Recycling strange stars to millisecond periods
... electron layer to be traversed (implying therefore higher energy loss). All in all, infalling protons (or more generally – nuclei) are not able to penetrate the Coulomb barrier, and one expects a gradual building-up of a normal-matter envelope (crust) on the top of the strange matter surface. The bo ...
... electron layer to be traversed (implying therefore higher energy loss). All in all, infalling protons (or more generally – nuclei) are not able to penetrate the Coulomb barrier, and one expects a gradual building-up of a normal-matter envelope (crust) on the top of the strange matter surface. The bo ...
On the origin of the fast solar wind in polar coronal funnels
... compressed state in the convection zone) to expand initially and to become finally homogeneous in the corona. The solar wind flows through this funnel structure, which is described by the magnetic field, and exactly follows the magnetic field lines. Given a mechanical wave energy input at the bottom ...
... compressed state in the convection zone) to expand initially and to become finally homogeneous in the corona. The solar wind flows through this funnel structure, which is described by the magnetic field, and exactly follows the magnetic field lines. Given a mechanical wave energy input at the bottom ...
18. Formation of Stars.
... • The evolution of a protostar can be followed on the H-R diagram. The early protostar is relatively cool and low luminosity. So, the star first appears on the extreme lower right portion of the H-R diagram. • The protostar's initial free-fall contraction is slowed by the increasing density a ...
... • The evolution of a protostar can be followed on the H-R diagram. The early protostar is relatively cool and low luminosity. So, the star first appears on the extreme lower right portion of the H-R diagram. • The protostar's initial free-fall contraction is slowed by the increasing density a ...
Cosmology - RHIG - Wayne State University
... total mass by the mass of a typical star (e.g., 1 solar mass). The result is about 200 billion stars! The actual number of stars could be several tens of billions less or more than this approximate value. ...
... total mass by the mass of a typical star (e.g., 1 solar mass). The result is about 200 billion stars! The actual number of stars could be several tens of billions less or more than this approximate value. ...
transparencies
... • R-modes vary the pressure and densities of the various particles. Beta equilibrium is lost. • Reactions between different particles drive the system back to the equilibrium with a delay depending on the characteristic time scale of the interaction. • Bulk viscosity is dominated by the processes ha ...
... • R-modes vary the pressure and densities of the various particles. Beta equilibrium is lost. • Reactions between different particles drive the system back to the equilibrium with a delay depending on the characteristic time scale of the interaction. • Bulk viscosity is dominated by the processes ha ...
Santilli’s New Fuels as Sources of Clean Combustion
... simplest nucleus of deuterium: The spin 1 of deuterium since quantum axioms require that the single stable bound state of two particles with spin ½, (proton and neutron) must be the singlet state with spin zero. ...
... simplest nucleus of deuterium: The spin 1 of deuterium since quantum axioms require that the single stable bound state of two particles with spin ½, (proton and neutron) must be the singlet state with spin zero. ...
What constitutes the dark matter?
... fall time 1/ density, diameter sound speed fall time, mass 100.000 suns • Gibson 1996: Viscosity leads to fragmentation in gas balls of a few earth masses • If gas balls coagulate, stars form • Then Jeans cluster becomes visible as globular cluster • Most gas balls cool and freeze, their ...
... fall time 1/ density, diameter sound speed fall time, mass 100.000 suns • Gibson 1996: Viscosity leads to fragmentation in gas balls of a few earth masses • If gas balls coagulate, stars form • Then Jeans cluster becomes visible as globular cluster • Most gas balls cool and freeze, their ...
The Evolution of Stars - a More Detailed Picture (Chapter 8
... fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces the evolutionary tracks of low-mass stars in the HR diagram to travel almost ...
... fall indefinitely. When the temperature of the outer layers of the star fall below a certain level, they become fully convective. This enables a greater luminosity to be carried by the outer layers and hence abruptly forces the evolutionary tracks of low-mass stars in the HR diagram to travel almost ...
Chapter 17 Star Stuff
... – Stars form in dark, dusty clouds of molecular gas with temperatures of 10-30 K – Stars form in clouds that are massive enough for gravity to overcome thermal pressure (and any other forms of resistance) – Such a cloud contracts and breaks up into pieces called proplyds that go on to form ...
... – Stars form in dark, dusty clouds of molecular gas with temperatures of 10-30 K – Stars form in clouds that are massive enough for gravity to overcome thermal pressure (and any other forms of resistance) – Such a cloud contracts and breaks up into pieces called proplyds that go on to form ...
Refusing to Go Quietly: GRBs and Their Progenitors
... Designed to detect nuclear tests (in violation of the test ban treaty), the Vela satellites discovered GRBs ...
... Designed to detect nuclear tests (in violation of the test ban treaty), the Vela satellites discovered GRBs ...
Merging white dwarfs and thermonuclear supernovae
... theoretically, and hence one has to turn to observational tests. So far, most have focused on trying to distinguish between the single- and double-degenerate scenario, with conflicting results: no signature of a (former) companion in early SN Ia lightcurves [41–44] or in SN Ia remnants [45,46], yet ...
... theoretically, and hence one has to turn to observational tests. So far, most have focused on trying to distinguish between the single- and double-degenerate scenario, with conflicting results: no signature of a (former) companion in early SN Ia lightcurves [41–44] or in SN Ia remnants [45,46], yet ...
Lecture 4 Hydrostatic equilibrium
... the star. Hence changes that involve substantial losses or gains of energy can not take place on timescales shorter than ...
... the star. Hence changes that involve substantial losses or gains of energy can not take place on timescales shorter than ...
slides - University of Mississippi Physics
... forces . In high energy accelerators, particles (electrons, protons and their anti-particles) are accelerated to extremely high energies, and make them to collide with each other to produce new particles and study their interactions. Conditions similar to very early stages of the universe, fraction ...
... forces . In high energy accelerators, particles (electrons, protons and their anti-particles) are accelerated to extremely high energies, and make them to collide with each other to produce new particles and study their interactions. Conditions similar to very early stages of the universe, fraction ...
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.