Level Energy Forces Waves Electricity and magnetism Matter Space
... Describe the relationship of transverse waves whilst current and time. states of matter in terms of between force and extension sound waves in air are b) Calculate the total resistance the arrangements of the Define and categorise longitudinal waves, and how of combinations of resistors atoms or mol ...
... Describe the relationship of transverse waves whilst current and time. states of matter in terms of between force and extension sound waves in air are b) Calculate the total resistance the arrangements of the Define and categorise longitudinal waves, and how of combinations of resistors atoms or mol ...
Double Layer Observations and role in particle acceleration
... Double layers are regions of charge separation along B that produce parallel E and parallel potential drops They were proposed by Alfven 55 years ago to be the mechanism for accelerating electrons in astrophysics Until now, they have not been observed with sufficient total potentials to matter VAP h ...
... Double layers are regions of charge separation along B that produce parallel E and parallel potential drops They were proposed by Alfven 55 years ago to be the mechanism for accelerating electrons in astrophysics Until now, they have not been observed with sufficient total potentials to matter VAP h ...
Physics of Stars and the Measurement Data: Part III
... electron gas effect on the plasma nuclear subsystem. It is accepted to consider dense plasma to be divided in plasma cells. These cells are filled by electron gas and they have positively charged nuclei in their centers [2]. This construction is non stable from the point of view of the classical mec ...
... electron gas effect on the plasma nuclear subsystem. It is accepted to consider dense plasma to be divided in plasma cells. These cells are filled by electron gas and they have positively charged nuclei in their centers [2]. This construction is non stable from the point of view of the classical mec ...
X-ray Sources in Nearby Galaxies Q. Daniel Wang University of Massachusetts
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
October 2003 Part 2 of 3
... Vigier Conference in 2000 where G* is the renormalized strong short-range Abdus Salam effective zero point energy density induced gravitational coupling. I. Highlights of the Vigier IV Paris Conference I have been following William Walker’s (1) very clear theoretical and experimental work on superlu ...
... Vigier Conference in 2000 where G* is the renormalized strong short-range Abdus Salam effective zero point energy density induced gravitational coupling. I. Highlights of the Vigier IV Paris Conference I have been following William Walker’s (1) very clear theoretical and experimental work on superlu ...
Driven reconnection and bursty bulk flows
... diverse observed features of substorm related changes in the magnetotail. Even though BBFs are positively correlated with the geomagnetic activity, there is no one-to-one correspondence between a substorm and BBF. Therefore, the NENL paradigm cannot be invoked to explain the bursty flows. There have ...
... diverse observed features of substorm related changes in the magnetotail. Even though BBFs are positively correlated with the geomagnetic activity, there is no one-to-one correspondence between a substorm and BBF. Therefore, the NENL paradigm cannot be invoked to explain the bursty flows. There have ...
Department of Physics and Astronomy University of
... of heavy isotopes in dense stellar plasmas is not generally available, we need to derive theoretical values for the ionization degree. To this end we consider plasma conditions characteristic for s-process nucleosynthesis and calculate probabilities for various charged states and ionization stages ...
... of heavy isotopes in dense stellar plasmas is not generally available, we need to derive theoretical values for the ionization degree. To this end we consider plasma conditions characteristic for s-process nucleosynthesis and calculate probabilities for various charged states and ionization stages ...
Neutron Stars – Thermal Emitters
... of the first sources of cosmic X-rays in the Early Sixties suggested that NSs could indeed be detected, which added impetus to theoretical work as well as to modeling of expected NS observational properties. The crucial point, attracting a lot of interest in the astrophysical community, was that the ...
... of the first sources of cosmic X-rays in the Early Sixties suggested that NSs could indeed be detected, which added impetus to theoretical work as well as to modeling of expected NS observational properties. The crucial point, attracting a lot of interest in the astrophysical community, was that the ...
Ion-supported tori: a thermal bremsstrahlung model for the X
... show no such spectral features (Gendreau et al. 1995a,b), implying that a new faint population with a very hard, smooth X-ray spectrum is required. A promising new population of sources with harder mean X-ray spectra discovered in deep ROSAT images (Hasinger et al. 1993; McHardy et al. 1995; Vikhlin ...
... show no such spectral features (Gendreau et al. 1995a,b), implying that a new faint population with a very hard, smooth X-ray spectrum is required. A promising new population of sources with harder mean X-ray spectra discovered in deep ROSAT images (Hasinger et al. 1993; McHardy et al. 1995; Vikhlin ...
