A Magneto-Gravitational Ultracold Neutron Trap
... shown in blue. In each case, events for times after the vanadium has been raised into the detector array are included. . . . . . . . . . . . . . . . . . . . . . . . . ...
... shown in blue. In each case, events for times after the vanadium has been raised into the detector array are included. . . . . . . . . . . . . . . . . . . . . . . . . ...
Pinned vortex hopping in a neutron star crust
... site to another giving rise to a more gradual creep. We find that there is a significant range of parameter space in which avalanches can be triggered, thus supporting the hypothesis that they may lie at the origin of pulsar glitches. For realistic values of the pinning force and superfluid drag par ...
... site to another giving rise to a more gradual creep. We find that there is a significant range of parameter space in which avalanches can be triggered, thus supporting the hypothesis that they may lie at the origin of pulsar glitches. For realistic values of the pinning force and superfluid drag par ...
Boron-10 layers, Neutron Reflectometry and Thermal Neutron
... magnifying glass. They have no charge, and their electric dipole moment is either zero or too small to be measured. For these reasons, neutrons can penetrate matter far better than charged particles and it is also why they are relatively hard to be detected. Available neutron beams have inherently l ...
... magnifying glass. They have no charge, and their electric dipole moment is either zero or too small to be measured. For these reasons, neutrons can penetrate matter far better than charged particles and it is also why they are relatively hard to be detected. Available neutron beams have inherently l ...
VIRGO status and GW physics
... – Doppler frequency shift, amplitude modulation from antenna pattern – For a triaxial star, expect GW signal at twice the spin frequency ...
... – Doppler frequency shift, amplitude modulation from antenna pattern – For a triaxial star, expect GW signal at twice the spin frequency ...
Power Point Presentation
... Neutron stars are supported by pressure from degenerate neutrons, formed from collapsed electrons and protons A teaspoonful of neutron star would weigh 1 billion ...
... Neutron stars are supported by pressure from degenerate neutrons, formed from collapsed electrons and protons A teaspoonful of neutron star would weigh 1 billion ...
Galactic Windmills - Dr. Karl Remeis
... electromagnetic force can work in two directions, and that as soon as equal amounts of positive and negative charges are put together, they become neutral and no force is present anymore. Gravity on the other side is a much more global force, as it acts on all matter with mass, including all baryoni ...
... electromagnetic force can work in two directions, and that as soon as equal amounts of positive and negative charges are put together, they become neutral and no force is present anymore. Gravity on the other side is a much more global force, as it acts on all matter with mass, including all baryoni ...
Gamma Ray Bursts
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
A New Search for the Neutron Electric Dipole Moment Funding Pre-proposal
... both weak and strong interactions. The experiment is based on the magnetic resonance technique of rotating a magnetic dipole moment in a magnetic field. We describe in this report a new method to make a precision measurement of the neutron precession frequency under the influence of an electric fiel ...
... both weak and strong interactions. The experiment is based on the magnetic resonance technique of rotating a magnetic dipole moment in a magnetic field. We describe in this report a new method to make a precision measurement of the neutron precession frequency under the influence of an electric fiel ...
Coherent Control of Polarized Neutron Interferometry
... interferometer to separate two paths where spin states are independently manipulated. The final measurement is made on the spin degree of freedom, so we observe spinbased contrast without a need for coherence in the path degree of freedom. This is difficult to achieve in a spin-echo interferometer b ...
... interferometer to separate two paths where spin states are independently manipulated. The final measurement is made on the spin degree of freedom, so we observe spinbased contrast without a need for coherence in the path degree of freedom. This is difficult to achieve in a spin-echo interferometer b ...
Neutron Data Booklet
... parameters involving nucleons (i.e. neutron, proton), but not the many neutron results on symmetry tests and basic interactions involving nuclei. For more details see also the compilation of the Particle Data Group, www-pdg.lbl.gov and [2], from which most of our data are taken, as well as the confe ...
... parameters involving nucleons (i.e. neutron, proton), but not the many neutron results on symmetry tests and basic interactions involving nuclei. For more details see also the compilation of the Particle Data Group, www-pdg.lbl.gov and [2], from which most of our data are taken, as well as the confe ...
