Anisotropy - IIT Kanpur
... 100 degrees by 50 degrees around the South Galactic Pole Intensities scaled to the number of galaxies blue, green and red for bright, medium and faint galaxies ...
... 100 degrees by 50 degrees around the South Galactic Pole Intensities scaled to the number of galaxies blue, green and red for bright, medium and faint galaxies ...
Fundamentals of Radio Astronomy - Radio Observations of Active
... • From Maxwell’s equations E•B=0 (E and B perpendicular) – By convention, we consider the time behavior of the E-field in a fixed perpendicular plane, from the point of view of the receiver. ...
... • From Maxwell’s equations E•B=0 (E and B perpendicular) – By convention, we consider the time behavior of the E-field in a fixed perpendicular plane, from the point of view of the receiver. ...
No Slide Title
... • Magnetospheric Accretion Models – Require magnetic field strengths from 0.1-5 kG for specific stars – Yield fields that differ by scale factors related to assumed coupling – Imply stellar field not simply function of mass, radius, and rotation ...
... • Magnetospheric Accretion Models – Require magnetic field strengths from 0.1-5 kG for specific stars – Yield fields that differ by scale factors related to assumed coupling – Imply stellar field not simply function of mass, radius, and rotation ...
Polarimetric technique to study (pre)biological organics in cosmic dust Lev Nagdimunov
... Eliel et al., 1994), where the circular dichroism and/or optical rotatory dispersion change sign through an electronic absorption band. Although the simulated trend of circular polarization spectra is well matched to the laboratory data and suggests that our model correctly reproduces polarization t ...
... Eliel et al., 1994), where the circular dichroism and/or optical rotatory dispersion change sign through an electronic absorption band. Although the simulated trend of circular polarization spectra is well matched to the laboratory data and suggests that our model correctly reproduces polarization t ...
McConnell XGPolarimetry SSE
... of the radiation. Such polarization can be measured relative to the plane defined by this preferred direction and the direction to the observer. For gamma-ray bursts, for example, the preferred direction may be the axis of the jet; in pulsars, it may be the magnetic axis; near black holes or neutron ...
... of the radiation. Such polarization can be measured relative to the plane defined by this preferred direction and the direction to the observer. For gamma-ray bursts, for example, the preferred direction may be the axis of the jet; in pulsars, it may be the magnetic axis; near black holes or neutron ...
Multidimensional and inhomogeneity effects on scattering
... He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the magnetic field, one usually assumes that the emergent spectral line is formed by single scattering (optically thin regime) of the incident continuum radiation, or, in a bi ...
... He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the magnetic field, one usually assumes that the emergent spectral line is formed by single scattering (optically thin regime) of the incident continuum radiation, or, in a bi ...
Investigation of the Earth Ionosphere using the Radio Emission of
... (2) A random number generator has formed the first array of amplitudes A0 (k) which had the Rayleigh distribution with the given r.m.s. deviation (σ1 ). Each amplitude in the array matched its radio frequency, see Equation (1) below; (3) The second amplitude array B0 (k), which had a similar distrib ...
... (2) A random number generator has formed the first array of amplitudes A0 (k) which had the Rayleigh distribution with the given r.m.s. deviation (σ1 ). Each amplitude in the array matched its radio frequency, see Equation (1) below; (3) The second amplitude array B0 (k), which had a similar distrib ...
Quest 1Waves - SFP Online!
... D. in phase 5. As observed from the Earth, the light from a star is shifted toward lower frequencies. This is an indication that the distance between the Earth and the star is A. decreasing B. increasing C. constant 6. Which point on the wave diagram below is in phase with point A? ...
... D. in phase 5. As observed from the Earth, the light from a star is shifted toward lower frequencies. This is an indication that the distance between the Earth and the star is A. decreasing B. increasing C. constant 6. Which point on the wave diagram below is in phase with point A? ...