Zettawatt-Exawatt Lasers and Their Applications in Ultrastrong
... Note that although large, the number of optical components involved will be small, compared to a MJ system calling for 4500 laser slabs, 800 large KDP frequency converter crystals, and 500 gratings of meter-size. An alternative method using a plasma has been suggested [8], but will lead to the same ...
... Note that although large, the number of optical components involved will be small, compared to a MJ system calling for 4500 laser slabs, 800 large KDP frequency converter crystals, and 500 gratings of meter-size. An alternative method using a plasma has been suggested [8], but will lead to the same ...
double shell–burning
... • Not enough mass to ignite carbon fusion • Ejection of outer layers into space producing a planetary nebula and leaving a white hot core (white dwarf) ...
... • Not enough mass to ignite carbon fusion • Ejection of outer layers into space producing a planetary nebula and leaving a white hot core (white dwarf) ...
Measurement of very low (α,n) cross sections of astrophysical interest
... Experimentally the cross sections at the relevant energies (Gamow window) have not been measured and currently they are estimated from extrapolations. The limiting factor in the measurements has been the relatively high level of neutron background in comparison with the weak reaction rates expected ...
... Experimentally the cross sections at the relevant energies (Gamow window) have not been measured and currently they are estimated from extrapolations. The limiting factor in the measurements has been the relatively high level of neutron background in comparison with the weak reaction rates expected ...
What keeps stars shining? What holds them up? Lecture 14. The
... luminosity!) is replaced. In the sun, this is the "proton-proton" variety of hydrogen fusion. Depends very sensitively on temperature. (There are other varieties active in other stars.) So the bottom line is, as long as fusion continues in the center of the sun, it replaces the heat lost to the outs ...
... luminosity!) is replaced. In the sun, this is the "proton-proton" variety of hydrogen fusion. Depends very sensitively on temperature. (There are other varieties active in other stars.) So the bottom line is, as long as fusion continues in the center of the sun, it replaces the heat lost to the outs ...
Fundamental Physics With Cold and Ultra-cold
... (at ILL). Note: over two orders of magnitude improvement may ultimately be possible! ...
... (at ILL). Note: over two orders of magnitude improvement may ultimately be possible! ...
Astroparticle physics A.M. van den Berg () O. Scholten
... Regions on the CMB sky separated by more than 1o had no time to interact, yet their temperature is the same to 100 ppm What is needed An initial condition of the Universe with a temperature between 1 MeV and 1014 GeV, which is almost homogenous and has = 1 to a very high precision Summary ...
... Regions on the CMB sky separated by more than 1o had no time to interact, yet their temperature is the same to 100 ppm What is needed An initial condition of the Universe with a temperature between 1 MeV and 1014 GeV, which is almost homogenous and has = 1 to a very high precision Summary ...
On the electron-ion temperature ratio established by - Hal-CEA
... Astrophysical shocks are often collisionless shocks, in which the changes in plasma flow and temperatures across the shock are established not through Coulomb interactions, but through electric and magnetic fields. An open question about collisionless shocks is whether electrons and ions each establ ...
... Astrophysical shocks are often collisionless shocks, in which the changes in plasma flow and temperatures across the shock are established not through Coulomb interactions, but through electric and magnetic fields. An open question about collisionless shocks is whether electrons and ions each establ ...
Lecture 16 - QMUL physics
... net change in neutron number between generations Defined for infinite medium - losses through surfaces ignored Thus each thermal neutron produces k∞new thermal neutrons Require k∞>1 for chain reaction to occur Note: 235U produces on average 2.5 fast (~1 MeV) neutrons per fission Need to slow neutron ...
... net change in neutron number between generations Defined for infinite medium - losses through surfaces ignored Thus each thermal neutron produces k∞new thermal neutrons Require k∞>1 for chain reaction to occur Note: 235U produces on average 2.5 fast (~1 MeV) neutrons per fission Need to slow neutron ...
On the electron temperature downstream of the solar wind
... that Voyager-2 measurements at the termination shock (TS) crossing (Richardson et al., 2008) deliver data which are unpredicted by presently existing TS models in the literature, like those by Fahr and Chalov (2008) or Wu et al. (2009). Based on identical upstream plasma conditions, none of the pres ...
... that Voyager-2 measurements at the termination shock (TS) crossing (Richardson et al., 2008) deliver data which are unpredicted by presently existing TS models in the literature, like those by Fahr and Chalov (2008) or Wu et al. (2009). Based on identical upstream plasma conditions, none of the pres ...
