001110   Kantharia N G;Das M;Krishna G (National Centre for Radio Astrophysics Tata Institute of Fundamental R, Ganeshkhind, Pune Univ, Pune Campus, Pune-411 007, Email: ngk@ncra.tifr.res.in) : GMRT detection of a new wide-angle tail (WAT) radio source associated with the galaxy PGC1519010. J Astrophys Astr 2009, 30(1), 37-51.

Reports the serendipitous detection of a Wide-Angle Tail (WAT) radio galaxy at 240 and 610 MHz, using the Giant Metrewave Radio Telescope (GMRT). This WAT is hosted by a cD galaxy PGC 1519010 whose photometric redshift given in the SDSS DR6 catalogue is close to the spectroscopic redshifts (0.105,0.106 and 0.107) of three galaxies found within 4' of the cD. Using the SDSS DR6, we have identified a total of 37 galaxies within 15' of the cD, whose photometric redshifts are between 0.08 and 0.14. This strongly suggests that the cD is associated with a group of galaxies whose conspicuous feature is a north-south chain of galaxies (filament) extending to at least 2.6 Mpc. The ROSAT all-sky survey shows a faint, diffuse X-ray source in this direction, which probably marks the hot intracluster gas in the potential well of this group. Combines the radio structural information for this WAT with the galaxy clustering in that region to check its overall consistency with the models of WAT formation. The bending of the jet before and after its disruption forming the radio plume, are found to be correlated in this WAT, as seen from the contrasting morphological patterns on the two sides of the core. Probable constraints imposed by this on the models of WAT formation are pointed out. We also briefly report on the other interesting radio sources found in the proximity of the WAT. These include a highly asymmetric double radio source and an ultra-steep spectrum radio source for which no optical counterpart is detected in the SDSS.

27 illus, 2 tables, 43 ref

001109   Isobe H;Shibata K (NO, Unit of Synergetic Studies for Space, Kyoto Univ, Japan, Email: isobe@kwasan.kyoto-u.ac.jp) : Reconnection in solar flares: outstanding questions. J Astrophys Astr 2009, 30(2), 79-85.

Space observations of solar flares such as those from Yohkoh, SOHO, TRACE, and RHESSI have revealed a lot of observational evidence of magnetic reconnection in solar flares: cusp-shaped arcades, reconnection inflows, plasmoids, etc. Thus it has been established, at least phenomeno-logically, that magnetic reconnection does occur in solar flares. However, a number of fundamental questions and puzzles still remain in the physics of reconnection in solar flares. Discusses the recent progresses and future prospects in the study of magnetic reconnection in solar flares from both theoretical and observational points of view.

1 illus, 61 ref

001108   Griffin R F (NO, The Observatories, Madingley Road, Gombridge CB3 OHA, England, Email: rfg@ast.com.ac.uk) : Spectroscopic binaries near the north galactic pole paper 12A: 6 bootis. J Astrophys Astr 2009, 30(2), 87-91.

About 25 years ago, in Paper 12 of this series, the author presented a spectroscopic orbit for 6 Bootis. The velocity amplitude of little more than 1 km s^{-1 was much smaller than for any star whose orbit had been determined up till that time. Although it was objectively demonstrated that the orbit was very secure, a few years ago subjective misgivings prompted the author to restore the star to his observing programme. New observations of much higher precision confirm not only the spectroscopic-binary nature of 6 Boo but also, with almost astonishing fidelity, the elements already given for it.}

1 illus, 2 tables, 15 ref

001107   Das M K;Narang P;Mahajan S;Yuasa M (Institute of Informatics and Communication, Delhi South Campus Univ, Benitojuarez Road, New Delhi-110 021) : On out of plane equilibrium points in photo-gravitational restricted three-body problem. J Astrophys Astr 2009, 30(3-4), 177-85.

Authors have investigated the out of plane equilibrium points of a passive micron size particle and their stability in the field of radiating binary stellar systems Kriiger-60, R W-Monocerotis within the framework of photo-gravitational circular restricted three-body problem. It was found that the out of plane equilibrium points (L_i, i = 6, 7, 8, 9) may exist for range of β₁ (ratio of radiation to gravitational force of the massive component) values for these binary systems in the presence of Poynting-Robertson drag (hereafter PR-drag). In the absence of PR-drag, we find that the motion of a particle near the equilibrium points L_6,7 is stable in both the binary systems for a specific range of β₁ values. The PR-drag is shown to cause instability of the various out of plane equilibrium points in these binary systems.

4 illus, 1 table, 23 ref

001106   Bradford R A W (NO, , Bennerley, 1 Merlin Haven, Wotton-under-edge, Gloucestershire, England, GL12 7BA., Email: rickatmerlinhaven@hotmail.com) : Effect of hypothetical diproton stability on the universe. J Astrophys Astr 2009, 30(2), 119-31.

By calculation of the proton-proton capture cross-section, it is shown that the existence of a bound diproton state would not lead to significant production of diprotons during big bang nucleosynthesis, contrary to popular belief. In typical stellar interiors, the stability of diprotons would lead to a reaction pathway for converting protons to deuterons perhaps ~ 10^{10 times faster than the usual weak capture reaction. This would prevent stars of the familiar hot, dense type from occurring in the universe. However, if diproton stability is achieved by an increase in the low-energy strong coupling, gs, then stars with temperatures and densities sufficiently reduced so as to offset the faster reaction pathway to deuterium will appear to meet elementary stability criteria. The claim that there is a fine-tuned, anthropic upper bound to the strong force which ensures diproton instability therefore appears to be unfounded.}

2 illus, 3 tables, 26 ref

001105   Bhatt N J;Jain R;Aggarwal M (NO, C.U. Shah Science College, Ashram Raod, Ahmedabad-380 014, Email: nijibhatt@hotmail.com) : Predicting maximum sunspot number in solar cycle 24. J Astrophys Astr 2009, 30(1), 71-7.

A few prediction methods have been developed based on the precursor technique which is found to be successful for forecasting the solar activity. Considering the geomagnetic activity aa indices during the descending phase of the preceding solar cycle as the precursor, we predict the maximum amplitude of annual mean sunspot number in cycle 24 to be 111 ± 21. This suggests that the maximum amplitude of the upcoming cycle 24 will be less than cycles 21-22. Further, we have estimated the annual mean geomagnetic activity aa index for the solar maximum year in cycle 24 to be 20.6 ± 4.7 and the average of the annual mean sunspot number during the descending phase of cycle 24 is estimated to be 48 ± 16.8.

