01.1PART I_Ch1.fm - The Thunderbolts Project
... Before new findings disproved these beliefs, they were so "obviously true" as to discourage challenges. It is easy to confuse theoretical assumption with fact. And today the tendency often conceals a tacit belief that, despite the mistakes of previous generations, we have the big picture right and t ...
... Before new findings disproved these beliefs, they were so "obviously true" as to discourage challenges. It is easy to confuse theoretical assumption with fact. And today the tendency often conceals a tacit belief that, despite the mistakes of previous generations, we have the big picture right and t ...
A self-consistent model of isolated neutron stars: the case of the X
... where ρ is the energy density, a0 = a0 (r) is a function that depends on the boundary conditions and we have omitted the relativistic factors for clarity. In the case µ = 0 the purely poloidal case is recovered, as discussed for example in Konno et al. (1999) for the weak magnetic field limit, and m ...
... where ρ is the energy density, a0 = a0 (r) is a function that depends on the boundary conditions and we have omitted the relativistic factors for clarity. In the case µ = 0 the purely poloidal case is recovered, as discussed for example in Konno et al. (1999) for the weak magnetic field limit, and m ...
The Science Case for SPICA Far
... likely to detect polarization along lines of sight with visual optical AV as low as 1mag. and to achieve 0.3% polarization uncertainties where AV > 5 mag. (Sensitivity estimated from Planck: The Scientific Programme, astroph/0604069, p. 10.) Unfortunately, Planck’s beam size is 5´, which will avera ...
... likely to detect polarization along lines of sight with visual optical AV as low as 1mag. and to achieve 0.3% polarization uncertainties where AV > 5 mag. (Sensitivity estimated from Planck: The Scientific Programme, astroph/0604069, p. 10.) Unfortunately, Planck’s beam size is 5´, which will avera ...
Level Energy Forces Waves Electricity and magnetism Matter Space
... a) describe how heating a system will change the energy stored within the system and raise its temperature or produce changes of state b) describe how and why the atomic model has changed over time c) recall that in each atom its electrons are arranged at different distances from the nucleus. d) rec ...
... a) describe how heating a system will change the energy stored within the system and raise its temperature or produce changes of state b) describe how and why the atomic model has changed over time c) recall that in each atom its electrons are arranged at different distances from the nucleus. d) rec ...
The centrifugal term is nearly equal to zero.
... The mildly PFD jet → (mildly) kinetic energy flux dominated (KFD) jet. The highly PFD jet with the steep atmosphere → an equipartition state between the kinetic and Poynting fluxes. Jets propagating in the trans-Alfvenic region before they become kinetic energy dominated, can be deformed into wiggle ...
... The mildly PFD jet → (mildly) kinetic energy flux dominated (KFD) jet. The highly PFD jet with the steep atmosphere → an equipartition state between the kinetic and Poynting fluxes. Jets propagating in the trans-Alfvenic region before they become kinetic energy dominated, can be deformed into wiggle ...
Energy densities of magnetic field and relativistic electrons at the
... 4 Summary and discussions Based on VLBA observation data at 43 GHz, we explore Ue /UB at the base of the M87 jet. We use standard basic theory of synchrotron radiation with the simplest geometry of one-zone sphere model for the radio core at 43 GHz. We impose the upper limit of total jet power Ljet ...
... 4 Summary and discussions Based on VLBA observation data at 43 GHz, we explore Ue /UB at the base of the M87 jet. We use standard basic theory of synchrotron radiation with the simplest geometry of one-zone sphere model for the radio core at 43 GHz. We impose the upper limit of total jet power Ljet ...
Theory of pulsar winds and nebulae - Max-Planck
... If one traces the escaping (“open”) magnetic field lines back to the stellar surface, they define areas which, in a dipole geometry, lie close to the magnetic axis and are called “polar caps”. To maintain a steady state, plasma must be continuously generated on the open field lines in these polar re ...
... If one traces the escaping (“open”) magnetic field lines back to the stellar surface, they define areas which, in a dipole geometry, lie close to the magnetic axis and are called “polar caps”. To maintain a steady state, plasma must be continuously generated on the open field lines in these polar re ...
Dissipation and heating in solar wind turbulence: from the macro to
... showed the now well-documented fact that at scales around the typical length of an orbit radius of protons/ions gyrating around a magnetic field (proton/ion gyro-scale), the power-law spectra in the inertial range, mentioned above, break abruptly and at smaller scales another steeper power-law [12–1 ...
