supernova remnants: a link between massive stars and the
... disruption of a carbon-oxygen white dwarf that has been accreting matter from a non-degenerate companion star, a donor that survives the explosion (see Branch 2001 for a review of current models for low mass SNe). Massive stars, on the other hand, presumably evolve from the main sequence to red gian ...
... disruption of a carbon-oxygen white dwarf that has been accreting matter from a non-degenerate companion star, a donor that survives the explosion (see Branch 2001 for a review of current models for low mass SNe). Massive stars, on the other hand, presumably evolve from the main sequence to red gian ...
Rogava_Course_-_First_lecture
... impact on each other, stars essentially evolve separately. • Semidetached binary stars: one of the components fills its Roche lobe and the other does not. Gas from the surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evo ...
... impact on each other, stars essentially evolve separately. • Semidetached binary stars: one of the components fills its Roche lobe and the other does not. Gas from the surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evo ...
A Brief Overview of Atomic Structure
... Atomic mass units (amu) are convenient units to use when dealing with extremely small masses of individual atoms. ...
... Atomic mass units (amu) are convenient units to use when dealing with extremely small masses of individual atoms. ...
Part 1: If a 10000 K blackbody has a wavelength of peak emission at
... NO – spectral types are measured from absorption line spectra (hence the name spectral type) in the same way you did for Homework 3. ...
... NO – spectral types are measured from absorption line spectra (hence the name spectral type) in the same way you did for Homework 3. ...
O_2 Theory (III) TUNNELING BENEATH THE He* FRAGMENTATION ENERGY
... The key to the mechanism is the lochons, which during the collision process attain significant energy from the nuclear Coulomb potential (many keV; but, being tightly bound in ground states, they do not radiate). During the fusion process, they would divide and can perhaps attain energies in the MeV ...
... The key to the mechanism is the lochons, which during the collision process attain significant energy from the nuclear Coulomb potential (many keV; but, being tightly bound in ground states, they do not radiate). During the fusion process, they would divide and can perhaps attain energies in the MeV ...
Document
... a superwind. The mechanisms behind superwinds are not very well understood. However, we know that they exist from observational evidence (the rate of mass loss can be observed). ...
... a superwind. The mechanisms behind superwinds are not very well understood. However, we know that they exist from observational evidence (the rate of mass loss can be observed). ...
Slide 1
... more stars in a region only 30 light years across, which suggests that all the stars were born in a single episode of star formation. Based on optical properties such as brightness and color some of the normal stars in the cluster are known to have masses of about 40 suns. ...
... more stars in a region only 30 light years across, which suggests that all the stars were born in a single episode of star formation. Based on optical properties such as brightness and color some of the normal stars in the cluster are known to have masses of about 40 suns. ...
Effects of triple-α and C(α, γ )16 O reaction rates on the supernova
... The triple-α and 12 C(α, γ )16 O rates are the key nuclear reaction rates concerning He-burning in massive star evolution. As a consequence, explosive nucleosynthesis and the resulting supernova yields of a massive star would be influenced seriously by the two rates. We select four combinations from ...
... The triple-α and 12 C(α, γ )16 O rates are the key nuclear reaction rates concerning He-burning in massive star evolution. As a consequence, explosive nucleosynthesis and the resulting supernova yields of a massive star would be influenced seriously by the two rates. We select four combinations from ...
Neutron Stars, first class
... 9 Msun and a not well determined mass, 30-40 Msun (depending, for example the star metallicity) ...
... 9 Msun and a not well determined mass, 30-40 Msun (depending, for example the star metallicity) ...
Physics116_L42
... evolution of the Universe) work - but this concept came from studies of Grand Unified Theories (GUTs) of particle physics Our Universe may be just one bubble in a foam of other universes… The net energy of the Universe could be zero and our Universe could be just a quantum fluctuation which has not ...
... evolution of the Universe) work - but this concept came from studies of Grand Unified Theories (GUTs) of particle physics Our Universe may be just one bubble in a foam of other universes… The net energy of the Universe could be zero and our Universe could be just a quantum fluctuation which has not ...
Life Cycle of a Star
... core temperature rises to a point where fuel is used up • A carbon-oxygen core forms • Eventually the gases at a star’s surface begin to blow ...