4 illus, 1 table, 14 ref

001104   Basu D (Physics Dep, Carleton Univ, Ottawa, ON KIS 5B6, Canada, Email: basu@physics.carleton.ca) : Close separation triple system QSO 1009-0252 with discordant redshifts: is the spectrum of one component blueshifted?. J Astrophys Astr 2009, 30(3-4), 133-43.

1009-0252 is a Quasi Stellar Object (QSO) with three components A, B, C. A, B are thought to be the result of gravitational lensing of one object, and A, C constitute a close pair with redshifts 2.74 and 1.62 respectively. Close separation pairs of QSOs with discordant redshifts have received special attention in recent years, probably because of the possibility that they may be physically associated, implying non-cosmological redshifts. Attempts have been made to explain their occurrences due to the effect of gravitational lensing. However, gravitational lensing has not offered a completely satisfactory explanation for this triplet. Furthermore, examination revealed some inadequacies and inconsistencies in the red-shift identification of the observed lines in the component A. Observational results of 1009-0252 therefore remain puzzling. We propose an alternative explanation by suggesting that A, B actually constitute a close pair and C is an unrelated object in the field. We show that the observed spectrum of A can be interpreted as blueshifted. This implies that A, B are two separate objects, one (A) approaching us and the other (B) receding from us, and are not the result of gravitational lensing of a single object. The oppositely directed pair A, B may have been ejected due to the merger of two galaxies.

1 illus, 2 tables, 60 ref

001103   Baruah R;Duorah K;Duorah H L (Physics Dep, HRH The Prince of Wales Institute of Engineering and Technology, Jorhat-785 001, Email: ruleebaruah@yahoo.co.in) : Rapid neutron capture process in supernovae and chemical element formation. J Astrophys Astr 2009, 30(3-4), 165-75.

The rapid neutron capture process (r-process) is one of the major nucleosynthesis processes responsible for the synthesis of heavy nuclei beyond iron. Isotopes beyond Fe are most exclusively formed in neutron capture processes and more heavier ones are produced by the r-process. Approximately half of the heavy elements with mass number A > 70 and all of the actinides in the solar system are believed to have been produced in the r-process. We have studied the r-process in supernovae for the production of heavy elements beyond A = 40 with the newest mass values available. The supernova envelopes at a temperature > 10^{9 K and neutron density of 1024 cm-3 are considered to be one of the most potential sites for the r-process. The primary goal of the r-process calculations is to fit the global abundance curve for solar system r-process isotopes by varying time dependent parameters such as temperature and neutron density. This method aims at comparing the calculated abundances of the stable isotopes with observation. We have studied the r-process path corresponding to temperatures ranging from 1.0 x 109 K to 3.0 x 109 K and neutron density ranging from 1020cm-3 to 1030cm-3. With temperature and density conditions of 3.0 x 109 K and 1020 cm-3 a nucleus of mass 273 was theoretically found corresponding to atomic number 115. The elements obtained along the r-process path are compared with the observed data at all the above temperature and density range.}

2 illus, 2 tables, 23 ref

001102   Barai P;Brito W;Martel H (De Physique Dep, de Genie Physique et d'Optique, Laval Univ, Quebec City, Quebec, GIK 7P4, Canada, Email: paramita.barai.I@ulaval.ca) : Fate of dwarf galaxies in clusters and the origin of intracluster stars. J Astrophys Astr 2009, 30(1), 1-36.

The main goal of this paper is to compare the relative importance of destruction by tides vs. destruction by mergers, in order to assess if tidal destruction of galaxies in clusters is a viable scenario for explaining the origin of intracluster stars. We have designed a simple algorithm for simulating the evolution of isolated clusters. The distribution of galaxies in the cluster is evolved using a direct gravitational N- body algorithm combined with a subgrid treatment of physical processes such as mergers, tidal disruption, and galaxy harassment. Using this algorithm, we have performed a total of 148 simulations. Our main results are: 1. destruction of dwarf galaxies by mergers dominates over destruction by tides, and 2. The destruction of galaxies by tides is sufficient to explain the observed intracluster light in clusters.

6 illus, 12 tables, 66 ref

014688   Sreekumar P;et al. (NO, ISRO Satellite Centre, Bangalore-560 017, Email: pskumar@isac.gov.in) : High energy X-ray spectrometer on Chandrayaan-1. Curr Sci 2009, 96(4), 520-5.

Chandrayaan-1, India's first planetary exploration mission to Moon carries a suite of payloads including a High Energy X-ray spectrometer (HEX) designed to study low-energy (30-270 keV) natural gamma rays emitted from the lunar surface due to decay of uranium and thorium. The primary science objective of HEX is to study transport of volatiles on the lunar surface through the detection of the 46.5 keV line from ^{210Pb decay, which is a decay product of volatile 222Rn, both belonging to the 238U decay series. HEX is designed to have a spatial resolution of ~33 km at energies below 120 keV. The low signal strength of these emissions requires a large area detector with high sensitivity and energy resolution, and a new generation Cd-Zn-Te (CZT) solid state array detector is used in this experiment. Long time integration will be required to detect the emission because of the significant lunar continuum background and weak signal strength. The various sub-systems of the HEX flight payload and test results from ground calibration are described in this article. HEX will be the first experiment aimed at detecting low energy (< 300 keV) gamma ray emission from a planetary surface.}

7 illus, 2 tables, 7 ref

014687   Spudis P;et al. (NO, Lunar and Planetary Institute, 3600 Bay Area Blvd. Houston, TX 77058, USA, Email: spudis@lpi.usra.edu) : Mini-SAR: an imaging radar experiment for the Chandrayaan-1 mission to the moon. Curr Sci 2009, 96(4), 533-9.

Mini-SAR is a single frequency (S-band; 13-cm wavelength) Synthetic Aperture Radar (SAR) in a lightweight (~9 kg) package. Previous Earth- and space-based radar observations of the permanently shadowed regions of the lunar poles have measured areas of high circular polarization ratio consistent with volume scattering from water ice buried at shallow (0.1-1 m) depths. This detection is not definitive because of poor viewing geometry and a limited number of observations. Mini-SAR utilizes a unique hybrid polarization architecture, which allows determination of the Stokes parameters of the reflected signal, intended to distinguish volume scattering (caused by the presence of ice) from other scattering mechanisms (e.g. sub-wavelength scale surface roughness).

