Physics of Neutron Star Crusts
... opportunities. The elementary constituents of the matter are neutrons, protons, and electrons – like in the atomic matter around us. The density is “subnuclear”, so that the methods developed and successfully applied in the last decades to terrestrial nuclear physics can be applied to neutron star c ...
... opportunities. The elementary constituents of the matter are neutrons, protons, and electrons – like in the atomic matter around us. The density is “subnuclear”, so that the methods developed and successfully applied in the last decades to terrestrial nuclear physics can be applied to neutron star c ...
Accretion Power in Astrophysics, Third Editiion
... an astrophysical system. Our discussion therefore centres mainly on close binary systems containing compact objects and on active nuclei. The reader is assumed to possess a basic knowledge of physics at first degree level, but only a rudimentary experience of astronomy is required. We have tried to c ...
... an astrophysical system. Our discussion therefore centres mainly on close binary systems containing compact objects and on active nuclei. The reader is assumed to possess a basic knowledge of physics at first degree level, but only a rudimentary experience of astronomy is required. We have tried to c ...
Photometric Variability and Rotation in Magnetic White Dwarfs
... emerged between the spin period and magnetic field strength and temperature, suggesting hotter MWDs spin faster and have higher field strengths, characteristics possibly associated with MWDs that might have formed in binary mergers. A similar investigation is carried out on longer timescales (months ...
... emerged between the spin period and magnetic field strength and temperature, suggesting hotter MWDs spin faster and have higher field strengths, characteristics possibly associated with MWDs that might have formed in binary mergers. A similar investigation is carried out on longer timescales (months ...
Electromagnetic Properties of Neutrinos
... between the left-handed components of the three flavor neutrino fields νe , νμ , ντ and the lefthanded components of three massive neutrino fields νk with masses mk k 1, 2, 3. The 3 × 3 mixing matrix U is unitary U† U−1 . Neutrino electromagnetic properties are discussed in 4–7, and in the ...
... between the left-handed components of the three flavor neutrino fields νe , νμ , ντ and the lefthanded components of three massive neutrino fields νk with masses mk k 1, 2, 3. The 3 × 3 mixing matrix U is unitary U† U−1 . Neutrino electromagnetic properties are discussed in 4–7, and in the ...
Basic Properties of Matter - Reciprocal System of theory
... composed entirely of motion. The characteristics o f the basic motion were defined in Nothing But M otion, the first volume of the series, in the form of seven assumptions as to the nature and interrelation of space and time. In the subsequent development, the necessary consequences of these assumpt ...
... composed entirely of motion. The characteristics o f the basic motion were defined in Nothing But M otion, the first volume of the series, in the form of seven assumptions as to the nature and interrelation of space and time. In the subsequent development, the necessary consequences of these assumpt ...
- Repository of the Academy`s Library
... adjacent research fields. In other words, the solar part is written for magnetospheric physicists, whereas the magnetospheric part — for solar specialists. The comprehensive reference list would be too lengthy and might exceed the review length. Therefore, we have provided references to key papers a ...
... adjacent research fields. In other words, the solar part is written for magnetospheric physicists, whereas the magnetospheric part — for solar specialists. The comprehensive reference list would be too lengthy and might exceed the review length. Therefore, we have provided references to key papers a ...
Solar Flares: Magnetohydrodynamic Processes | SpringerLink
... which is sufficient to produce even the largest flare, although only a small portion of this total energy can be used, that is, a large amount of energy is unavailable because it is distributed as the potential field energy. Following observational results, theoretical studies began to focus on the ...
... which is sufficient to produce even the largest flare, although only a small portion of this total energy can be used, that is, a large amount of energy is unavailable because it is distributed as the potential field energy. Following observational results, theoretical studies began to focus on the ...
THE SPECIFIC ACCELERATION RATE IN LOOP
... effects. However, since Lu (E) is equal to the square root of a ratio of integrals, the results do not depend significantly on the values of the s-integration limits used. The forms of Equations (2) and (3) do not result in a closed analytic form for Lu (E) (see Equation (1)), and so a straightforwa ...
... effects. However, since Lu (E) is equal to the square root of a ratio of integrals, the results do not depend significantly on the values of the s-integration limits used. The forms of Equations (2) and (3) do not result in a closed analytic form for Lu (E) (see Equation (1)), and so a straightforwa ...
Photospheric processes and magnetic flux tubes
... Br0 (R0 ) is not known from the very beginning so that the boundary condition for the pressure needs to be adjusted in the course of the iteration. If we further assume that the temperature at a given hight level is constant, then the gas ...
... Br0 (R0 ) is not known from the very beginning so that the boundary condition for the pressure needs to be adjusted in the course of the iteration. If we further assume that the temperature at a given hight level is constant, then the gas ...