Neutron Data Booklet - Institut Laue
... where a more direct relation between the scattering length and the measurable quantities exist [4,11]. That means, less corrections must be performed during the data evaluation and the accuracy of the deduced quantity becomes much higher. The considerable efforts to determine scattering lengths with ...
... where a more direct relation between the scattering length and the measurable quantities exist [4,11]. That means, less corrections must be performed during the data evaluation and the accuracy of the deduced quantity becomes much higher. The considerable efforts to determine scattering lengths with ...
MAGNETIC FIELDS IN NEUTRON STARS Daniele Viganò
... Supernovae are very bright and short-lasting stellar explosions. During the last two millennia, at least seven of them happened close enough to be detected by human eye and reported in historical records by different populations, mainly in China (Clark & Stephenson, 1982). Conversely, observations o ...
... Supernovae are very bright and short-lasting stellar explosions. During the last two millennia, at least seven of them happened close enough to be detected by human eye and reported in historical records by different populations, mainly in China (Clark & Stephenson, 1982). Conversely, observations o ...
Neutron Scattering Instrumentation
... present with what probability at any time t and at any place r along the beam trajectory. Optical elements, for example, reshape phase space elements by concentrating the beam intensity in space or by rendering the beam more parallel. It is the transformation of phase space elements that fully char ...
... present with what probability at any time t and at any place r along the beam trajectory. Optical elements, for example, reshape phase space elements by concentrating the beam intensity in space or by rendering the beam more parallel. It is the transformation of phase space elements that fully char ...
Type II SuperNova - University of Dayton
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
An X-Ray, Optical and Infra-red study of High-Mass X
... inspiring mountain top, and I thank Malcolm for being so insistent that I go to as many as possible! When Malcolm wasn’t around there was always two people I could turn to for advice. Matthew and Vanessa, thank you for all your help during the early years of my Ph.D. and your continued willingness t ...
... inspiring mountain top, and I thank Malcolm for being so insistent that I go to as many as possible! When Malcolm wasn’t around there was always two people I could turn to for advice. Matthew and Vanessa, thank you for all your help during the early years of my Ph.D. and your continued willingness t ...
GLAST Science at Lunch - Aug 11, 2005
... The binary system LS 5039, at a distance of about 3 kpc, was discovered by Motch et al. 1997, crosscorrelating X-ray sources from the ROSAT catalog with OB star catalogues in order to locate systems made of a compact X-ray source orbiting a massive star. Using the VLA radio interferometer, Marti et ...
... The binary system LS 5039, at a distance of about 3 kpc, was discovered by Motch et al. 1997, crosscorrelating X-ray sources from the ROSAT catalog with OB star catalogues in order to locate systems made of a compact X-ray source orbiting a massive star. Using the VLA radio interferometer, Marti et ...
Rotating White Dwarfs and Neutron Stars in - Padis
... collectively planet-like objects, white dwarfs, neutron stars, other exotic dense stars, and black holes. It is well known that Newtonian theory of gravitation provides an adequate description of the gravitational field of conventional astrophysical objects. However, the discovery of exotic compact ...
... collectively planet-like objects, white dwarfs, neutron stars, other exotic dense stars, and black holes. It is well known that Newtonian theory of gravitation provides an adequate description of the gravitational field of conventional astrophysical objects. However, the discovery of exotic compact ...
Untitled - METU Astrophysics Home Page
... calculations of neutron star mass and radii. However, the first observational evidence of a rotation powered pulsar hasn’t come until 1967, when Bell detected radio pulsations from outside the solar system which later was understood to be the first detection of a pulsar by the humankind. Following t ...
... calculations of neutron star mass and radii. However, the first observational evidence of a rotation powered pulsar hasn’t come until 1967, when Bell detected radio pulsations from outside the solar system which later was understood to be the first detection of a pulsar by the humankind. Following t ...
Final Stages of Stellar Evolution - supernovae and the synthesis of
... Naming of Supernovae prefix “SN” followed by year of discovery first 26 supernovae upper case letter from A to Z following combination of lower case letters aa to zz eg. SN1987A was the first observed supernova in 1987 last supernova in 2005: SN2005nc ...