8 illus, 2 tables, 14 ref

014686   Pieters C M;et al. (Geological Sciences Dep, Brown Univ, Providence, RI 02912, USA, Email: Carle_Pieters@brown.edu) : Moon mineralogy mapper (M<. Curr Sci 2009, 96(4), 500-5.

The Moon Mineralogy Mapper (M^{3) is a NASA-supported guest instrument on ISRO's remote sensing mission to Moon, Chandrayaan-1. The M3 is an imaging spectrometer that operates from the visible into the near-infrared (0.42-3.0 μm) where highly diagnostic mineral absorption bands occur. Over the course of the mission M3 will provide low resolution spectro-scopic data for the entire lunar surface at 140 m/pixel (86 spectral channels) to be used as a base-map and high spectral resolution science data (80 m/pixel; 260 spectral channels) for 25-50% of the surface. The detailed mineral assessment of different lunar terrains provided by M3 is principal information needed for understanding the geologic evolution of the lunar crust and lays the foundation for focused future in-depth exploration of the Moon.}

5 illus, 1 table, 9 ref

014685   Marvin Herndon J (NO, , Transdyne Corporation, 11044 Red Rock Drive, San Diego, CA 92131, USA, Email: mherndon@san.rr.com) : Internal heat production in hot jupiter exo-planets, thermonuclear ignition of dark galaxies, and the basis for galactic luminous star distributions. Curr Sci 2009, 96(11), 1453-6.

3 illus, 34 ref

014684   Mall U;Banaszkiewicz M;Bronstad K;McKenna Lawlor S;Nathues A;Soraas F;Vilenius E;Ullaland K (NO, Max-Planck-Institute for Solar System Research, 37191 Katlenburg Katlenburg-Lindau, Germany, Email: mall@mps.mpg.de) : Near infrared spectrometer SIR-2 on Chandrayaan-1. Curr Sci 2009, 96(4), 506-11.

Chandrayaan-1, the first Indian mission to the Moon, will provide an opportunity for in situ lunar observations over a two-year period from a 100 km polar orbit. A comprehensive suite of onboard instruments will include the SIR-2 near-infrared grating spectrometer. SIR-2, a pointing spectrometer, will observe the Moon in the spectral range 900-2400 nm, with a unique spectral resolution of 6 nm over a wide range of phase angles. The high resolution SIR-2 observations, particularly of the lunar far side and polar region, are expected to have a large impact on our understanding of the mineralogy and composition of the Moon.

3 illus, 2 tables, 18 ref

014683   Kiran Kumar A S (NO, Space Applications Centre, Jodhpur Tekra, Ahmedabad-380 015, Email: kiran@sac.isro.gov.in) : Hyper spectral imager for lunar mineral mapping in visible and near infrared band. Curr Sci 2009, 96(4), 496-9.

The Hyper Spectral Imager (HySI), operating in the visible and near infrared spectral region, is one of the three imaging instruments on board Chandrayaan-1 spacecraft for mineralological study of the Moon. HySI will map the entire lunar surface in 64 contiguous bands in the visible and near infrared (VNIR: 421-964 nm) with a spatial sampling of 80 m. A wedge filter is employed for the spectral separation and the image is mapped on an area detector. The detector output is processed in the front-end electronics to generate the 64-bands with 12-bit quantization. HySI is a highly compact instrument weighing 2.5 kg with a power requirement of 2.6 W.

9 illus, 1 table, 2 ref

014682   Kamalakar J A;Laxmi Prasad A S;Bhaskar K V S; Selvaraj P;Venkateswaran R;Kalyani K;Goswami A;Sridhar Raja V L N (Laboratory for Electro-Optics Systems, Indian Space Researc Organization, Bangalore-560 058, Email: kamalakar@leos.gov.in) : Lunar laser ranging instrument (LLRI): a tool for the study of topography and gravitational field of the moon. Curr Sci 2009, 96(4), 512-16.

The Lunar Laser Ranging Instrument (LLRI) developed for flight on the Chandrayaan-1 spacecraft was designed to measure the topography of the lunar surface over a 2-year period from a 100 km polar orbit of Moon. A 10 mJ diode-pumped pulsed laser together with 200 mm diameter telescope and a silicon avalanche photodiode are the principal optical assemblies of this active remote-sensing instrument. We present here science objectives of LLRI and its performance specifications along with details of instrument design. The methods by means of which LLRI performance and operability were analysed are also presented. During end-to-end testing, the integrated LLRI was operated in free space aiming at a distant target (~30 km). Test results were found to be satisfactory and well within the desired specifications.

7 illus, 2 tables, 14 ref

014681   Grande M (Institute of Mathematical and Physical Sciences, Wales Univ, Aberystwyth, SY23 3BZ, UK, Email: m.grande@aber.ac.uk) : Chandrayaan-1 X-ray spectrometer. Curr Sci 2009, 96(4), 517-19.

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Chandrayaan-1 lunar mission. It exploits heritage from the D-C1XS instrument on ESA's SMART-1 mission. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ti, Ca and Fe) over the lunar surface. The baseline design consists of 24 nadir pointing Swept Charge Device detectors, which provide high detection efficiency in the 1-7 keV range, which contains the X-ray fluorescence lines of the above elements of interest. Micro-machined collimators provide a 14 degree FWHM FOV, equivalent to 25 km from 100 km altitude. A deploy-able door protects the instrument during launch and cruise, and also provides a ^{55Fe calibration X-ray source for detector calibration. Additional refinements compared to D-C1XS will result in a significantly improved energy resolution. To record the incident solar X-ray flux at the Moon, C1XS carries an X-ray Solar Monitor (XSM). C1XS will arrive at the Moon in the run up to the maximum of the solar cycle 24, and the expected high incident X-ray flux coupled to a 100 km circular polar orbit, will provide composition data accurate to better than 10% of major elemental abundances over the lunar surface.}

3 illus, 5 ref

014680   Goswami N;Annadurai M (NO, Physical Research Laboratory, Ahmedabad-380 009, Email: goswami@prl.res.in) : Chandrayaan-1: India's first planetary science mission to the moon. Curr Sci 2009, 96(4), 486-91.