... core temperature rises to a point where fuel is used up • A carbon-oxygen core forms • Eventually the gases at a star’s surface begin to blow ...
Дубовиченко С
... The astrophysical S-factor, which determines the reaction cross-section, is the main characteristic of any thermonuclear reaction in the Sun and the stars of our Universe, i.e. it defines the probability of the reaction behavior at very low energies [1]. The astrophysical Sfactor may be obtained exp ...
... The astrophysical S-factor, which determines the reaction cross-section, is the main characteristic of any thermonuclear reaction in the Sun and the stars of our Universe, i.e. it defines the probability of the reaction behavior at very low energies [1]. The astrophysical Sfactor may be obtained exp ...
Dynamics of nuclear burning during type-I X-ray bursts 1. 2. 3.
... •Conduction: too slow (100 cm/s) •Convection: convective speed 5x106cm/s 1) Front width = scaleheight; ...
... •Conduction: too slow (100 cm/s) •Convection: convective speed 5x106cm/s 1) Front width = scaleheight; ...
Galactic chemical evolution of heavy elements: from Barium to
... Sneden et al. 1998). For the elements considered here, we make the simplifying hypothesis that their r-contributions in the solar system can be considered of primary origin (i.e. with yields independent of the initial stellar metallicity). Hence, after the s-contributions at the epoch of the solar f ...
... Sneden et al. 1998). For the elements considered here, we make the simplifying hypothesis that their r-contributions in the solar system can be considered of primary origin (i.e. with yields independent of the initial stellar metallicity). Hence, after the s-contributions at the epoch of the solar f ...
Slide 1
... Superbubbles, and the Source of Cosmic Rays” 2005, ApJ, 268, 738 Ikeuchi, S. “Evolution of Evolution of Superbubbles” 1998, LNP, 506, 399 Mac Low, M.M. & McCray, R. “Superbubbles in disk galaxies”, 1988, ApJ, 324, 776 Maiz-Apellaniz, J. “The Origin of the Local Bubble” 2001, ApJ, 560, L86 Oey, M.S. ...
... Superbubbles, and the Source of Cosmic Rays” 2005, ApJ, 268, 738 Ikeuchi, S. “Evolution of Evolution of Superbubbles” 1998, LNP, 506, 399 Mac Low, M.M. & McCray, R. “Superbubbles in disk galaxies”, 1988, ApJ, 324, 776 Maiz-Apellaniz, J. “The Origin of the Local Bubble” 2001, ApJ, 560, L86 Oey, M.S. ...
The Mass-Radius Relation for Polytropes The mass within any point
... Note what this means: for a polytropic index of 3/2 (the γ = 5/3 case), R ∝ M−1/3 . Thus, for a set of stars with the same K and n (i.e., white dwarfs, or a fully convective star that is undergoing mass transfer), the stellar radius is inversely proportional to the mass. Equation (16.1.4) can also b ...
... Note what this means: for a polytropic index of 3/2 (the γ = 5/3 case), R ∝ M−1/3 . Thus, for a set of stars with the same K and n (i.e., white dwarfs, or a fully convective star that is undergoing mass transfer), the stellar radius is inversely proportional to the mass. Equation (16.1.4) can also b ...
Powerpoint - Physics and Astronomy
... b) repeated helium fusion flashes in red giants. c) rapid collapse of a protostar into a massive O star. d) the explosion of a low-mass star. e) the birth of a massive star in a new cluster. Explanation: Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for ...
... b) repeated helium fusion flashes in red giants. c) rapid collapse of a protostar into a massive O star. d) the explosion of a low-mass star. e) the birth of a massive star in a new cluster. Explanation: Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for ...
A model of low-mass neutron stars with a quark core
... The table lists the basic parameters of critical configurations a, b, c, d, e, f (Mcore and Rcore are the core mass and radius, respectively). Also given here is the packing factor α. For all critical configurations, this quantity is positive and (except for configuration f ) of the same order of magni ...
... The table lists the basic parameters of critical configurations a, b, c, d, e, f (Mcore and Rcore are the core mass and radius, respectively). Also given here is the packing factor α. For all critical configurations, this quantity is positive and (except for configuration f ) of the same order of magni ...
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.