– 1 – 1. Chemical Evolution 1.1.
... suggests that the Salpeter IMF is too steep to fit the observations for low mass stars below 0.5M⊙ , and that a flatter slope is required, reaching −0.3 ± 0.7 for 0.01 < M/M⊙ < 0.08. Note that the transformation from luminosity to mass (the IMF is a function of stellar mass) is not as well determine ...
... suggests that the Salpeter IMF is too steep to fit the observations for low mass stars below 0.5M⊙ , and that a flatter slope is required, reaching −0.3 ± 0.7 for 0.01 < M/M⊙ < 0.08. Note that the transformation from luminosity to mass (the IMF is a function of stellar mass) is not as well determine ...
MSc Project: A combined fit of neutrino models using astrophysics
... • Will be supported by Prof. Sarah Bridle (Astro) • Include electron-neutrino data, including anomalies, for accelerator/reactor experiments. • Use same statistical methods for both data set (currently not done) • Expand to more than just 3+1 flavour, study impact of various ...
... • Will be supported by Prof. Sarah Bridle (Astro) • Include electron-neutrino data, including anomalies, for accelerator/reactor experiments. • Use same statistical methods for both data set (currently not done) • Expand to more than just 3+1 flavour, study impact of various ...
Document
... stabilized, the luminosity increases. • During this phase, the carbon core develops Decrease of the pressure of the core (molecular weight increases). Expanding of the envelope Evolution to Asymptotic Giant Branch. ...
... stabilized, the luminosity increases. • During this phase, the carbon core develops Decrease of the pressure of the core (molecular weight increases). Expanding of the envelope Evolution to Asymptotic Giant Branch. ...
CHP 14
... b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the supernova explosion that formed them made them spin faster. 3. Although neutron stars are very hot, they are not easy to locate because a. light does not escape from their event ...
... b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the supernova explosion that formed them made them spin faster. 3. Although neutron stars are very hot, they are not easy to locate because a. light does not escape from their event ...
Neutron Stars and Black Holes
... b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the supernova explosion that formed them made them spin faster. 3. Although neutron stars are very hot, they are not easy to locate because a. light does not escape from their event ...
... b. they have high orbital velocities. c. they have high densities. d. they have high temperatures. e. the energy from the supernova explosion that formed them made them spin faster. 3. Although neutron stars are very hot, they are not easy to locate because a. light does not escape from their event ...
Isotopes Tell Origin and Operation of the Sun
... significance of lightweight neon in the solar wind could not be deciphered in 1969, when isotopic anomalies from stellar nuclear reactions and mass fractionation were not resolved, decay products of only two extinct nuclides had been found in meteorites [4, 5], and it was still widely believed that ...
... significance of lightweight neon in the solar wind could not be deciphered in 1969, when isotopic anomalies from stellar nuclear reactions and mass fractionation were not resolved, decay products of only two extinct nuclides had been found in meteorites [4, 5], and it was still widely believed that ...
ms
... comparing the luminosity function and color-magnitude diagrams with a reference cluster, 47 Tucanae. They found a distance of 8.2 ± 0.6 kpc, which is consistent with the earlier measurement but has an improved uncertainty, and where the quoted error takes into account the systematic uncertainties in ...
... comparing the luminosity function and color-magnitude diagrams with a reference cluster, 47 Tucanae. They found a distance of 8.2 ± 0.6 kpc, which is consistent with the earlier measurement but has an improved uncertainty, and where the quoted error takes into account the systematic uncertainties in ...
Transcript - Chandra X
... ~50,000 years old as the materials becomes more and more tenuous over time as they spread into the interstellar medium. Eventually the white dwarf remains as the stellar core end product. If the white dwarf is in a multiple star system and a companion star evolves into a red giant then the white dwa ...
... ~50,000 years old as the materials becomes more and more tenuous over time as they spread into the interstellar medium. Eventually the white dwarf remains as the stellar core end product. If the white dwarf is in a multiple star system and a companion star evolves into a red giant then the white dwa ...
Astronomy 112: The Physics of Stars Class 16 Notes: Post
... the Schönberg-Chandrasekhar limit. This does not stop it from heating up, but it does change what happens once the He ignites. Recall our discussion of runaway nuclear burning instability. In a degenerate gas, the pressure and density are not connected to the temperature. As a result, once a nuclea ...