Polarimetry: a powerful diagnostic tool in astronomy
... by absorption, so at least some of the interstellar grains must be aligned, and hence must be nonspherical. How the grains are aligned has been the subject of many papers (e.g. those of Alex Lazarian) and it is probable that different mechanisms operate in different environments. In the early 1970s ...
... by absorption, so at least some of the interstellar grains must be aligned, and hence must be nonspherical. How the grains are aligned has been the subject of many papers (e.g. those of Alex Lazarian) and it is probable that different mechanisms operate in different environments. In the early 1970s ...
as a PDF
... SPHERE-ZIMPOL1,2,3,4 (Spectro-Polarimetric High Contrast Exoplanet Research - Zurich Imaging Polarimeter) is one of the first instruments which aim for the direct detection of reflected light from extra-solar planets. The instrument will search for direct light from old planets with orbital periods ...
... SPHERE-ZIMPOL1,2,3,4 (Spectro-Polarimetric High Contrast Exoplanet Research - Zurich Imaging Polarimeter) is one of the first instruments which aim for the direct detection of reflected light from extra-solar planets. The instrument will search for direct light from old planets with orbital periods ...
zaneposter
... We implemented in XSPEC two model tables. The first one is angleaveraged, and spectra depend on 4 parameters: - kT: the BB temperature of the seed surface photons; - bulk: the bulk velocity of the magnetospheric currents - : the twist angle of the magnetosphere (zero for untwisted dipole) - K: a ...
... We implemented in XSPEC two model tables. The first one is angleaveraged, and spectra depend on 4 parameters: - kT: the BB temperature of the seed surface photons; - bulk: the bulk velocity of the magnetospheric currents - : the twist angle of the magnetosphere (zero for untwisted dipole) - K: a ...
Space-Variant Polarization Patterns of Non-Collinear Poincare Superpositions
... Space-variant polarization is an interesting case study of complex light fields. Since eyes and cameras are oblivious to polarization, a rich aspect of light waves is largely ignored because it is unseen. Yet, extraordinary complexity is ubiquitous. Linear superposition is at the heart of this probl ...
... Space-variant polarization is an interesting case study of complex light fields. Since eyes and cameras are oblivious to polarization, a rich aspect of light waves is largely ignored because it is unseen. Yet, extraordinary complexity is ubiquitous. Linear superposition is at the heart of this probl ...
Unusually large polarizabilities of excited states of Ba
... interaction on handedness Photo-multiplier tubes Oven Collimator Ytterbium atoms ...
... interaction on handedness Photo-multiplier tubes Oven Collimator Ytterbium atoms ...
Document
... state, for higher spins, there are more degrees of freedom, and many spin states yield the same P. For 8 Li+ 4 parameters specify the spin state1 , and specifying P leaves 3. Also, unlike spin 1/2 particles, 8 Li+ has an electric quadrupole moment that couples the spin to the local EFG, which is gen ...
... state, for higher spins, there are more degrees of freedom, and many spin states yield the same P. For 8 Li+ 4 parameters specify the spin state1 , and specifying P leaves 3. Also, unlike spin 1/2 particles, 8 Li+ has an electric quadrupole moment that couples the spin to the local EFG, which is gen ...
Strong linear polarization of V4332 Sagittarii: a dusty disc geometry⋆
... spectrum observed in the optical would in fact be the giant spectrum scattered on dust grains in the disc. In this case, forward scattering on big dust grains at the outer edge of the disc is most effective in producing the observed radiation. However, the expected polarization degree is small, if sc ...
... spectrum observed in the optical would in fact be the giant spectrum scattered on dust grains in the disc. In this case, forward scattering on big dust grains at the outer edge of the disc is most effective in producing the observed radiation. However, the expected polarization degree is small, if sc ...
Coronal Polarization Measurements and
... small dust particles in the ecliptic plane results in the Fraunhofer (or F-) corona, named for the photospheric Fraunhofer absorption lines it displays (Golub and Pasachoff, 1997, p. 3-6). Often the first task of a scientist studying coronal light is to separate the contributions from each of these ...
