constraints on primordial magnetic fields with cmb anisotropies
... cosmological scales the charged component of the cascade interacts with the magnetic fields reducing the flux of secondary photons in the GeV range from the blazar (Dolag et al. 2000). FERMI observations of the Blazar 1ES 0229+200 presents a lack of flux of GeV photons with respect to the prediction ...
... cosmological scales the charged component of the cascade interacts with the magnetic fields reducing the flux of secondary photons in the GeV range from the blazar (Dolag et al. 2000). FERMI observations of the Blazar 1ES 0229+200 presents a lack of flux of GeV photons with respect to the prediction ...
ASTRONOMY AND ASTROPHYSICS Properties of solar pores
... November 7th 1994 (III), cf. Table 1. Series I and III involved polarimetric observations, for these the almost polarization-free Gregory-Coudé-Telescope (GCT) was used. The Stokes-I observations of series II were done at the Vacuum Tower Telescope (VTT), which allows to observe up to four wavelengt ...
... November 7th 1994 (III), cf. Table 1. Series I and III involved polarimetric observations, for these the almost polarization-free Gregory-Coudé-Telescope (GCT) was used. The Stokes-I observations of series II were done at the Vacuum Tower Telescope (VTT), which allows to observe up to four wavelengt ...
The origin of the strongest magnetic fields in dwarfs
... to be done and hence the electrons exert a pressure. Chandrasekhar [2] showed that they have a maximum mass because, at high pressures, electrons must move at speeds close to that of light. For typical white dwarfs, composed of hydrogen deficient material, this mass is 1.44M . Because all adjacent ...
... to be done and hence the electrons exert a pressure. Chandrasekhar [2] showed that they have a maximum mass because, at high pressures, electrons must move at speeds close to that of light. For typical white dwarfs, composed of hydrogen deficient material, this mass is 1.44M . Because all adjacent ...
スライド 1
... Why doesn’t RC injection rate saturate? Polar cap potential is known to be saturated for high solar wind electric field. But, the ring current intensity does not show saturation. Neutral line moves closer to the Earth, the volume per unit magnetic flux in the closed field line region is less. Flux t ...
... Why doesn’t RC injection rate saturate? Polar cap potential is known to be saturated for high solar wind electric field. But, the ring current intensity does not show saturation. Neutral line moves closer to the Earth, the volume per unit magnetic flux in the closed field line region is less. Flux t ...
Determination of the levitation limits of dust particles within the
... E kB Te =ek, where k is the ion mean free path.6 Therefore, in order to satisfy the Bohm criterion for the sheath edge, ions in the bulk plasma must be accelerated to the Bohm velocity. This realization led to the introduction of the presheath region. The presheath is defined as the quasineutral ...
... E kB Te =ek, where k is the ion mean free path.6 Therefore, in order to satisfy the Bohm criterion for the sheath edge, ions in the bulk plasma must be accelerated to the Bohm velocity. This realization led to the introduction of the presheath region. The presheath is defined as the quasineutral ...
Precipitation Behavior and Magnetic Properties of Cu-Fe
... Figure 5 shows the hysteresis loops of Cu-1.8at%Fe1.2at%Co specimens annealed at 973 K for 10, 50, 1000, and 5000 min. All specimens exhibited the saturated magnetization at a similar level. However, we found that the specimen which annealed for 50 min showed the largest coercivity and anisotropy. F ...
... Figure 5 shows the hysteresis loops of Cu-1.8at%Fe1.2at%Co specimens annealed at 973 K for 10, 50, 1000, and 5000 min. All specimens exhibited the saturated magnetization at a similar level. However, we found that the specimen which annealed for 50 min showed the largest coercivity and anisotropy. F ...
A systematic examination of particle motion in a collapsing magnetic
... which start at positions further away from the centre of the trap (x = 0) are more likely to escape quickly even for initial pitch angles relatively close to 90◦ , often without mirroring, whereas particles starting close to the centre are more likely to remain trapped. The reason is that outside th ...
... which start at positions further away from the centre of the trap (x = 0) are more likely to escape quickly even for initial pitch angles relatively close to 90◦ , often without mirroring, whereas particles starting close to the centre are more likely to remain trapped. The reason is that outside th ...
The magnetic field and wind confinement of b Cephei: new clues for
... of the escape velocity (equal to 800 km s21 in the case of b Cep). This is in reasonable agreement with observations of the C IV line profile, showing variability down to velocities of 2 750 km s21 (Henrichs et al. 2001) and with the theoretical estimates of Abbott (1982, using the Castor–Abbott–Kle ...