Particle kinematics in solar flares: observations - ETH E
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
EUV and X-ray Spectroscopy of the Active Sun
... path of propagating electrons towards the dense chromosphere (c). Heating of the chromosphere results in chromospheric evaporation (d) which fills the loops with hot, SXR emitting plasma (e). Direct heating of the looptop can result in large pressure gradients that drive conductive fronts (f ). . . ...
... path of propagating electrons towards the dense chromosphere (c). Heating of the chromosphere results in chromospheric evaporation (d) which fills the loops with hot, SXR emitting plasma (e). Direct heating of the looptop can result in large pressure gradients that drive conductive fronts (f ). . . ...
The Physics of Background Discrimination in Liquid Xenon, and First Results from Xenon10 in the Hunt for WIMP Dark Matter
... We also build a simple recombination model that successfully reproduces the mean recombination in electron and nuclear recoils, including the the surprising reversal of the expected trend for recombination with ionization density in low energy electron recoils. The model also reproduces the measured ...
... We also build a simple recombination model that successfully reproduces the mean recombination in electron and nuclear recoils, including the the surprising reversal of the expected trend for recombination with ionization density in low energy electron recoils. The model also reproduces the measured ...
Flare Observations
... sources appear before the hard X-ray emission in chromospheric footpoints, major flare acceleration sites appear to be independent of coronal mass ejections (CMEs), electrons, and ions may be accelerated at different sites, there are at least 3 different magnetic topologies, and basic characteristic ...
... sources appear before the hard X-ray emission in chromospheric footpoints, major flare acceleration sites appear to be independent of coronal mass ejections (CMEs), electrons, and ions may be accelerated at different sites, there are at least 3 different magnetic topologies, and basic characteristic ...
High frequency ion sound waves - Nonlinear Processes in Geophysics
... dov et al., 1990; Karfidov and Lukina, 1997; McFarland and Wong, 1997; Vyacheslavov et al., 2002) as well as in numerical simulations (Degtyarev et al., 1980). Strong turbulence features of Langmuir wave packets were identified in the Jovian foreshock regions (Gurnett et al., 1981; Thiessen and Kell ...
... dov et al., 1990; Karfidov and Lukina, 1997; McFarland and Wong, 1997; Vyacheslavov et al., 2002) as well as in numerical simulations (Degtyarev et al., 1980). Strong turbulence features of Langmuir wave packets were identified in the Jovian foreshock regions (Gurnett et al., 1981; Thiessen and Kell ...
Magnetic fields and mass loss in massive stars
... Figure 1.1: Typical examples of magnetic signatures in stellar wind behaviour in the C IV line of known magnetic B stars. Left: two chemically peculiar stars; a He-strong star (top) and a He-weak star (bottom). Middle/right: four magnetic massive B stars: β Cep, V2052 Oph, ζ Cas and the classical Be ...
... Figure 1.1: Typical examples of magnetic signatures in stellar wind behaviour in the C IV line of known magnetic B stars. Left: two chemically peculiar stars; a He-strong star (top) and a He-weak star (bottom). Middle/right: four magnetic massive B stars: β Cep, V2052 Oph, ζ Cas and the classical Be ...
A Review of the 0.1 Reconnection Rate Problem
... is the reconnecting magnetic field strength, and he showed that δ/L ∼ 1/S 1/2 when the mechanism allowing the magnetic topology to change is a uniform resistivity, where S is the Lundquist number. The local reconnection rate, normalized to B and cA = vout , is E ′ ∼ δ/L. He originally suggested reco ...
... is the reconnecting magnetic field strength, and he showed that δ/L ∼ 1/S 1/2 when the mechanism allowing the magnetic topology to change is a uniform resistivity, where S is the Lundquist number. The local reconnection rate, normalized to B and cA = vout , is E ′ ∼ δ/L. He originally suggested reco ...
Spin light of neutrino in matter and electromagnetic fields
... A new type of electromagnetic radiation by a neutrino with non-zero magnetic (and/or electric) moment moving in background matter and electromagnetic field is considered. This radiation originates from the quantum spin flip transitions and we have named it as ”spin light of neutrino”(SLν). The neutr ...
... A new type of electromagnetic radiation by a neutrino with non-zero magnetic (and/or electric) moment moving in background matter and electromagnetic field is considered. This radiation originates from the quantum spin flip transitions and we have named it as ”spin light of neutrino”(SLν). The neutr ...
Plasmoid-induced-reconnection and fractal reconnection Kazunari Shibata and Syuniti Tanuma
... the plasmoid-induced-reconnection in more detail. We consider a situation where reconnection has just begun and a plasmoid, with a length L p and a width W p , has just started to form. The reconnection generates a jet (with the Alfvén speed V A ) which collides with the plasmoid and accelerates it ...
