Description:    Pitch-angle diffusion coefficients of electrons have been calculated for resonant interaction with electrostatic electron-cyclotron harmonic (ECH) waves using quasi linear diffusion theory. Calculations have been performed for the planets Earth and Jupiter at three radial distances for each planet. Electron precipitation fluxes have also been calculated and compared with observed fluxes. At Earth, electrons of energy ≤200 eV may be put on strong diffusion at L = 10. At lower L values, observed ECH wave amplitudes are insufficient to put electrons on strong diffusion. At Jupiter, electrons can be put on strong diffusion at all L values. However, the energy of electrons which may be put on strong diffusion decreases from about 1 keV at L = 7 to ~100 eV at L = 17. It is concluded that ECH waves may be partly responsible for diffuse auroral precipitation of low energy electrons at Jupiter for lower L values. At Earth contribution of ECH waves to diffuse aurora is quite small. Content Type Journal Article Pages 1-17 DOI 10.1007/s11038-012-9407-x Authors A. K. Tripathi, Department of Applied Physics, Institute of Technology, Banaras Hindu University, Varanasi, 221005 India R. P. Singhal, Department of Applied Physics, Institute of Technology, Banaras Hindu University, Varanasi, 221005 India K. P. Singh, Department of Electronics Engineering, Institute of Technology, Banaras Hindu University, Varanasi, 221005 India O. N. Singh II, Department of Applied Physics, Institute of Technology, Banaras Hindu University, Varanasi, 221005 India Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    We studied the relation between the near-Earth signatures of the interplanetary coronal mass ejections (ICMEs) shocks such as sudden storms commencement (SSC), and their counterparts of coronal mass ejections (CMEs) observed near-Sun by solar and heliospheric observatory (SOHO)/large angle and spectrometric coronagraph (LASCO) coronagraph during 1996–2008. Our result showed that there is a good correlation between the travel time of the ICMEs shocks and their associated radial speeds. Also we have separated the ICME shocks into two groups according to their effective acceleration and deceleration. The results showed that the faster ICME shocks (with negative accelerations which decelerated by solar wind plasma) are more correlated to their associated travel time than those with positive accelerations. Content Type Journal Article Pages 1-15 DOI 10.1007/s11038-012-9398-7 Authors M. Youssef, National Research Institutes of Astronomy and Geophysics (NRIAG), Helawn, Egypt Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    Using the standard reductive perturbation technique, nonlinear cylindrical and spherical Kadomtsev-Petviashvili (KP) equations are derived for the propagation of ion acoustic solitary waves in an unmagnetized collisionless plasma with nonthermal electrons and warm ions. The influence of nonthermally distributed electrons and the effects caused by the transverse perturbation on cylindrical and spherical ion acoustic waves (IAWs) are investigated. It is observed that the presence of nonthermally distributed electrons has a significant role in the nature of ion acoustic waves. In particular, when the nonthermal distribution parameter β takes certain values the usual cylindrical KP equation (CKPE) and spherical KP equation (SKPE) become invalid. One then has to have recourse to the modified CKPE or SKPE. Analytical solutions of both CKPE and SKPE and their modified versions are discussed in the present paper. The present investigation may have relevance in the study of propagation of IAWs in space and laboratory plasmas. Content Type Journal Article Pages 1-13 DOI 10.1007/s11038-012-9405-z Authors Biswajit Sahu, Department of Mathematics, West Bengal State University, Barasat, Kolkata, 700126 India Rajkumar Roychoudhury, Physics and Applied Mathematics Unit, Indian Statistical Institute, Kolkata, 700108 India Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    The Carancas meteorite fell on 15 September 2007 approximately 10 km south of Desaguadero, near Lake Titicaca, Peru, producing bright lights, clouds of dust in the sky and intense detonations. The Carancas meteorite is classified as a H4–5 ordinary chondrite with shock stage S3 and a degree of weathering W0. The Carancas meteorite is characterized by well defined chondrules composed either of olivine or pyroxene. The Mössbauer spectra show an overlapping of paramagnetic and magnetic phases. The spectra show two quadrupole doublets associated to olivine and pyroxene; and two magnetic sextets, associated with the primary phases kamacite/taenite and Troilite (Fe 2+ ). Metal particles were extracted from the bulk powdered samples exhibit only kamacite and small amounts of the intergrowth tetrataenite/antitaenite. X-Ray diffractogram shows the primary phases olivine, pyroxene, troilite, kamacite, diopside