Constraints on the Production of Ultra–High
... neutron stars could easily account for cosmic rays ; at a median space velocity of 500 km s~1 the energy per neutron star is B4 ] 1048 ergs. To tap that energy the star must be slowed down by collisions. However, collisions between stars are extremely improbable in the disk of the Galaxy, and typica ...
... neutron stars could easily account for cosmic rays ; at a median space velocity of 500 km s~1 the energy per neutron star is B4 ] 1048 ergs. To tap that energy the star must be slowed down by collisions. However, collisions between stars are extremely improbable in the disk of the Galaxy, and typica ...
ASPERA-3: Analyser of Space Plasmas and
... partially thermalised by the bow shock (Kallio et al., 1997). Others undergo chargeexchange reactions with ambient exospheric and thermospheric neutrals, particularly hydrogen, and then impact the exobase as ENAs (Kallio et al., 1997). In both cases, solar wind energy is ‘directly’ deposited into th ...
... partially thermalised by the bow shock (Kallio et al., 1997). Others undergo chargeexchange reactions with ambient exospheric and thermospheric neutrals, particularly hydrogen, and then impact the exobase as ENAs (Kallio et al., 1997). In both cases, solar wind energy is ‘directly’ deposited into th ...
Measuring difficult reaction rates involving
... Beam cooling with ionisation losses – C. Rubbia, A Ferrari, Y. Kadi and V. Vlachoudis in NIM A, In press “Many other applications in a number of different fields may also take profit of intense beams of radioactive ions.” 7Li 6Li ...
... Beam cooling with ionisation losses – C. Rubbia, A Ferrari, Y. Kadi and V. Vlachoudis in NIM A, In press “Many other applications in a number of different fields may also take profit of intense beams of radioactive ions.” 7Li 6Li ...
Simultaneous observation of the electron acceleration and ion deceleration
... 0 deg. is the parallel direction toward the Moon. The accelerated electrons were heated and had mostly parallel velocity toward the Moon surface. The deceleration of the ions was observed simultaneously with the electron acceleration and the deceleration was clearly observed for both protons and alp ...
... 0 deg. is the parallel direction toward the Moon. The accelerated electrons were heated and had mostly parallel velocity toward the Moon surface. The deceleration of the ions was observed simultaneously with the electron acceleration and the deceleration was clearly observed for both protons and alp ...
small free negative ions
... severe; they are principally the requirement of an appropriate negative ion source, of high intensity in the light beam and of moderately stability in the two sources. Discharges have proved to be satisfactory sources; constricting the discharge electrically, magnetically, or both can be used to giv ...
... severe; they are principally the requirement of an appropriate negative ion source, of high intensity in the light beam and of moderately stability in the two sources. Discharges have proved to be satisfactory sources; constricting the discharge electrically, magnetically, or both can be used to giv ...
Power Point slides for Reporter Review
... Electrostatic Coupling and Acceleration of Auroral Electrons (Observations) Direct measurements of parallel electric fields Upward current region: FAST shows large E|| (~ 100 mV/m) at lower edge of auroral density cavity (Ergun et al., 2002) parallel electric fields of 25-300 mV/m seen on Polar; ...
... Electrostatic Coupling and Acceleration of Auroral Electrons (Observations) Direct measurements of parallel electric fields Upward current region: FAST shows large E|| (~ 100 mV/m) at lower edge of auroral density cavity (Ergun et al., 2002) parallel electric fields of 25-300 mV/m seen on Polar; ...
Fusor
A fusor is a device that uses an electric field to heat ions to conditions suitable for nuclear fusion. The machine has a voltage between two metal cages inside a vacuum. Positive ions fall down this voltage drop, building up speed. If they collide in the center, they can fuse. This is a type of Inertial electrostatic confinement device.A Farnsworth–Hirsch fusor is the most common type of fusor. This design came from work by Philo T. Farnsworth (in 1964) and Robert L. Hirsch in 1967. A variant of fusor had been proposed previously by William Elmore, James L. Tuck, and Ken Watson at the Los Alamos National Laboratory though they never built the machine.Fusors have been built by various institutions. These include academic institutions such as the University of Wisconsin–Madison, the Massachusetts Institute of Technology and government entities, such as the Atomic Energy Organization of Iran and the Turkish Atomic Energy Authority. Fusors have also been developed commercially, as sources for neutrons by DaimlerChrysler Aerospace and as a method for generating medical isotopes. Fusors have also become very popular for hobbyists and amateurs. A growing number of amateurs have performed nuclear fusion using simple fusor machines.