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Structure of Neutron Stars - Relativistic Astrophysics Department
... Neutron stars and white dwarfs ...
... Neutron stars and white dwarfs ...
Slides from Lecture19 - Department of Physics & Astronomy
... Determining Size of MW Galaxy • We have not always known that the diameter of our Galaxy is ~ 50 kpc (as illustrated in following slide) • For example, Herschel’s map of our Galaxy (1785) based on star counts … – Thin disk not much more than 1 kpc across – Sun approximately at center of disk ...
... Determining Size of MW Galaxy • We have not always known that the diameter of our Galaxy is ~ 50 kpc (as illustrated in following slide) • For example, Herschel’s map of our Galaxy (1785) based on star counts … – Thin disk not much more than 1 kpc across – Sun approximately at center of disk ...
Observations and analysis of phase scintillation of spacecraft signal
... well-known hydrodynamic turbulence described by Kolmogorov (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its ...
... well-known hydrodynamic turbulence described by Kolmogorov (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its ...
Talk
... The gamma-ray source of the 2.2 MeV neutron-capture line was found to be displaced by 20”+/- 6” from the 25 keV hard X-ray footpoints during the 2002 Jul 23 flare. A similar result was found for the Oct/Nov 2003 flares. Energized electrons and ions show displaced energy loss sites (1) different ac ...
... The gamma-ray source of the 2.2 MeV neutron-capture line was found to be displaced by 20”+/- 6” from the 25 keV hard X-ray footpoints during the 2002 Jul 23 flare. A similar result was found for the Oct/Nov 2003 flares. Energized electrons and ions show displaced energy loss sites (1) different ac ...
release history and transport parameters of relativistic solar
... which was located in the Earth’s magnetosheath on 1980 May 28. In contrast to Helios-1 observations, IMP-8 detected only a single extended particle intensity enhancement; i.e. IMP-8 did not resolve four individual events. Wibberenz & Cane (2006) suggested that the source of the events seen by Helios ...
... which was located in the Earth’s magnetosheath on 1980 May 28. In contrast to Helios-1 observations, IMP-8 detected only a single extended particle intensity enhancement; i.e. IMP-8 did not resolve four individual events. Wibberenz & Cane (2006) suggested that the source of the events seen by Helios ...
From the Sun`s atmosphere to the Earth`s atmosphere
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
Solar and Stellar Active Regions
... active regions exhibits a well defined power law with index ≈ −1.94 and active regions cover only a small fraction of the solar surface (around ∼ 8%) [13]. The fractal dimension of the active regions has been studied using highresolution magnetograms by [9], and more recently by [30]. These authors ...
... active regions exhibits a well defined power law with index ≈ −1.94 and active regions cover only a small fraction of the solar surface (around ∼ 8%) [13]. The fractal dimension of the active regions has been studied using highresolution magnetograms by [9], and more recently by [30]. These authors ...
ASR201017 - UCLA IGPP
... Observations in the magnetotail during substorms have demonstrated the existence of large bundles of magnetic flux and plasma moving tailward that are called plasmoids [Hones et al., 1984]. These were envisioned as magnetic O regions containing magnetic field lines in closed loops. Further observati ...
... Observations in the magnetotail during substorms have demonstrated the existence of large bundles of magnetic flux and plasma moving tailward that are called plasmoids [Hones et al., 1984]. These were envisioned as magnetic O regions containing magnetic field lines in closed loops. Further observati ...
PPT
... Shaping • Among existing models, wind instability models by Pittard et al (2005) & Dyson et al. (2006) can reproduce the shape well ...
... Shaping • Among existing models, wind instability models by Pittard et al (2005) & Dyson et al. (2006) can reproduce the shape well ...
Angular momentum evolution
... • Models with a constant coupling timescale between the core and the envelope cannot reproduce the observations • Need for a rotation-dependent core-envelope coupling timescale : weak coupling in slow rotators, strong coupling in fast rotators • Still need to identify the physical origin of this rot ...
... • Models with a constant coupling timescale between the core and the envelope cannot reproduce the observations • Need for a rotation-dependent core-envelope coupling timescale : weak coupling in slow rotators, strong coupling in fast rotators • Still need to identify the physical origin of this rot ...