Chandrayaan-1, the first Indian planetary exploration mission, will carry out high resolution remote sensing studies of the moon to further our understanding about its origin and evolution. Hyper-spectral imaging in the UV-VIS-NIR region using three imaging spectrometers, along with a low energy X-ray spectrometer will provide mineralogical and chemical composition of the lunar surface at high spatial resolution. A terrain mapping camera will provide high resolution three-dimensional images of the lunar surface and will be complemented by a laser ranging instrument that will provide lunar altimetry. Three payloads - a high energy X-γ ray spectrometer, a sub-keV atom reflecting analyser, and miniature imaging radar - will be used for the first time for remote sensing exploration of a planetary body. They will investigate transport of volatiles on the lunar surface, presence of localized lunar mini-magnetosphere and possible presence of water ice in the permanently shadowed lunar polar region respectively. A radiation dose monitor will provide information on energetic particle flux en route to the moon and in lunar orbit. An impact probe carrying an imaging system, a radar altimeter and a mass spectrometer will be released from the spacecraft to land at a predestinated lunar site. The design of the one tonne-class spacecraft is primarily adapted from flight proven Indian Remote Sensing satellite bus with several modifications that are specific to the lunar mission. The spacecraft was launched by using a variant of the indigenous Polar Satellite Launch Vehicle (PSLV-XL) and placed in a 100 km circular polar orbit around the moon with a planned mission life of two years. An Indian Deep Space Network and an Indian Space Science Data Center have been established as a part of Chandrayaan-1 mission and will cater to the need of future Indian space science and planetary missions.

5 illus

014679   Dachev T;Tomov B;Dimitrov P;Matviichuk Y (Solar-Terrestrial influences Laboratory, Bulgarian Academy of Sciences, Sofia, Bulgaria, Email: tdachev59@gmail.com) : Monitoring lunar radiation environment: RADOM instrument on Chandrayaan-1. Curr Sci 2009, 96(4), 544-6.

Describes the RADOM instrument on Chandrayaan-1 spacecraft to monitor the radiation environment en-route to Moon and in lunar orbit. The instrument is a miniature (98 g; 100 mW) 256 channels spectrometer for the measurement of energy deposited (dose) due to incident primary and secondary energetic particles using a single 0.3 mm thick 2 cm2 silicon detector. The science objectives, instrument details and operation sequence as well as the data analysis procedure and instrument calibration results are presented.

3 illus, 11 ref

014678   Bjorn L O;Papageorgiou G C;Dravins D; Govindjee (Cell and Organism Biology Dep, , Solvegatan 35, SE-22467 Lund, Sweden, Email: Lars_Olof.Bjorn@cob.lu.se) : Detectability of life and photosynthesis on exoplanets. Curr Sci 2009, 96(9), 1171-5.

2 illus, 45 ref

014677   Barbash S;et al. (NO, Swedish Institute of Space Physics, Box 812, 98128 Kiruna, Sweden, Email: stas@irf.se) : Investigation of the solar wind-moon interaction onboard Chandrayaan-1 mission with the SARA experiment. Curr Sci 2009, 96(4), 526-32.

The SARA instrument (Sub-keV Atom Reflecting Analyser) comprises a low energy neutral atom (LENA) sensor for the energy range 10 eV-3.3 keV and an ion mass spectrometer (10 eV-15 keV). It is the first ever experiment to study the solar wind-planetary surface interaction via measurements of the sputtered atoms and neutralized back-scattered solar wind hydrogen. The neutral atom sensor uses conversion of the incoming neutrals to positive ions, which are then analysed via surface interaction technique. The ion mass spectrometer is based on the same principle. SARA performs LENA imaging of the Moon's elemental surface composition including that of permanently shadowed areas, and imaging of the lunar surface magnetic anomalies. It will also investigate processes of space weathering and sputtered sources of the exospheric gases.

5 illus, 1 table, 22 ref

014676   Ashok Kumar Y (NO, Vikram Sarabhai Space Centre, Thriuvananthapuram-695 022, Email: ashok_kumar@vssc.gov.in) : Moon impact probe on Chandrayaan-1. Curr Sci 2009, 96(4), 540-3.

Unique, stand alone micro satellite called the Moon Impact Probe (MIP), designed to impact at a pre-decided location near the South Pole of the moon was a part of the Chandrayaan-1 mission. The MIP has two technology and one scientific experiments, viz. a Moon Imaging System (MIS) for surface photography along its path, a Radar Altimeter for terrain topography at close distance (<5 km) and a Mass Spectrometer, CHACE (Chandra's Altitudinal Composition Explorer), for measuring the neutral composition on the sunlit side of the moon. A description of the various sub-systems of the MIP and of the instruments is presented in this article.

7 illus, 2 tables, 1 ref

014688   Sreekumar P;et al. (NO, ISRO Satellite Centre, Bangalore-560 017, Email: pskumar@isac.gov.in) : High energy X-ray spectrometer on Chandrayaan-1. Curr Sci 2009, 96(4), 520-5.

Chandrayaan-1, India's first planetary exploration mission to Moon carries a suite of payloads including a High Energy X-ray spectrometer (HEX) designed to study low-energy (30-270 keV) natural gamma rays emitted from the lunar surface due to decay of uranium and thorium. The primary science objective of HEX is to study transport of volatiles on the lunar surface through the detection of the 46.5 keV line from ^{210Pb decay, which is a decay product of volatile 222Rn, both belonging to the 238U decay series. HEX is designed to have a spatial resolution of ~33 km at energies below 120 keV. The low signal strength of these emissions requires a large area detector with high sensitivity and energy resolution, and a new generation Cd-Zn-Te (CZT) solid state array detector is used in this experiment. Long time integration will be required to detect the emission because of the significant lunar continuum background and weak signal strength. The various sub-systems of the HEX flight payload and test results from ground calibration are described in this article. HEX will be the first experiment aimed at detecting low energy (< 300 keV) gamma ray emission from a planetary surface.}

7 illus, 2 tables, 7 ref

014687   Spudis P;et al. (NO, Lunar and Planetary Institute, 3600 Bay Area Blvd. Houston, TX 77058, USA, Email: spudis@lpi.usra.edu) : Mini-SAR: an imaging radar experiment for the Chandrayaan-1 mission to the moon. Curr Sci 2009, 96(4), 533-9.