... the Schönberg-Chandrasekhar limit. This does not stop it from heating up, but it does change what happens once the He ignites. Recall our discussion of runaway nuclear burning instability. In a degenerate gas, the pressure and density are not connected to the temperature. As a result, once a nuclea ...
electron degeneracy pressure and white dwarfs
... Confinement of elementary particles (continued) This confinement has to do not only with the electric repulsion they may experience; there is an additional quantum-mechanical repulsion of electrons by each other, which sets in at very small distances, such that wave properties are displayed. If t ...
... Confinement of elementary particles (continued) This confinement has to do not only with the electric repulsion they may experience; there is an additional quantum-mechanical repulsion of electrons by each other, which sets in at very small distances, such that wave properties are displayed. If t ...
Radiation from Proxima Centauri
... Sketch a graph on the same axes to show how the spectrum of a star with a slightly higher temperature would appear. ...
... Sketch a graph on the same axes to show how the spectrum of a star with a slightly higher temperature would appear. ...
New Frontiers in Nuclear Physics Kai Hebeler (OSU)
... • small resolution dependence indicates converged calculation • energy sensitive to uncertainties in 3N interaction • variation due to 3N input uncertainty much larger than resolution dependence • good agreement with other approaches (different NN interactions) ...
... • small resolution dependence indicates converged calculation • energy sensitive to uncertainties in 3N interaction • variation due to 3N input uncertainty much larger than resolution dependence • good agreement with other approaches (different NN interactions) ...
Is $^ 6$ Li in metal-poor halo stars produced in situ by solar
... studies, because the reaction 4 He(3 He, p)6 Li was not taken into account. Second, it is very likely that most halo stars were much more active in their youth than the contemporary Sun. Indeed stellar rotation being the decisive factor of solar-like activity of dwarf stars, magnetic braking during ...
... studies, because the reaction 4 He(3 He, p)6 Li was not taken into account. Second, it is very likely that most halo stars were much more active in their youth than the contemporary Sun. Indeed stellar rotation being the decisive factor of solar-like activity of dwarf stars, magnetic braking during ...
Chapter 14 – Chemical Analysis
... At what line strength do lines become sensitive to microturbulence? Why is it hard to determine abundances from lines on the “flat part” of the curve of growth? ...
... At what line strength do lines become sensitive to microturbulence? Why is it hard to determine abundances from lines on the “flat part” of the curve of growth? ...
Stellar Physics 1
... Stellar Physics 1 14. Which of the following statements is true about eclipsing binary systems? A. A secondary maximum occurs when a smaller star eclipses a larger star. B. A primary minimum occurs when a smaller star eclipses a larger one. C. A secondary minimum occurs when a smaller star eclipses ...
... Stellar Physics 1 14. Which of the following statements is true about eclipsing binary systems? A. A secondary maximum occurs when a smaller star eclipses a larger star. B. A primary minimum occurs when a smaller star eclipses a larger one. C. A secondary minimum occurs when a smaller star eclipses ...
Low-Mass Star Formation Triggered by Supernova in Primordial
... low temperature gas ⇒ small Jeans mass ⇒ low mass star formation In early Universe (no dust, no metal), the gas cools to about 300-500K ...
... low temperature gas ⇒ small Jeans mass ⇒ low mass star formation In early Universe (no dust, no metal), the gas cools to about 300-500K ...
Slide 1
... Previous star formation can trigger further star formation through: b) Ionization fronts of hot, massive O or B stars which produce a lot of UV radiation: Massive stars die young => O and B stars only exist near sites of recent star formation ...
... Previous star formation can trigger further star formation through: b) Ionization fronts of hot, massive O or B stars which produce a lot of UV radiation: Massive stars die young => O and B stars only exist near sites of recent star formation ...
The figure below shows what scientists over 1000 years ago thought
... The Moon takes a longer time than any of the other satellites to orbit the Earth. Give one other way in which the Moon is different from the other satellites in the table. ...
... The Moon takes a longer time than any of the other satellites to orbit the Earth. Give one other way in which the Moon is different from the other satellites in the table. ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.