... the plasmoid-induced-reconnection in more detail. We consider a situation where reconnection has just begun and a plasmoid, with a length L p and a width W p , has just started to form. The reconnection generates a jet (with the Alfvén speed V A ) which collides with the plasmoid and accelerates it ...
The Limits of Our Solar System - Lunar and Planetary Institute
... slows further as it piles up in front of the heliosphere. So when charge exchange occurs, the new neutrals have speeds and temperatures from the shocked plasma, not the pristine interstellar medium. The H observed in the heliosphere has an inflow speed of only 20 km/s, 6 km/s less than the interstel ...
... slows further as it piles up in front of the heliosphere. So when charge exchange occurs, the new neutrals have speeds and temperatures from the shocked plasma, not the pristine interstellar medium. The H observed in the heliosphere has an inflow speed of only 20 km/s, 6 km/s less than the interstel ...
Magnetized Quark and Strange Quark Matter in the Spherical Symmetric Space-Time Admitting Conformal Motion
... be influenced by magnetic forces. Furthermore, reports of Faraday rotation in highredshift, Lyman-α absorption systems suggest that dynamically significant magnetic fields could be present in protogalactic condensations. Despite their widespread presence, however, the precise origin of any large-sca ...
... be influenced by magnetic forces. Furthermore, reports of Faraday rotation in highredshift, Lyman-α absorption systems suggest that dynamically significant magnetic fields could be present in protogalactic condensations. Despite their widespread presence, however, the precise origin of any large-sca ...
The physics of neutron stars
... Ginzburg and co-workers greatly contributed to the elucidation of the nature of radio pulsars – cosmic sources of periodic radio pulses: they first developed the model of oscillating white dwarfs [10, 11], and later the models of rotating neutron stars with strong magnetic fields [12–14]; in these s ...
... Ginzburg and co-workers greatly contributed to the elucidation of the nature of radio pulsars – cosmic sources of periodic radio pulses: they first developed the model of oscillating white dwarfs [10, 11], and later the models of rotating neutron stars with strong magnetic fields [12–14]; in these s ...
The Solar Tachocline: A Self-Consistent Model of Magnetic
... just a few seconds. In reality most of this angular momentum was lost during the early stages of the Sun’s formation, but nevertheless the Sun probably had a rotation period of less than one day when it arrived on the main sequence (e.g. Mestel & Weiss, 1987, & refs). The Sun must therefore have con ...
... just a few seconds. In reality most of this angular momentum was lost during the early stages of the Sun’s formation, but nevertheless the Sun probably had a rotation period of less than one day when it arrived on the main sequence (e.g. Mestel & Weiss, 1987, & refs). The Sun must therefore have con ...
Accreting Neutron Stars: Strong Gravity and Type I Bursts
... et al., 2007) is that neutron stars are compact objects of mass M ∼ 1.4 M⊙ and radius R ∼ 10 km, the high M/R ratio being what makes them compact. Such high compactness also makes them general relativistic objects. Spacetime is highly curved around them and effects such as gravitational redshift, be ...
... et al., 2007) is that neutron stars are compact objects of mass M ∼ 1.4 M⊙ and radius R ∼ 10 km, the high M/R ratio being what makes them compact. Such high compactness also makes them general relativistic objects. Spacetime is highly curved around them and effects such as gravitational redshift, be ...
PDF file
... In Chapter 2 we report a detailed examination of the fine structures inside flare ribbons and the temporal evolution of such structures. We examined systems of conjugate footpoints, inside flare ribbons by using Hα data with high spatial resolution. We first identified the conjugate footpoints of ea ...
... In Chapter 2 we report a detailed examination of the fine structures inside flare ribbons and the temporal evolution of such structures. We examined systems of conjugate footpoints, inside flare ribbons by using Hα data with high spatial resolution. We first identified the conjugate footpoints of ea ...
Polywell
The polywell is a type of nuclear fusion reactor that uses an electric field to heat ions to fusion conditions. It is closely related to the magnetic mirror, the fusor, the biconic cusp and the high beta fusion reactor. A set of electromagnets generates a magnetic field which traps electrons. This creates a negative voltage, which attracts positive ions. As the ions accelerate towards the negative center, their kinetic energy rises. If the ions collide in the center, they can fuse.The polywell is one of many devices that use an electric field to heat ions to fusion conditions. This branch of fusion research is known as inertial electrostatic confinement. The polywell was developed by Robert Bussard, as an improvement over the fusor. His company, EMC2, Inc., developed the initial devices for the U.S. Navy.