... small dust particles in the ecliptic plane results in the Fraunhofer (or F-) corona, named for the photospheric Fraunhofer absorption lines it displays (Golub and Pasachoff, 1997, p. 3-6). Often the first task of a scientist studying coronal light is to separate the contributions from each of these ...
Radiative Processes in Astrophysics. Radio Polarization
... Faraday rotation can occur within the ionised plasma responsible for the observed synchrotron radiation. Since a single electron’s contribution to the Faraday rotation is inversely proportional to the square of the electron’s effective mass (equation 18), relativistic electrons such as those respons ...
... Faraday rotation can occur within the ionised plasma responsible for the observed synchrotron radiation. Since a single electron’s contribution to the Faraday rotation is inversely proportional to the square of the electron’s effective mass (equation 18), relativistic electrons such as those respons ...
Talk - IIT Kanpur
... A common model for dark energy is a scalar field slowly rolling towards its true vacuum ...
... A common model for dark energy is a scalar field slowly rolling towards its true vacuum ...
X-ray polarimetry in astrophysics
... Gamma-ray bursts are the most energetic events in the Universe, with radiated energy up to 1054 erg. The collapse of a massive rotating star produces a hot fireball which is ejected at relativistic velocity in form of a jet. Internal shocks are responsible for the observed variability (prompt emissi ...
... Gamma-ray bursts are the most energetic events in the Universe, with radiated energy up to 1054 erg. The collapse of a massive rotating star produces a hot fireball which is ejected at relativistic velocity in form of a jet. Internal shocks are responsible for the observed variability (prompt emissi ...
Alexander Polnarev QMUL, SPA 28 March 2014
... The solution is localized around the visibility function (around the epoch of recombination). Physically this is a consequence of the fact that: on the one hand due to the enormous optical depth before recombination we cannot see the polarization generated much before recombination on the other hand ...
... The solution is localized around the visibility function (around the epoch of recombination). Physically this is a consequence of the fact that: on the one hand due to the enormous optical depth before recombination we cannot see the polarization generated much before recombination on the other hand ...
X-ray polarimetry in Xenon gas filled detectors
... (θ is the polar angle relative to the x-ray propagation direction, θ and φ are the polar and azimuthal angles relative to the polarization direction, β is the dipole asymmetry parameter and P2 is the 2nd Legendre polynomial) Derevianko et. al., At.Dat.Nucl.Dat. Tables 73 (1999) 153 ...
... (θ is the polar angle relative to the x-ray propagation direction, θ and φ are the polar and azimuthal angles relative to the polarization direction, β is the dipole asymmetry parameter and P2 is the 2nd Legendre polynomial) Derevianko et. al., At.Dat.Nucl.Dat. Tables 73 (1999) 153 ...
Three-year WMAP Observations: Method and Results
... era (free-fall time scale is longer than the expansion time scale during the radiation era), ISW effect increases anisotropy at around the Horizon size at the equality. ...
... era (free-fall time scale is longer than the expansion time scale during the radiation era), ISW effect increases anisotropy at around the Horizon size at the equality. ...
Circular polarization
In electrodynamics, circular polarization of an electromagnetic wave is a polarization in which the electric field of the passing wave does not change strength but only changes direction in a rotary manner.In electrodynamics the strength and direction of an electric field is defined by what is called an electric field vector. In the case of a circularly polarized wave, as seen in the accompanying animation, the tip of the electric field vector, at a given point in space, describes a circle as time progresses. If the wave is frozen in time, the electric field vector of the wave describes a helix along the direction of propagation.Circular polarization is a limiting case of the more general condition of elliptical polarization. The other special case is the easier-to-understand linear polarization.The phenomenon of polarization arises as a consequence of the fact that light behaves as a two-dimensional transverse wave.