... Naming of Supernovae prefix “SN” followed by year of discovery first 26 supernovae upper case letter from A to Z following combination of lower case letters aa to zz eg. SN1987A was the first observed supernova in 1987 last supernova in 2005: SN2005nc ...
Solutions to the excercises
... inhalation or food intake. Finally, the biological effect can be quantized as 20 times higher than an equivalent of beta or gamma radiation. ...
... inhalation or food intake. Finally, the biological effect can be quantized as 20 times higher than an equivalent of beta or gamma radiation. ...
Finite Temperature Effects in the White Dwarf - Padis
... neutron stars (mass, radius, rotation velocity, thermal evolution, etc.) are extremely sensitive to the star’s composition. In this way, taking into account the analysis of these properties, it is possible to constrain the equation of state of dense matter and its composition. In particular, in this ...
... neutron stars (mass, radius, rotation velocity, thermal evolution, etc.) are extremely sensitive to the star’s composition. In this way, taking into account the analysis of these properties, it is possible to constrain the equation of state of dense matter and its composition. In particular, in this ...
Quark matter influence on observational - Instituut
... of Theoretical Physics of the Vrije Universiteit, as my Master’s research the combined Masters for Theoretical Physics and Astronomy and Astrophysics. The theory of colour interactions (QCD) has the peculiar behaviour that the interaction strength declines for higher energies. Therefore, calculation ...
... of Theoretical Physics of the Vrije Universiteit, as my Master’s research the combined Masters for Theoretical Physics and Astronomy and Astrophysics. The theory of colour interactions (QCD) has the peculiar behaviour that the interaction strength declines for higher energies. Therefore, calculation ...
Lecture Notes
... Menkar, Shedir, Algorah, Propus, and numerous others probably are, we may then look upon them as sufficiently out of reach of mutual attractions, to deserve the name of insulated stars. If a certain star should be situated at any, perhaps immense, distance behind another, and but very little deviati ...
... Menkar, Shedir, Algorah, Propus, and numerous others probably are, we may then look upon them as sufficiently out of reach of mutual attractions, to deserve the name of insulated stars. If a certain star should be situated at any, perhaps immense, distance behind another, and but very little deviati ...
Power Point - Stanford University
... Expect ~200 Hz for a 10 solar mass nonspinning BH. This implies that the disk extends very close to the hole, and the hole has spin in the direction of the rotation of the accretion disk. The right most line has no break point (Dc2 = 0.8). Thus it is not likely that we have yet seen the inner edge o ...
... Expect ~200 Hz for a 10 solar mass nonspinning BH. This implies that the disk extends very close to the hole, and the hole has spin in the direction of the rotation of the accretion disk. The right most line has no break point (Dc2 = 0.8). Thus it is not likely that we have yet seen the inner edge o ...
The Confrontation between General Relativity and Experiment
... experiments were carried out primarily to search for a “fifth force” (see Sec. 2.3), but their null results also constituted tests of WEP. In the “free-fall Galileo experiment” performed at the University of Colorado, the relative free-fall acceleration of two bodies made of uranium and copper was ...
... experiments were carried out primarily to search for a “fifth force” (see Sec. 2.3), but their null results also constituted tests of WEP. In the “free-fall Galileo experiment” performed at the University of Colorado, the relative free-fall acceleration of two bodies made of uranium and copper was ...
Pulsar
A pulsar (short for pulsating radio star) is a highly magnetized, rotating neutron star that emits a beam of electromagnetic radiation. This radiation can only be observed when the beam of emission is pointing toward Earth, much the way a lighthouse can only be seen when the light is pointed in the direction of an observer, and is responsible for the pulsed appearance of emission. Neutron stars are very dense, and have short, regular rotational periods. This produces a very precise interval between pulses that range roughly from milliseconds to seconds for an individual pulsar. Pulsars are believed to be one of the candidates of high and ultra-high energy astroparticles (see also Centrifugal mechanism of acceleration).The precise periods of pulsars make them useful tools. Observations of a pulsar in a binary neutron star system were used to indirectly confirm the existence of gravitational radiation. The first extrasolar planets were discovered around a pulsar, PSR B1257+12. Certain types of pulsars rival atomic clocks in their accuracy in keeping time.