and albite. Iron oxides has not been detected by Mössbauer spectroscopy or XRD as can be expected for a meteorite immediately recovered after its fall. Content Type Journal Article Pages 1-9 DOI 10.1007/s11038-012-9406-y Authors P. Munayco, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rua Xavier Sigaud 150, Rio de Janeiro, 22290-180 Brazil J. Munayco, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rua Xavier Sigaud 150, Rio de Janeiro, 22290-180 Brazil M. E. Varela, Instituto de Ciencias Astronómicas de la Tierra y del Espacio (ICATE/CONICET), Av. España 1512 Sur, CPJ5402DSP San Juan, Argentina R. B. Scorzelli, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rua Xavier Sigaud 150, Rio de Janeiro, 22290-180 Brazil Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    The use of lithosphere strength indicators (as for example the effective elastic thickness of the lithosphere or the depth to the brittle-ductile transition) can give clues on the surface heat flow and the thermal state of the ice crust of icy satellites, which in turn has profound implications for the internal evolution, and the possible existence of internal oceans, in these planetary bodies. As shown in this review, this kind of approach has found very high (and possibly recent) surface heat flows for Europa and ancient high heat flows for Ganymede. On the other hand, the heavily cratered of Callisto suggests a cold and inactive outer ice shell throughout the entire history of that body. However, irrespective of the greatly different geology recorded on the surface of the icy Galilean satellites, there is evidence from orbital magnetic observations for internal oceans in all them. By considering heat flow estimates in the context existence of internal oceans, a more complete description of the thermal history of the icy Galilean satellites should emerge. Content Type Journal Article Pages 1-9 DOI 10.1007/s11038-012-9403-1 Authors Javier Ruiz, Departamento de Geodinámica, Facultad de Ciencias Geológicas, Universidad Complutense de Madrid, 28040 Madrid, Spain Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    The paper is devoted to calculation of the precessional effect of the orbit of a two-body system in its geodesic motion through the deformed spacetime of a third body assumed non-rotating. The obtained result is generic, in that no specific assumption on the orbit geometry is made Content Type Journal Article Pages 1-5 DOI 10.1007/s11038-012-9402-2 Authors G. Renzetti, Pescara, Italy Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    Varre-Sai, the most recent Brazilian meteorite fall, on June 19th, 2010 at Varre-Sai, in Rio de Janeiro State, Brazil (20°51′41″S; 41°44′.80″W). At least eight masses (total ~3.5 kg) were recovered. Most are totally covered by fusion crust. The exposed interior is of light-grey colour with a few dark shock veins. Five thin polished and etched sections were prepared from a slice weighing 35 g on deposit at the National Museum/UFRJ. It consists mostly of chondrules ranging in size from 0.35 to ~2.2 mm, and chondrule fragments enclosed in a crystalline matrix. The matrix consists of tiny isolated subhedral and anhedral crystals and opaque minerals that are intergrown with broken chondrules. The chondritic texture is poorly defined with chondrule textures that vary from non-porphyritic to porphyritic ones. The essential minerals are olivine (Fa 25±0.2 ) and low-Ca pyroxene (Fa 21.66±0.2 Wo 1.4 ). Accessory minerals are plagioclase, apatite, Fe–Ni metal phases, troilite, chromite and magnetite. Mössbauer spectroscopy analysis confirms that the mineral phases are olivine, pyroxene, troilite and kamacite/taenite. Chemical data indicate that Varre-Sai is a member of the low iron L chondrite group. The observed texture and mineral phases led us to classify Varre-Sai as an equilibrated petrologic type 5. The shock features of the minerals (undulatory extinction, planar structure and numerous cracks), as well as plagioclase partial or totally transformed to maskelynite, suggest a shock stage S4. Also, some post-impact metamorphic processes could be inferred from the meta-sulfide conjoint grains that show complex mixtures of kamacite–taenite–tetrataenite and troilite. The occurrence of veins crosscutting the studied sections indicates that Varre-Sai was affected by a late fracturing event. Sealing of these fractures must have been a fast process, as shown by troilite globule textures pointing towards rapid solidification. The meteorite name was approved by the Nomenclature Committee of the Meteoritical Society (Meteoritic Bulletin, no 99). Content Type Journal Article Pages 1-11 DOI 10.1007/s11038-012-9401-3 Authors M. E. Zucolotto, Museu Nacional/UFRJ, Rio de Janeiro, RJ, Brazil L. L. Antonello, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rio de Janeiro, Brazil M. E. Varela, ICATE-CONICET, Av España 1512 Sur, San Juan, J5402DSP