Mini-SAR is a single frequency (S-band; 13-cm wavelength) Synthetic Aperture Radar (SAR) in a lightweight (~9 kg) package. Previous Earth- and space-based radar observations of the permanently shadowed regions of the lunar poles have measured areas of high circular polarization ratio consistent with volume scattering from water ice buried at shallow (0.1-1 m) depths. This detection is not definitive because of poor viewing geometry and a limited number of observations. Mini-SAR utilizes a unique hybrid polarization architecture, which allows determination of the Stokes parameters of the reflected signal, intended to distinguish volume scattering (caused by the presence of ice) from other scattering mechanisms (e.g. sub-wavelength scale surface roughness).

8 illus, 2 tables, 14 ref

014686   Pieters C M;et al. (Geological Sciences Dep, Brown Univ, Providence, RI 02912, USA, Email: Carle_Pieters@brown.edu) : Moon mineralogy mapper (M<. Curr Sci 2009, 96(4), 500-5.

The Moon Mineralogy Mapper (M^{3) is a NASA-supported guest instrument on ISRO's remote sensing mission to Moon, Chandrayaan-1. The M3 is an imaging spectrometer that operates from the visible into the near-infrared (0.42-3.0 μm) where highly diagnostic mineral absorption bands occur. Over the course of the mission M3 will provide low resolution spectro-scopic data for the entire lunar surface at 140 m/pixel (86 spectral channels) to be used as a base-map and high spectral resolution science data (80 m/pixel; 260 spectral channels) for 25-50% of the surface. The detailed mineral assessment of different lunar terrains provided by M3 is principal information needed for understanding the geologic evolution of the lunar crust and lays the foundation for focused future in-depth exploration of the Moon.}

5 illus, 1 table, 9 ref

014685   Marvin Herndon J (NO, , Transdyne Corporation, 11044 Red Rock Drive, San Diego, CA 92131, USA, Email: mherndon@san.rr.com) : Internal heat production in hot jupiter exo-planets, thermonuclear ignition of dark galaxies, and the basis for galactic luminous star distributions. Curr Sci 2009, 96(11), 1453-6.

3 illus, 34 ref

014684   Mall U;Banaszkiewicz M;Bronstad K;McKenna Lawlor S;Nathues A;Soraas F;Vilenius E;Ullaland K (NO, Max-Planck-Institute for Solar System Research, 37191 Katlenburg Katlenburg-Lindau, Germany, Email: mall@mps.mpg.de) : Near infrared spectrometer SIR-2 on Chandrayaan-1. Curr Sci 2009, 96(4), 506-11.

Chandrayaan-1, the first Indian mission to the Moon, will provide an opportunity for in situ lunar observations over a two-year period from a 100 km polar orbit. A comprehensive suite of onboard instruments will include the SIR-2 near-infrared grating spectrometer. SIR-2, a pointing spectrometer, will observe the Moon in the spectral range 900-2400 nm, with a unique spectral resolution of 6 nm over a wide range of phase angles. The high resolution SIR-2 observations, particularly of the lunar far side and polar region, are expected to have a large impact on our understanding of the mineralogy and composition of the Moon.

3 illus, 2 tables, 18 ref

014683   Kiran Kumar A S (NO, Space Applications Centre, Jodhpur Tekra, Ahmedabad-380 015, Email: kiran@sac.isro.gov.in) : Hyper spectral imager for lunar mineral mapping in visible and near infrared band. Curr Sci 2009, 96(4), 496-9.

The Hyper Spectral Imager (HySI), operating in the visible and near infrared spectral region, is one of the three imaging instruments on board Chandrayaan-1 spacecraft for mineralological study of the Moon. HySI will map the entire lunar surface in 64 contiguous bands in the visible and near infrared (VNIR: 421-964 nm) with a spatial sampling of 80 m. A wedge filter is employed for the spectral separation and the image is mapped on an area detector. The detector output is processed in the front-end electronics to generate the 64-bands with 12-bit quantization. HySI is a highly compact instrument weighing 2.5 kg with a power requirement of 2.6 W.

9 illus, 1 table, 2 ref

014682   Kamalakar J A;Laxmi Prasad A S;Bhaskar K V S; Selvaraj P;Venkateswaran R;Kalyani K;Goswami A;Sridhar Raja V L N (Laboratory for Electro-Optics Systems, Indian Space Researc Organization, Bangalore-560 058, Email: kamalakar@leos.gov.in) : Lunar laser ranging instrument (LLRI): a tool for the study of topography and gravitational field of the moon. Curr Sci 2009, 96(4), 512-16.

The Lunar Laser Ranging Instrument (LLRI) developed for flight on the Chandrayaan-1 spacecraft was designed to measure the topography of the lunar surface over a 2-year period from a 100 km polar orbit of Moon. A 10 mJ diode-pumped pulsed laser together with 200 mm diameter telescope and a silicon avalanche photodiode are the principal optical assemblies of this active remote-sensing instrument. We present here science objectives of LLRI and its performance specifications along with details of instrument design. The methods by means of which LLRI performance and operability were analysed are also presented. During end-to-end testing, the integrated LLRI was operated in free space aiming at a distant target (~30 km). Test results were found to be satisfactory and well within the desired specifications.

7 illus, 2 tables, 14 ref

014681   Grande M (Institute of Mathematical and Physical Sciences, Wales Univ, Aberystwyth, SY23 3BZ, UK, Email: m.grande@aber.ac.uk) : Chandrayaan-1 X-ray spectrometer. Curr Sci 2009, 96(4), 517-19.