P38.Planet Sedna
... Orbit: Sedna’s orbit is extremely elliptical, unlike that of closer planets, and could take it out more than ten times further away from Earth than it is now. Its unusual orbit may be caused by passing stars or perhaps by a larger body (not yet found), about the size of Mars or bigger, existing arou ...
... Orbit: Sedna’s orbit is extremely elliptical, unlike that of closer planets, and could take it out more than ten times further away from Earth than it is now. Its unusual orbit may be caused by passing stars or perhaps by a larger body (not yet found), about the size of Mars or bigger, existing arou ...
Solar Changes and the Climate
... The sun changes in its activity on time scales that vary from 27 days to 11, 22, 80, 106, 212 years and more. A more active sun is brighter due to the dominance of faculae over cooler sunspots with the result that the irradiance emitted by the sun and received by the earth is higher during active so ...
... The sun changes in its activity on time scales that vary from 27 days to 11, 22, 80, 106, 212 years and more. A more active sun is brighter due to the dominance of faculae over cooler sunspots with the result that the irradiance emitted by the sun and received by the earth is higher during active so ...
paper - Lunar and Planetary Institute
... surfaces, atmospheres, and ionospheres in between. The interplanetary environment includes magnetic and electrical fields, plasma, and dust. In order to understand planetary processes over these vast ranges, the properties of materials must be known, and most of the necessary information comes from ...
... surfaces, atmospheres, and ionospheres in between. The interplanetary environment includes magnetic and electrical fields, plasma, and dust. In order to understand planetary processes over these vast ranges, the properties of materials must be known, and most of the necessary information comes from ...
Observation of the Bastille day flare on 2000 July 14
... then due to bumps between particles; it would emit electromagnetic wave such as HXR, radio and even microwave. And meantime, solar flare also would accelerate a part of particles out of the sun’s surface along the magnetic line of force, called Corona Mass Ejection (CME), it also might form the stro ...
... then due to bumps between particles; it would emit electromagnetic wave such as HXR, radio and even microwave. And meantime, solar flare also would accelerate a part of particles out of the sun’s surface along the magnetic line of force, called Corona Mass Ejection (CME), it also might form the stro ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... Our idea: fit lines with the simplest model that can do the job, and use one that, while based in physics, is general in the sense that any number of physical models can be tested or constrained based on the model fits. From Owocki & Cohen (2001): spherically symmetric, two-fluid (hot plasma is int ...
... Our idea: fit lines with the simplest model that can do the job, and use one that, while based in physics, is general in the sense that any number of physical models can be tested or constrained based on the model fits. From Owocki & Cohen (2001): spherically symmetric, two-fluid (hot plasma is int ...
Plasma physics, space research and the origin of the solar system
... of plasmas is also fundamental to our understanding of the origin and evolution of the Solar System, because there are good reasons to believe that the matter which now forms the celestial bodies once was dispersed in a plasma state. The second decade of space research seems to display a different c ...
... of plasmas is also fundamental to our understanding of the origin and evolution of the Solar System, because there are good reasons to believe that the matter which now forms the celestial bodies once was dispersed in a plasma state. The second decade of space research seems to display a different c ...
Time From the Perspective of a Particle Physicist
... glows red (H atom) seen in eclipse • CORONA even lower density and higher T (over 1,000,000 degrees) • SOLAR WIND protons escaping Sun’s gravity so large velocity. Can interact in Earth’s atmosphere ...
... glows red (H atom) seen in eclipse • CORONA even lower density and higher T (over 1,000,000 degrees) • SOLAR WIND protons escaping Sun’s gravity so large velocity. Can interact in Earth’s atmosphere ...
Layers of the Sun Test 1 study guide. Intoduction to Stars
... glows red (H atom) seen in eclipse • CORONA even lower density and higher T (over 1,000,000 degrees) • SOLAR WIND protons escaping Sun’s gravity so large velocity. Can interact in Earth’s atmosphere ...
... glows red (H atom) seen in eclipse • CORONA even lower density and higher T (over 1,000,000 degrees) • SOLAR WIND protons escaping Sun’s gravity so large velocity. Can interact in Earth’s atmosphere ...
