Convection in stellar envelopes: a changing paradigm
... is neutrally buoyant. It flows towards the boundaries to replace the mass flowing in the threads, rather than being driven there by convective buoyancy. Convection in a cell at high Ra is therefore as non-local as it can possibly be: the heat flux is carried by flows that maintain their identity fro ...
... is neutrally buoyant. It flows towards the boundaries to replace the mass flowing in the threads, rather than being driven there by convective buoyancy. Convection in a cell at high Ra is therefore as non-local as it can possibly be: the heat flux is carried by flows that maintain their identity fro ...
Gamma - Ray Observations of Olaf Reimer
... X-Ray Binaries as Gamma-Ray Sources Binary systems of a compact object (neutron star or black hole) and a stellar companion Matter is flowing over from the stellar companion onto the compact object. Angular momentum conservation => Formation of an accretion disk Matter in the accretion disk heats u ...
... X-Ray Binaries as Gamma-Ray Sources Binary systems of a compact object (neutron star or black hole) and a stellar companion Matter is flowing over from the stellar companion onto the compact object. Angular momentum conservation => Formation of an accretion disk Matter in the accretion disk heats u ...
Estimating the total radiative power output from the hot outer layers
... see for example Doyle et al. 1989). This has the e ect of diminishing errors in abundances as the radiative loss function is `almost' the inverse of the EM curve. Throughout, we used the radiative loss function of Cook et al. (1990) which was derived using the same solar abundance as used here. A su ...
... see for example Doyle et al. 1989). This has the e ect of diminishing errors in abundances as the radiative loss function is `almost' the inverse of the EM curve. Throughout, we used the radiative loss function of Cook et al. (1990) which was derived using the same solar abundance as used here. A su ...
X-ray emission from supernova shock waves Tanja Kramer Nymark Department of Astronomy
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
The Korean 1592--1593 Record of a Guest Star: Animpostor`of the
... (1967) and Chu (1968) independently proposed that it might have been the Cas A SN event. On the other hand, Stephenson & Yau (1987) (see also Stephenson & Green 2002, for a summary), who studied this Korean record in detail, concluded that not only the date but also the positional agreement between ...
... (1967) and Chu (1968) independently proposed that it might have been the Cas A SN event. On the other hand, Stephenson & Yau (1987) (see also Stephenson & Green 2002, for a summary), who studied this Korean record in detail, concluded that not only the date but also the positional agreement between ...
How Massive Single Stars End Their Life - TigerPrints
... neutron star, fallback black hole, and direct black hole formation. For very massive stars, the remnant of the collapsing star depends sensitively on the metallicity. Above 40 M, low-metallicity stars form black holes directly, while at higher metallicities, black holes of smaller mass are produced ...
... neutron star, fallback black hole, and direct black hole formation. For very massive stars, the remnant of the collapsing star depends sensitively on the metallicity. Above 40 M, low-metallicity stars form black holes directly, while at higher metallicities, black holes of smaller mass are produced ...
The chemical composition of TS 01, the most oxygen
... in PNe cannot be used for TS 01, since the electron temperature cannot be determined directly from observations. To go further in the abundance determination of TS 01 required an estimate of the effective temperature of the central star. One way is to obtain a good blue spectrum of the PN, and use th ...
... in PNe cannot be used for TS 01, since the electron temperature cannot be determined directly from observations. To go further in the abundance determination of TS 01 required an estimate of the effective temperature of the central star. One way is to obtain a good blue spectrum of the PN, and use th ...
Particle-in-cell simulation study of single and multispecies
... particles is non-relativistic. These fields are then Lorentztransformed to the laboratory frame [8]. The equations of motion of macroparticles of each species are integrated using a second order leap-frog method [1]. The transverse calculation region is divided into n x n y uniform rectangular mes ...