... showed the now well-documented fact that at scales around the typical length of an orbit radius of protons/ions gyrating around a magnetic field (proton/ion gyro-scale), the power-law spectra in the inertial range, mentioned above, break abruptly and at smaller scales another steeper power-law [12–1 ...
What is ZEUS-3D? - Institute for Computational Astrophysics
... Stone, 2005) which require an additional round of two-point averaging and/or interpolation between the zone-centred and face-centred magnetic field components (or, more accurately, the fluxes and induced fields) in each MHD cycle. While flux-cleaning and hybrid methods both eliminate magnetic monopo ...
... Stone, 2005) which require an additional round of two-point averaging and/or interpolation between the zone-centred and face-centred magnetic field components (or, more accurately, the fluxes and induced fields) in each MHD cycle. While flux-cleaning and hybrid methods both eliminate magnetic monopo ...
2 Solar magnetic fields. - High Altitude Observatory
... elementary aspects of the complex interaction of magnetic fields and plasma in the Sun, from the point of view of Newton, and Maxwell. Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots ...
... elementary aspects of the complex interaction of magnetic fields and plasma in the Sun, from the point of view of Newton, and Maxwell. Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots ...
Evolution of the multipolar magnetic field in isolated neutron stars
... multipoles of order l * R* =er; the decay rates would be similar because of the finite thickness er of the crust over which the current is confined. The evolution plotted in Fig. 1 assumes that er 1:2 km; for which R* =er , 8: However it is seen from Figs 1 and 2 that significant decay occurs only ...
... multipoles of order l * R* =er; the decay rates would be similar because of the finite thickness er of the crust over which the current is confined. The evolution plotted in Fig. 1 assumes that er 1:2 km; for which R* =er , 8: However it is seen from Figs 1 and 2 that significant decay occurs only ...
Stellar Evolu1on Stars spend most of their lives on the main
... Stars expand and become more luminous while on the main-‐sequence -‐> the conversion of hydrogen into helium changes the chemical composi,on in the core. According to the ideal gas law (see on-‐line ...
... Stars expand and become more luminous while on the main-‐sequence -‐> the conversion of hydrogen into helium changes the chemical composi,on in the core. According to the ideal gas law (see on-‐line ...
radio loudness. - Rencontres de Moriond
... XXXXth Recontres de Moriond “Very High Energy Phenomena in the Universe”, La Thuile, Italy ...
... XXXXth Recontres de Moriond “Very High Energy Phenomena in the Universe”, La Thuile, Italy ...
Stellar Magnetic Field_1
... The quadratic term dominates for hydrogen H10 for B > 104 G The sigma components shift twice as much as the pi components At 1 MG, H8 would be shifted by about 350 km/s blueward relative to H8, easily detectable (cf Preston 1970, ApJ 160, L143) Polarisation effects are similar to those of Zeeman eff ...
... The quadratic term dominates for hydrogen H10 for B > 104 G The sigma components shift twice as much as the pi components At 1 MG, H8 would be shifted by about 350 km/s blueward relative to H8, easily detectable (cf Preston 1970, ApJ 160, L143) Polarisation effects are similar to those of Zeeman eff ...
Dynamic Martian magnetosphere: Transient - HAL
... (with Bz > 0), a parallel Bow Shock (BS) region (region of the BS where the shock normal is parallel to the IMF direction) can be identified in the -Z half plane. Figure 1 represents an isovalue surface of the total magnetic field at 5 nT highlighting the BS surface at t = 0 s corresponding to the o ...
... (with Bz > 0), a parallel Bow Shock (BS) region (region of the BS where the shock normal is parallel to the IMF direction) can be identified in the -Z half plane. Figure 1 represents an isovalue surface of the total magnetic field at 5 nT highlighting the BS surface at t = 0 s corresponding to the o ...
New results on the age- activity relation from Kepler Alfio Bonanno
... Total oscillation power (in quiet Sun units) ...
... Total oscillation power (in quiet Sun units) ...
A Rigid-Field Hydrodynamics approach to modelling the
... synthesizing observables for the shock-heated wind plasma, across a broad range of wavelengths extending from X-ray through to radio. In the following section, we consider the one-dimensional (1D) hydrodynamical problem of flow along each rigid field line, with an emphasis on the specific, simple ca ...
