and dust. The biggest stars begin producing light before the smaller stars. This means that the energy released by the biggest stars can affect the smaller, still-forming stars that are near the big stars ...
On the importance of nucleation for the formation of quark cores
... is formed. (F. Weber, 2000) ...
... is formed. (F. Weber, 2000) ...
Comparison of low- and high-mass star formation
... to be near virial equilibrium, after accounting for clump envelope. Possibly slightly sub-virial; or have stronger The Turbulent Core Model does not make any prediction about the timescale for the B-fields. But we need a larger sample - massive starless cores are rare! cores to assemble, except that ...
... to be near virial equilibrium, after accounting for clump envelope. Possibly slightly sub-virial; or have stronger The Turbulent Core Model does not make any prediction about the timescale for the B-fields. But we need a larger sample - massive starless cores are rare! cores to assemble, except that ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.