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Chandrayaan-1 lunar mission. It exploits heritage from the D-C1XS instrument on ESA's SMART-1 mission. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ti, Ca and Fe) over the lunar surface. The baseline design consists of 24 nadir pointing Swept Charge Device detectors, which provide high detection efficiency in the 1-7 keV range, which contains the X-ray fluorescence lines of the above elements of interest. Micro-machined collimators provide a 14 degree FWHM FOV, equivalent to 25 km from 100 km altitude. A deploy-able door protects the instrument during launch and cruise, and also provides a ^{55Fe calibration X-ray source for detector calibration. Additional refinements compared to D-C1XS will result in a significantly improved energy resolution. To record the incident solar X-ray flux at the Moon, C1XS carries an X-ray Solar Monitor (XSM). C1XS will arrive at the Moon in the run up to the maximum of the solar cycle 24, and the expected high incident X-ray flux coupled to a 100 km circular polar orbit, will provide composition data accurate to better than 10% of major elemental abundances over the lunar surface.}

3 illus, 5 ref

014680   Goswami N;Annadurai M (NO, Physical Research Laboratory, Ahmedabad-380 009, Email: goswami@prl.res.in) : Chandrayaan-1: India's first planetary science mission to the moon. Curr Sci 2009, 96(4), 486-91.

Chandrayaan-1, the first Indian planetary exploration mission, will carry out high resolution remote sensing studies of the moon to further our understanding about its origin and evolution. Hyper-spectral imaging in the UV-VIS-NIR region using three imaging spectrometers, along with a low energy X-ray spectrometer will provide mineralogical and chemical composition of the lunar surface at high spatial resolution. A terrain mapping camera will provide high resolution three-dimensional images of the lunar surface and will be complemented by a laser ranging instrument that will provide lunar altimetry. Three payloads - a high energy X-γ ray spectrometer, a sub-keV atom reflecting analyser, and miniature imaging radar - will be used for the first time for remote sensing exploration of a planetary body. They will investigate transport of volatiles on the lunar surface, presence of localized lunar mini-magnetosphere and possible presence of water ice in the permanently shadowed lunar polar region respectively. A radiation dose monitor will provide information on energetic particle flux en route to the moon and in lunar orbit. An impact probe carrying an imaging system, a radar altimeter and a mass spectrometer will be released from the spacecraft to land at a predestinated lunar site. The design of the one tonne-class spacecraft is primarily adapted from flight proven Indian Remote Sensing satellite bus with several modifications that are specific to the lunar mission. The spacecraft was launched by using a variant of the indigenous Polar Satellite Launch Vehicle (PSLV-XL) and placed in a 100 km circular polar orbit around the moon with a planned mission life of two years. An Indian Deep Space Network and an Indian Space Science Data Center have been established as a part of Chandrayaan-1 mission and will cater to the need of future Indian space science and planetary missions.

5 illus

014679   Dachev T;Tomov B;Dimitrov P;Matviichuk Y (Solar-Terrestrial influences Laboratory, Bulgarian Academy of Sciences, Sofia, Bulgaria, Email: tdachev59@gmail.com) : Monitoring lunar radiation environment: RADOM instrument on Chandrayaan-1. Curr Sci 2009, 96(4), 544-6.

Describes the RADOM instrument on Chandrayaan-1 spacecraft to monitor the radiation environment en-route to Moon and in lunar orbit. The instrument is a miniature (98 g; 100 mW) 256 channels spectrometer for the measurement of energy deposited (dose) due to incident primary and secondary energetic particles using a single 0.3 mm thick 2 cm2 silicon detector. The science objectives, instrument details and operation sequence as well as the data analysis procedure and instrument calibration results are presented.

3 illus, 11 ref

014678   Bjorn L O;Papageorgiou G C;Dravins D; Govindjee (Cell and Organism Biology Dep, , Solvegatan 35, SE-22467 Lund, Sweden, Email: Lars_Olof.Bjorn@cob.lu.se) : Detectability of life and photosynthesis on exoplanets. Curr Sci 2009, 96(9), 1171-5.

2 illus, 45 ref

014677   Barbash S;et al. (NO, Swedish Institute of Space Physics, Box 812, 98128 Kiruna, Sweden, Email: stas@irf.se) : Investigation of the solar wind-moon interaction onboard Chandrayaan-1 mission with the SARA experiment. Curr Sci 2009, 96(4), 526-32.

The SARA instrument (Sub-keV Atom Reflecting Analyser) comprises a low energy neutral atom (LENA) sensor for the energy range 10 eV-3.3 keV and an ion mass spectrometer (10 eV-15 keV). It is the first ever experiment to study the solar wind-planetary surface interaction via measurements of the sputtered atoms and neutralized back-scattered solar wind hydrogen. The neutral atom sensor uses conversion of the incoming neutrals to positive ions, which are then analysed via surface interaction technique. The ion mass spectrometer is based on the same principle. SARA performs LENA imaging of the Moon's elemental surface composition including that of permanently shadowed areas, and imaging of the lunar surface magnetic anomalies. It will also investigate processes of space weathering and sputtered sources of the exospheric gases.

5 illus, 1 table, 22 ref

014676   Ashok Kumar Y (NO, Vikram Sarabhai Space Centre, Thriuvananthapuram-695 022, Email: ashok_kumar@vssc.gov.in) : Moon impact probe on Chandrayaan-1. Curr Sci 2009, 96(4), 540-3.

Unique, stand alone micro satellite called the Moon Impact Probe (MIP), designed to impact at a pre-decided location near the South Pole of the moon was a part of the Chandrayaan-1 mission. The MIP has two technology and one scientific experiments, viz. a Moon Imaging System (MIS) for surface photography along its path, a Radar Altimeter for terrain topography at close distance (<5 km) and a Mass Spectrometer, CHACE (Chandra's Altitudinal Composition Explorer), for measuring the neutral composition on the sunlit side of the moon. A description of the various sub-systems of the MIP and of the instruments is presented in this article.

7 illus, 2 tables, 1 ref

015713   Pickup R M;Cywinski R;Pappas C;Fouquet P; Farago E;Falus P (NO, School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK, Email: pappas@hmi.de) : Generalized approach to non-exponential relaxation. Pramana J Phys 2008, 71(5), 901.

Non-exponential relaxation is a universal feature of systems as diverse as glasses, spin glasses, earthquakes, financial markets and the universe. Complex relaxation results from hierarchically constrained dynamics with the strength of the constraints being directly related to the form of the relaxation, which changes from a simple exponential a stretched exponential and a power law by increasing the constraints in the system. global and unified approach to non-exponentiality was first achieved by Weron and was further generalized by Brouers and Sotolongo-Costa, who applied the concept of nonªextensive entropy introduced by Tsallis to the relaxation of disordered systems. These concepts are now confronted with experimental results on the classical metallic spin glasses CuMn, AuFe and the insulating system EuSrS. The revisited data have also be complemented by new results on several compositions of the classical CuMn spin glass and on systems, like CoGa and CuCo, the magnetic behaviour of which is believed to arise from magnetic clusters and should be characteristic for superparamagnetism.