... synthesizing observables for the shock-heated wind plasma, across a broad range of wavelengths extending from X-ray through to radio. In the following section, we consider the one-dimensional (1D) hydrodynamical problem of flow along each rigid field line, with an emphasis on the specific, simple ca ...
Evolution of inflation-generated magnetic field through
... [11]. In this case the power spectrum of the magnetic field is |B(k)|2 ∝ k/a4 , where k is the coordinate wave number, and the evolution with scale factor a is as expected from flux conservation. This tiny value is a consequence of the conformal invariance of the abelian vector field lagrangian dens ...
... [11]. In this case the power spectrum of the magnetic field is |B(k)|2 ∝ k/a4 , where k is the coordinate wave number, and the evolution with scale factor a is as expected from flux conservation. This tiny value is a consequence of the conformal invariance of the abelian vector field lagrangian dens ...
Physics of Stars and the Measurement Data: Part III
... 2 He have the times of life, which can reach tenth part of the seconds. Stars have the time of life about billions years and the lines of their spectrum of masses are not smoothed. Thus we should suppose that there is some mechanism of stabilization of neutron-excess nuclei inside stars. This mechan ...
... 2 He have the times of life, which can reach tenth part of the seconds. Stars have the time of life about billions years and the lines of their spectrum of masses are not smoothed. Thus we should suppose that there is some mechanism of stabilization of neutron-excess nuclei inside stars. This mechan ...
Acoustic Waves - The Evergreen State College
... permeability and ρ is the mass density. Magnetosonic waves are longitudinal magnetic waves; they travel across magnetic field lines and cause perturbations to the magnetic pressure. Both Alfvén and magnetosonic waves have been observed in the ionosphere during geomagnetic storms caused by CMEs4. ...
... permeability and ρ is the mass density. Magnetosonic waves are longitudinal magnetic waves; they travel across magnetic field lines and cause perturbations to the magnetic pressure. Both Alfvén and magnetosonic waves have been observed in the ionosphere during geomagnetic storms caused by CMEs4. ...
Particle acceleration and synchrotron emission in blazar jets
... with γmax = (βs tacc )−1 . The quantities tacc and tesc have been assumed independent of energy in this solution, the more general solution allowing for energy dependence is given in the Appendix. In the model developed by Ball & Kirk (1992), accelerated particles escape into the downstream plasma, ...
... with γmax = (βs tacc )−1 . The quantities tacc and tesc have been assumed independent of energy in this solution, the more general solution allowing for energy dependence is given in the Appendix. In the model developed by Ball & Kirk (1992), accelerated particles escape into the downstream plasma, ...
Formation of high-field magnetic white dwarfs from common envelopes
... Bϕ ∼ 2 × 104 G. To survive past the PN stage, the fields must reach the WD surface (which is the core of the AGB star, a distance L ≃ Rconv interior to the base of the convective zone; see figure 3 of ref. 18 for a pictorial representation), anchor, and sustain or induce a field in the WD. The latte ...
... Bϕ ∼ 2 × 104 G. To survive past the PN stage, the fields must reach the WD surface (which is the core of the AGB star, a distance L ≃ Rconv interior to the base of the convective zone; see figure 3 of ref. 18 for a pictorial representation), anchor, and sustain or induce a field in the WD. The latte ...
Two Years in Heaven (1983-1985) TAPIR
... Good match to GRB observations (Tchekhovskoy et al. 2009a) ...
... Good match to GRB observations (Tchekhovskoy et al. 2009a) ...
PPT - JMMC
... Matsumura & Pudritz 03: X-rays, CR and radioactivity, disc = Chiang & Goldreich 97 Passive disc with Ma=0 (more consistent) => Ionization CR > X-rays (unless kTX ≈ 5-10 keV) => dead zone between 0.2- 3 au => Results highly depend only chosen value So ≈ 103 g cm-2 => Interesting proposition: low mass ...
... Matsumura & Pudritz 03: X-rays, CR and radioactivity, disc = Chiang & Goldreich 97 Passive disc with Ma=0 (more consistent) => Ionization CR > X-rays (unless kTX ≈ 5-10 keV) => dead zone between 0.2- 3 au => Results highly depend only chosen value So ≈ 103 g cm-2 => Interesting proposition: low mass ...
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.