... The behaviour of the polarization efficiency (see Eq. ( 14 )) for non-absorbing and absorbing spheroids is shown in Fig. 11 for the case when a maximum polarization is expected (PF alignment, ). ... Figure 11: Polarization efficiency against for prolate and oblate spheroids with and , picket fence orientation, . The size/shape effects are illustrated. ... Figure: Polarization efficiency as a function of particle equivolume radius for prolate core-mantle spheroids with and , PF orientation, . ...

... Energetic magnetospheric ions are often unstable to the electromagnetic ion cyclotron (EMIC) instability . ... generation of EMIC waves below the proton gyrofrequency , and . ... Depending on the local proton gyrofrequency, the frequency of the EMIC waves varies: in the magnetosphere we deal with the ULF range (more precisely 0.1-5 Hz), while in the auroral field lines we have ELF waves (tens or hundreds of Hz; see radio frequencies and flickering aurora ). ... Space Physics Text Book of Oulu ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

Wave-Particle Duality of Light. click here to see a wave experiment . ... In the wave theory, greater light intensity simply means more photons. Each photon ejects electrons in the same way, so more intensity means more electrons. Threshold frequency and electron K.E. should not be affected by intensity. ... Light frequencies below the threshold eject no electrons, no matter how intense the light. Light frequencies above the threshold eject electrons, no matter how low the intensity. ...

... The polarimetry group at the Arcetri Observatory has been working for several years, mainly from the theoretical-interpretative side, on the polarization of the radiation emitted by objects of astrophysical interest. ... E. Landi Degl'Innocenti "The physics of polarization" in "Astrophysical Spectropolarimetry", J. Trujillo Bueno, F. Moreno Insertis, F. Sanchez (eds.), Cambridge University Press, 1. ... E. Landi Degl'Innocenti "The Zeeman effect: applications to solar physics" Astron. ...

... It should be recalled that most (99.99 percent) of the energy is dissipated by single radiopulsars in the form of relativistic particles and low-frequency electromagnetic waves which are not observable. ... This gives rise to an interesting analog of the classical reflection or heating effect (Lipunov, 1980[ 97 ]; Lipunov and Prokhorov, 1984[ 110 ]; Harding, 1991[ 64 ]; Lipunov and Nazin, 1994[ 119 ]). ... For close binary systems, -0.3 and the transformation coefficient may be several percent. ...

... a) As source material for the high-school or college curriculum, especially in physics. astronomy and their history. (b) As a source of supplemental projects by high school students or by undergraduates. (c) As material for independent studies, In particular by motivated students who seek to know more about space . ... Those wishing to look up specific topics are advised to use the index file, accessible from the end of any "Exploration" file. ... files not listed and at other resource material. ...