... of the escape velocity (equal to 800 km s21 in the case of b Cep). This is in reasonable agreement with observations of the C IV line profile, showing variability down to velocities of 2 750 km s21 (Henrichs et al. 2001) and with the theoretical estimates of Abbott (1982, using the Castor–Abbott–Kle ...
Accreting neutron stars: strong gravity and type I bursts - UvA-DARE
... 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 ...
Probing magnetic fields with Square Kilometre array and its precursors
... inclination of the magnetic field vector to the line of sight and number density of thermal electrons (in cm−3 ), respectively. The integral is carried out along the line of sight from source at r to the the observer. When the emission originates from a single FD, it is equivalent to the Faraday rot ...
... inclination of the magnetic field vector to the line of sight and number density of thermal electrons (in cm−3 ), respectively. The integral is carried out along the line of sight from source at r to the the observer. When the emission originates from a single FD, it is equivalent to the Faraday rot ...
Laboratory Astrophysics: Spectral Analysis of Photoionized Neon
... simulations have not been experimentally tested like the commonly used collisional ionization codes (APEC, for example). Indeed, these codes do not always produce identical results. Most importantly, these codes do not always produce results that match observations well [12]. Such disparities do not ...
... simulations have not been experimentally tested like the commonly used collisional ionization codes (APEC, for example). Indeed, these codes do not always produce identical results. Most importantly, these codes do not always produce results that match observations well [12]. Such disparities do not ...
- Achieve the Core
... region where the Voyagers are now "the heliosheath." It is essentially the border crossing between the Solar System and the rest of the Milky Way. Lots of things try to get across— interstellar clouds, knots of galactic magnetism, cosmic rays and so on. Will these intruders encounter a riot of bubbl ...
... region where the Voyagers are now "the heliosheath." It is essentially the border crossing between the Solar System and the rest of the Milky Way. Lots of things try to get across— interstellar clouds, knots of galactic magnetism, cosmic rays and so on. Will these intruders encounter a riot of bubbl ...
Laboratory Astrophysics: Spectral Analysis of Photoionized Neon J ames MacArthur
... simulations have not been experimentally tested like the commonly used collisional ionization codes (APEC , for example). Indeed, these codes do not always produce identical results. Most importantly, these codes do not always produce results that match observations well [12]. Such disparities do no ...
... simulations have not been experimentally tested like the commonly used collisional ionization codes (APEC , for example). Indeed, these codes do not always produce identical results. Most importantly, these codes do not always produce results that match observations well [12]. Such disparities do no ...
Energy Extraction from Spinning Black Holes Via Relativistic Jets
... great insight was to realize that it is possible to have Ė(rH ) < 0 (net outward energy flow as measured at the horizon), and thus η > 1. In the context of an accretion flow, Ė(rH ) < 0 means that, even though rest mass flows steadily into the BH, there is a net energy flow out of the BH. As a res ...
... great insight was to realize that it is possible to have Ė(rH ) < 0 (net outward energy flow as measured at the horizon), and thus η > 1. In the context of an accretion flow, Ė(rH ) < 0 means that, even though rest mass flows steadily into the BH, there is a net energy flow out of the BH. As a res ...
Plasma waves above the ion cyclotron frequency in the solar wind: a
... almost Maxwellian, but also of a halo (representing electrons of higher energy) which strongly departs from a thermal distribution function. In some specific environments (high speed solar wind, far from magnetic sector boundaries), a third component appears: called a “strahl”, it represents an enha ...
... almost Maxwellian, but also of a halo (representing electrons of higher energy) which strongly departs from a thermal distribution function. In some specific environments (high speed solar wind, far from magnetic sector boundaries), a third component appears: called a “strahl”, it represents an enha ...
Optimization of SMES Coil by Using Virial Theorem
... solenoidal coil. The combination removes the net electromagnetic force in major radius direction[3] by canceling the centering force of the TF coil and the hoop force of the solenoidal coil. Furthermore, we showed the configuration without the tilting force, by giving poloidal dependence to the pitch ...
... solenoidal coil. The combination removes the net electromagnetic force in major radius direction[3] by canceling the centering force of the TF coil and the hoop force of the solenoidal coil. Furthermore, we showed the configuration without the tilting force, by giving poloidal dependence to the pitch ...