The Sun
... Solar Neutrino Puzzle Unreactive and Large mean free path !!! Solar neutrinos originate from the core of the Sun due to thermonuclear reactions and thus offer the possibility of probing solar interior. They are highly unreactive and even pass through the Earth undetected. Flux at Earth is of the ord ...
... Solar Neutrino Puzzle Unreactive and Large mean free path !!! Solar neutrinos originate from the core of the Sun due to thermonuclear reactions and thus offer the possibility of probing solar interior. They are highly unreactive and even pass through the Earth undetected. Flux at Earth is of the ord ...
++ (?) Non-thermal heating
... In both magnetized/unmagnetized planets, strong Bfield lies between the ionosphere and (shocked) SW. 1. Thick ionosphere means higher ionization rate by the electron impact ionization. Extra ionization of neutrals with escape velocity, while these ions cannot escape beyond the magnetized ionopause ...
... In both magnetized/unmagnetized planets, strong Bfield lies between the ionosphere and (shocked) SW. 1. Thick ionosphere means higher ionization rate by the electron impact ionization. Extra ionization of neutrals with escape velocity, while these ions cannot escape beyond the magnetized ionopause ...
journey to the stars - American Museum of Natural History
... anyone’s out there. Voyager continues to travel across the region where the solar wind slams into the surrounding interstellar gas and the Milky Way’s own magnetic field. ...
... anyone’s out there. Voyager continues to travel across the region where the solar wind slams into the surrounding interstellar gas and the Milky Way’s own magnetic field. ...
ppt
... At the end of the XIXe century, scientists were puzzled by the spontaneous discharge of their electroscopes which suggested the presence of an ionizing radiation. In 1909, Wulf noted that the rate of the discharge was decreasing with altitude (Eiffel tower). Between 1911 and 1913 the Austrian physic ...
... At the end of the XIXe century, scientists were puzzled by the spontaneous discharge of their electroscopes which suggested the presence of an ionizing radiation. In 1909, Wulf noted that the rate of the discharge was decreasing with altitude (Eiffel tower). Between 1911 and 1913 the Austrian physic ...
COSPAR WORKSHOP ON CAPACITY DEVELOPMENT
... In ordinary fluid flow tangential stress (or drag as sometimes called) is caused by the viscous interaction Particles are scattered from the moving fluid into the stationary fluid adding momentum, i.e. exerting a force on the boundary A flowing boundary layer is produced In a collisionless plasma pa ...
... In ordinary fluid flow tangential stress (or drag as sometimes called) is caused by the viscous interaction Particles are scattered from the moving fluid into the stationary fluid adding momentum, i.e. exerting a force on the boundary A flowing boundary layer is produced In a collisionless plasma pa ...
Relationship between solar wind dynamic pressure and amplitude
... 1994). A computer simulation by Li et al. (1993) shows that a strong magnetopause compression occurred at 15 h LT and a produced hydromagnetic pulse propagated tail-ward accelerating magnetospheric particles to form the inner radiation belt which lasted nearly 1 year. The amplitude of the electric ...
... 1994). A computer simulation by Li et al. (1993) shows that a strong magnetopause compression occurred at 15 h LT and a produced hydromagnetic pulse propagated tail-ward accelerating magnetospheric particles to form the inner radiation belt which lasted nearly 1 year. The amplitude of the electric ...
Solar wind
![](https://commons.wikimedia.org/wiki/Special:FilePath/Solar_wind_Speed_interplanetary_magnetic_field.jpg?width=300)
The solar wind is a stream of charged particles released from the upper atmosphere of the Sun. This plasma consists of mostly electrons, protons and alpha particles with energies usually between 1.5 and 10 keV; embedded in the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar longitude. Its particles can escape the Sun's gravity because of their high energy, from the high temperature of the corona and magnetic, electrical and electromagnetic phenomena in it.The solar wind flows outward supersonically to great distances, filling a region known as the heliosphere, an enormous bubble-like volume surrounded by the interstellar medium. Other related phenomena include the aurora (northern and southern lights), the plasma tails of comets that always point away from the Sun, and geomagnetic storms that can change the direction of magnetic field lines and create strong currents in power grids on Earth.