015712   Paul B C;Paul D (Physics Dep, North Bangal University, Siliguri, Dist. Darjeeling-734 013, Email: bepaul@iucaa.ernet.in) : Anisotropic bianchi-I universe with phantom field and cosmological constant. Pramana J Phys 2008, 71(6), 1247-57.

Studies an anisotropic Bianchi-I universe in the presence of a phantom field and a cosmological constant. Cosmological solutions are obtained when the kinetic energy of the phantom field is of the order of anisotropy and dominates over the potential energy of the field. The anisotropy of the universe decreases and the universe transits to an isotropic fiat FRW universe accommodating the present acceleration. A class of new cosmological solutions is obtained for an anisotropic universe in case an initial anisotropy exists which is bigger than the value determined by the parameter of the kinetic part of the field. Later, an autonomous system of equations for an axially symmetric Bianchi-I universe with phantom field in an exponential potential is studied. We discuss the stability of the cosmological solutions.

1 illus, 29 ref

015711   Patnaik S;Kamila S K;Roy G S (NO, , Plot No. -6 Budheswari Colony, Bhubaneswar-751 006) : Visual binary stars - calculation of orbital parameters of WDS 04374-0951 & WDS 18384+0850. Ultra Scient phys Sci 2009, 21(2), 365-74.

A Study of Binary Stars - its Detection, Resolution & Classification has been undertaken using general diffraction integral. The calculation for the orbits of visual binary stars: WDS04374-0951 & WDS 18384+0850 have been undertaken along with the determination of the mass, dynamical parallax and ephemerid by using data available in ADS.

5 illus, 3 tables, 23 ref

015710   Kumaravel S;Gurugnanam P;Suresh M; Senthilkumar m;Sivanatarajan G (Earth Sciences Dep, Annamalai University, Annamalai Nagar, Chidambaram, Tamil Nadu, Email: kumaravel644@yahoo.com) : Demarcate groundwater favorable zones through geophysical and GIS study in Parivillikottai Firka, Tuticorin district, Tamilnadu, India. Ultra Scient phys Sci 2009, 21(2), 375-86.

GIS is a powerful tools in analysing the multiple thematic maps at a lime. GIS analysis is carried out in the present study to locate favorable shallow and deep groundwater bearing zones. To do this subsurface investigation and its interpretation were carried out through geophysical survey. Fifteen vertical electrical soundings (YES) survey were carried out in the study area. The field data were interpreted by RESIST software to determine the resistivity and thickness of the different layers. By using conventional GIS method, the spatial distribution maps for fracture zone resistivity and thickness zones were prepared. Integration of the said themes was done it in GIS. First layer fracture zone thickness and resistivity maps were overlaid and the polygon combinations were brought out. 9 combinations of 1LR-1LT, 1LR-1MT, 1LR-1HT, 1MR- 1LT, 1MR-1MT, 1MR-1HT, 1HR-1LT, 1HR-1MT and 1HR-1LT were arrived, and designated as output map 1. This map shows that the shallow depth groundwater combination of (1LR-1HT and 1LR-1MT) covers an area of 50.39 Km^{2 and 28.73 Km2. Similarly, the second fracture zone thickness and resistivity maps were superposed. The result map designated as output map 2 gives a combination of 9 polygons of 2LR-2LT, 2LR-2MT, 2LR-2HT, 2MR-2LT, 2MR-2MT, 2MRª2HT, 2HR-2LT, 2HR-2MT and 2HR-2LT. This map shows that the deeper depth groundwater combinations of (2LR-2HT and 2LR-2MT) for deep groundwater zones were delineated and occupies an area 00.16 Km2 and 13.10 Km2.}

8 illus, 4 tables, 11 ref

015709   Choyal Y;Gupta L;Deshpande P;Maheshwari K P; Mittal K C;Bapna S C (School of Physics, , Ahilya Vishwavidyalaya, Email: ychoyal@yahoo.com) : Development of a 2 MW relativistic backward wave oscillator. Pramana J Phys 2008, 71(6), 1301-10.

A high power relativistic backward wave oscillator (BWO) experiment is reported. A 230 keV, 2 kA, 150 ns relativistic electron beam is generated using a Marx generator. The beam is then injected into a hollow rippled wall metallic cylindrical tube that forms a slow wave structure. The beam is guided using an axial pulsed magnetic field having a peak value 1 T and duration 1 ms. The field is generated by the discharge of a capacitor bank into a solenoidal coil. A synchronization circuit ensures the generation of the electron beam at the instant when the axial magnetic field attains its peak value. The beam interacts with the SWS modes and generates microwaves due to Cherenkov interaction. Estimated power of 2 MW in TMv01D mode is observed.

9 illus, 19 ref

011434   Umezu M (Astronomical Institute, Graduate School of Science, Tohoku Univ, Sendai 980-8578, Japan, Email: umezu@astr.tohoku.ac.jp) : Instability of a convection zone with large gradient of the mean molecular weight. Bull Astr Soc India 2009, 37(3-4), 91-107.

An inefficient convective solution with non - negligible gradient of the mean molecular weight was discovered by extending the mixing-length theory of convection (Umezu & Nakakita 1988). This solution is unstable, but becomes stable if the radiative heat loss from the convective element is negligible. However, since the size of the convective element necessary to stabilize this solution is larger than the stellar radius by several orders, this inefficient convection solution never becomes stable. If the radiative heat loss is neglected, the zone with this inefficient convection solution resembles the Ledoux semicon-vection zone. Hence this study might show another reason against the Ledoux semiconvection zone.

8 illus, 1 table, 39 ref

011433   Saikia D J;Jamrozy M (NO, National Centre for Radio Astrophysics, Post Bag 3, Ganeshkhind, Pune-411 007, Email: djs@ncra.tifr.rs.in) : Recurrent activity in active galactic nuclei. Bull Astr Soc India 2009, 37(3-4), 63-89.