Argentina R. B. Scorzelli, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rio de Janeiro, Brazil P. Munayco, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rio de Janeiro, Brazil E. dos Santos, Centro Brasileiro de Pesquisas Físicas (CBPF/MCT), Rio de Janeiro, Brazil Isabel P. Ludka, Instituto de Geociências/UFRJ, Rio de Janeiro, RJ, Brazil Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    Using particle aspect approach, the effect of multi-ions densities on the dispersion relation, growth rate, perpendicular resonant energy and growth length of electromagnetic ion cyclotron wave with general loss-cone distribution function in hot anisotropic multi-ion plasma is presented for auroral acceleration region. It is observed that higher He + and O + ions densities enhance the wave frequency closer to the H + ion cyclotron frequency and growth rate of the wave. The differential heating of He + ions perpendicular to the magnetic field is enhanced at higher densities of He + ions. The waves require longer distances to achieve observable amplitude by wave-particle interactions mechanism as predicted by growth length. It is also found that electron thermal anisotropy of the background plasma enhances the growth rate and reduces the growth length of multi-ions plasma. These results are determined for auroral acceleration region. Content Type Journal Article Pages 1-13 DOI 10.1007/s11038-012-9400-4 Authors Soniya Patel, Department of Physics, Dr. H.S.Gour Central University, Sagar, MP 470003, India P. Varma, Department of Physics, Dr. H.S.Gour Central University, Sagar, MP 470003, India M. S. Tiwari, Department of Physics, Dr. H.S.Gour Central University, Sagar, MP 470003, India Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    Acoustic radiation is the signal of choice for exploring Earth’s oceans. Its potential application for the oceans of icy moons requires investigation. However acoustic technology needs to be treated with care for extra-terrestrial purposes. Instruments, calibrations, and predictive codes that have served well on Earth may require fundamental redesign for use on other worlds. However when such an assessment is achieved, acoustic signals open up the possibility of exploring volumes exceeding one million cubic kilometres in a few minutes. This paper begins at tutorial level for novice acousticians, illustrating the principles by which acoustics can be used to monitor the environment at great distances from the source, both by projecting out signals and by using natural signals of opportunity. It then progresses to calculations for a generic icy moon (which resembles, but does not model Europa), proceeding from tutorial calculations of ‘flat world’ models to calculate the propagation times for pulses to circumpropagate around the entire moon. Given that a single emitted pulse can produce multiple arrivals from different propagation paths, the paper discusses how the structure of the received time history can be used to monitor changes in the temperature profile in the ocean, position of the water/ice layer and the asphericity of the moon during orbit. Content Type Journal Article Pages 1-26 DOI 10.1007/s11038-012-9399-6 Authors T. G. Leighton, Faculty of Engineering and the Environment, Institute of Sound and Vibration Research, University of Southampton, Highfield, Southampton, SO17 1BJ UK P. R. White, Faculty of Engineering and the Environment, Institute of Sound and Vibration Research, University of Southampton, Highfield, Southampton, SO17 1BJ UK D. C. Finfer, Faculty of Engineering and the Environment, Institute of Sound and Vibration Research, University of Southampton, Highfield, Southampton, SO17 1BJ UK Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295

Description:    This paper analyzes Robe’s circular restricted three-body problem when the hydrostatic equilibrium figure of the first primary is assumed to be an oblate spheroid, the shape of the second primary is considered as a triaxial rigid body, and the full buoyancy force of the fluid is taken into account. It is found that there is an equilibrium point near the center of the first primary, another equilibrium point exists on the line joining the centers of the primaries and there exist infinite number of equilibrium points on an ellipse in the orbital plane of the second primary. It is also observed that under certain conditions, all these equilibrium points can be stable. The most interesting and distinguishable results of this study are the existence of elliptical points and their stability. Content Type Journal Article Pages 1-11 DOI 10.1007/s11038-012-9397-8 Authors Jagadish Singh, Department of Mathematics, Faculty of Science, Ahmadu Bello University, Zaria, Nigeria Hafsah Laraba Mohammed, Department of Mathematics, Faculty of Science, Ahmadu Bello University, Zaria, Nigeria Journal Earth, Moon, and Planets Online ISSN 1573-0794 Print ISSN 0167-9295