Magnetized massive stars as magnetar progenitors
... 1995). By magnetic flux conservation during the stellar evolution, Ferrario & Wickramasinghe (2005) argued that stellar magnetic fields (∼100 G) in their main-sequence phase can be enhanced up to the range of ∼106 –109 G on the surface of magnetic white dwarfs. This fossil-field scenario is supporte ...
... 1995). By magnetic flux conservation during the stellar evolution, Ferrario & Wickramasinghe (2005) argued that stellar magnetic fields (∼100 G) in their main-sequence phase can be enhanced up to the range of ∼106 –109 G on the surface of magnetic white dwarfs. This fossil-field scenario is supporte ...
PDF only
... order in systems far from equilibrium. It is on this basis that Little Effect explains and determines the dynamics and the basis for order under extreme conditions that organize diamond formation, superconductivity and pycnonuclear reactions. We here introduce multi-spin catalytic effects during adi ...
... order in systems far from equilibrium. It is on this basis that Little Effect explains and determines the dynamics and the basis for order under extreme conditions that organize diamond formation, superconductivity and pycnonuclear reactions. We here introduce multi-spin catalytic effects during adi ...
double shell–burning
... reactions involving iron do not release energy. (This is because iron has lowest mass per nuclear particle.) ...
... reactions involving iron do not release energy. (This is because iron has lowest mass per nuclear particle.) ...
Radiative Processes in Astrophysics. Radio Polarization
... maps from interferometer data – a priori amplitude calibration, fringe-fitting, self-calibration and deconvolution. The calibration of polarization data is largely similar but with a few extra steps required to produce well-calibrated cross-hand visibilities (i.e. the RL and LR correlations which pr ...
... maps from interferometer data – a priori amplitude calibration, fringe-fitting, self-calibration and deconvolution. The calibration of polarization data is largely similar but with a few extra steps required to produce well-calibrated cross-hand visibilities (i.e. the RL and LR correlations which pr ...
TeV gamma rays from blazars beyond z= 1?
... can be found from Fig. 1 as the point where the distance to the source is equal the mean free path of protons at the present epoch, d = λpγ (E ∗ , z = 0). The contributions of protons with lower or higher energies would be significantly smaller. For lower energies, the interaction probability is too ...
... can be found from Fig. 1 as the point where the distance to the source is equal the mean free path of protons at the present epoch, d = λpγ (E ∗ , z = 0). The contributions of protons with lower or higher energies would be significantly smaller. For lower energies, the interaction probability is too ...
PHY 380L Introduction to Plasma Physics Richard Fitzpatrick
... melt, molecules disassociate. At temperatures near or exceeding atomic ionization energies, atoms similarly decompose into negatively charged electrons and positively charged ions. These charged particles are by no means free: in fact, they are strongly affected by each others’ electromagnetic fiel ...
... melt, molecules disassociate. At temperatures near or exceeding atomic ionization energies, atoms similarly decompose into negatively charged electrons and positively charged ions. These charged particles are by no means free: in fact, they are strongly affected by each others’ electromagnetic fiel ...
Polarimetric evidence of a white dwarf pulsar in
... energy distribution. These observations were explained in terms of beamed synchrotron radiation from the white dwarf, some of which is reprocessed by the companion star (2). The weak X-ray emission suggests that little accretion power is produced in AR Sco, which either implies that it is currently ...
... energy distribution. These observations were explained in terms of beamed synchrotron radiation from the white dwarf, some of which is reprocessed by the companion star (2). The weak X-ray emission suggests that little accretion power is produced in AR Sco, which either implies that it is currently ...
PHY418 Particle Astrophysics
... Issues with Fermi 2nd order • It’s too slow • relative velocities of objects in Galactic disc are only 10s of km/s, so fractional energy gain per reflection is only ~10−8 • There is no obvious reason why different sources should ...
... Issues with Fermi 2nd order • It’s too slow • relative velocities of objects in Galactic disc are only 10s of km/s, so fractional energy gain per reflection is only ~10−8 • There is no obvious reason why different sources should ...
Analytical formulae for the energy of electron subshells in atoms and
... The next essential step was generalization of the Schrödinger equation to the two-electron helium atom. No exact analytical solution to the problem was found, but the hydrogen wave functions have been modified in different ways. The most important summary of results in this direction is given in th ...
... The next essential step was generalization of the Schrödinger equation to the two-electron helium atom. No exact analytical solution to the problem was found, but the hydrogen wave functions have been modified in different ways. The most important summary of results in this direction is given in th ...
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.