... particles is non-relativistic. These fields are then Lorentztransformed to the laboratory frame [8]. The equations of motion of macroparticles of each species are integrated using a second order leap-frog method [1]. The transverse calculation region is divided into n x n y uniform rectangular mes ...
Study Systematics on the ICM metallicity measurements
... weak emission compared to the continuum IS NOT A SOLID AND ROBUST ESTIMATE Iron estimate for systems of 2-3 keV can likely be biased towards higher values since this is a critical temperature range where we mix together plasma presenting either strong Fe-L or strong Fe-K lines. ...
... weak emission compared to the continuum IS NOT A SOLID AND ROBUST ESTIMATE Iron estimate for systems of 2-3 keV can likely be biased towards higher values since this is a critical temperature range where we mix together plasma presenting either strong Fe-L or strong Fe-K lines. ...
The significant contribution of minor mergers to the cosmic star
... We estimate an empirical lower limit for the fraction of cosmic star formation that is triggered by minor mergers in the local Universe. Splitting the star-formation budget by galaxy morphology, we find that early-type galaxies (ETGs) host ∼14% of the budget, while Sb/Sc galaxies host the bulk (∼53% ...
... We estimate an empirical lower limit for the fraction of cosmic star formation that is triggered by minor mergers in the local Universe. Splitting the star-formation budget by galaxy morphology, we find that early-type galaxies (ETGs) host ∼14% of the budget, while Sb/Sc galaxies host the bulk (∼53% ...
Matter and antimatter in the same universe?
... There are still several problems in the inflationary model related to the exact definition of the energy density function (Coleman-Weinberg) describing the Higgs fields in order to obtain a proper phase transition; moreover, it is probably in the framework of a new class of superunification theories ...
... There are still several problems in the inflationary model related to the exact definition of the energy density function (Coleman-Weinberg) describing the Higgs fields in order to obtain a proper phase transition; moreover, it is probably in the framework of a new class of superunification theories ...
Differentially-rotating neutron star models with a parametrized
... hole or another type of compact star (quark star, hybrid star). This may lead to a unique signal either of neutrinos or gravitational waves from the supernova. An exciting way in which a neutron star’s life can end by spiralling into and consequently merging with a binary companion. Numerical relati ...
... hole or another type of compact star (quark star, hybrid star). This may lead to a unique signal either of neutrinos or gravitational waves from the supernova. An exciting way in which a neutron star’s life can end by spiralling into and consequently merging with a binary companion. Numerical relati ...
Observing Stellar Evolution
... When they run out of heat and they become a black dwarf. High mass stars (more than 8 solar masses)… Live fast die young. They may remain on main sequence only a few million years. They go through many phases of evolution quickly, creating heaver elements as they go. When the core becomes iron, they ...
... When they run out of heat and they become a black dwarf. High mass stars (more than 8 solar masses)… Live fast die young. They may remain on main sequence only a few million years. They go through many phases of evolution quickly, creating heaver elements as they go. When the core becomes iron, they ...
Here - HESPERIA
... Solar energetic particles (SEPs), especially protons and heavy ions, are a major space weather hazard when they impact spacecraft and the terrestrial atmosphere. Forecasting schemes have been developed, which use earlier signatures of particle acceleration to predict the arrival of solar protons and ...
... Solar energetic particles (SEPs), especially protons and heavy ions, are a major space weather hazard when they impact spacecraft and the terrestrial atmosphere. Forecasting schemes have been developed, which use earlier signatures of particle acceleration to predict the arrival of solar protons and ...
Kathy Geise `08 - DU Portfolio
... Optical Depth The motion of a photon through a gas follows a random walk because individual photons are repeatedly scattered in random directions after encountering gas particles. Emission is any process that adds photons to a beam of light and includes scattering photons into the beam as well as em ...
... Optical Depth The motion of a photon through a gas follows a random walk because individual photons are repeatedly scattered in random directions after encountering gas particles. Emission is any process that adds photons to a beam of light and includes scattering photons into the beam as well as em ...
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.