There has been a growing body of evidence to suggest that AGN activity, which is powered by mass accretion on to a supermasive black hole, could be episodic, although the range of time scales involved needs to be explored further. The structure and spectra of radio emission from radio galaxies, whose sizes range up to ~ 5 Mpc, contain information on the history of AGN activity in the source. They thus provide a unique opportunity to study the time scales of recurrent AGN activity. The most striking examples of recurrent activity in radio galaxies and quasars are the double-double or triple-double radio sources which contain two or three pairs of distinct lobes on opposite sides of the parent optical object. Spectral and dynamical ages of these lobes could be used to constrain time scales of episodic activity. Inverse-Compton scattered cosmic microwave background radiation could in principle probe lower Lorentz-factor particles than radio observations of synchrotron emission, and thereby reveal an older population. We review briefly the radio continuum as well as molecular and atomic gas properties of radio sources which exhibit recurrent or episodic activity, and present a few cases of quasars which require further observations to confirm their episodic nature. We also illustrate evidence of episodic AGN activity in radio sources in clusters of galaxies.

8 illus, 12 tables, 172 ref

011432   Safonova M;Shalima P;Murthy J (NO, Indian Institute of Astrophysics, Bangalore-560 034, Email: rita@iiap.res.in) : TAUVEX flight calibrations: plans and challenges. Bull Astr Soc India 2009, 37(1-2), 23-43.

The operational tasks for the Performance Verification (PV) and calibration phase in the first year of TAUVEX operation are presented. The new challenges regarding the possible reduction in sensitivity are outlined and are reflected in the specialized plan for first few months of the mission. The calibration operations will be extended into the first year, in parallel to an unprecedented deep exposure of the celestial poles. The preliminary zero-points of the instrumental photometric system, in AB and Vega-based magnitude systems, are calculated for pre-ground calibrations data as well as for the updated results. For flux calibration, the effective wavelengths, bandwidths and conversion factors are calculated for both pre-ground and updated values. These conversion factors are to be used for converting the TAUVEX count rates to flux and UV luminosity of the sources.

1 illus, 11 tables, 9 ref

011431   Munshi R;Prasad B R;Murthy J (Physics and Meterology Dep, Indian Institute of Technology, Kharagpur-721 302, Email: murthy@iiap.res.in) : Design and analysis of an FUV spectrograph for a small satellite. Bull Astr Soc India 2009, 37(1-2), 11-21.

The Halo Ultraviolet Explorer (HUE) is a payload aimed at studying the diffuse far ultraviolet sky over a bandpass of 800 - 1200 A. The novel features of HUE include a large effective collecting area (254 cm^{2) and fast (f/2.2) optics in a compact design optimized for a standard small satellite bus. We have investigated two different models, each with an 18 cm off-axis parabolic primary mirror, but one with an additional folding mirror to decrease the total length of the spectrograph. The spectrograph slit is dumbbell shaped maximizing the spectral resolution in the centre of the slit while increasing the sensitivity to diffuse sources at the edges. The primary scientific goal of the mission is to investigate the distribution of OVI in the Galactic halo. This line is a sensitive indicator of the hot gas in the interstellar medium and is critical in understanding the dynamics and energetics of the Galaxy.}

8 illus, 5 tables, 4 ref

011430   Green D A (NO, , Astrophysics Group, Govendish Laboratory, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, United Kingdom, Email: D.A.Green@mrao.cam.ac.uk) : Revised galactic supernova remnant catalogue. Bull Astr Soc India 2009, 37(1-2), 45-61.

A revised catalogue of 274 Galactic supernova remnants (SNRs) is presented, along with some simple statistics of their parameters. It is shown that the remnants that have recently been identified are generally faint, as is expected from the selection effects that apply to the identification of remnants.

3 illus, 34 ref

011429   Deb S;Tiwari S K;Singh H P;Seshadri T R; Chabye U S (Physics & Astrophysics Dep, Delhi Univ, Delhi-110 007, Email: sdeb@physics.du.ac.in) : Photometry of the δ scuti star HD 40372. Bull Astr Soc India 2009, 37(3-4), 109-23.

Presents B band photometry of the δ Scuti star HD 40372 using the ARIES three channel fast photometer attached to the 104-cm Sam-purnanand telescope in high-speed photometric mode. The star was observed for ~ 5 hours on December 13, 2008. Based on the high quality photometric data, we have done period analysis by various periodogram analysis techniques. The best estimate of the period is found to be ~ 0.067 days. With this period and the other stellar parameters determined from uvby β photometry available in the literature, we have calculated the Q value for the star. Comparison of this Q value with that determined from the model calculations shows that the star is pulsating in pa mode with l = 2.

9 illus, 2 tables, 137 ref

011428   Anand M Y;Kagali B A;Murthy J (Physics Dep, Bangalore Univ, Bangalore-560 056) : Bubble nebula using IUE high resolution spectra. Bull Astr Soc India 2009, 37(1-2), 1-10.

Analyses IUE high resolution spectra of the central star (BD+602522) of the Bubble nebula. Discusses velocities of the different regions along the line of sight to the bubble. It was found that the Bubble nebula is younger (by a factor of 100) than the exciting star suggesting that either the bubble is expanding into an inhomogeneous interstellar medium or that the mechanics of the stellar wind are not fully understood.

6 illus, 5 tables, 18 ref

010427   Fogedby H C (Physics and Astronomy Dep, Aarhus Univ, Ny Munkegade, DK-8200, Aarhus C, Denmark and Niels Bohr Institute, Copenhagen Univ, DK-2100, Copenhagen, Denmark, Email: foged@phys.au.dk) : Patterns in the Kardar-Parisi-Zhang equation. Pramana J Phys 2008, 71(2), 253-62.

Review a recent asymptotic weak noise approach to the Kardar-Parisi-Zhang equation for the kinetic growth of an interface in higher dimensions. The weak noise approach provides a many-body picture of a growing interface in terms of a network of localized growth modes. Scaling in 1d is associated with a gapless domain wall mode. The method also provides an independent argument for the existence of an upper critical dimension.

4 illus, 9 ref

009383   Nath B (NO, Raman Research Institute, C V Raman Avenue, Sadashivnagar, Bangalore-560 080, Email: biman@rri.res.in ) : Biggest explosions in the universe. Resonance 2009, 14(10), 989-95.

Gamma ray bursts - which are first detected in energetic gamma rays and which then glow in X-ray, visible and radio wavelengths - are the result of the biggest explosions in the universe. Astronomers wonder what causes these violent events, and some of their ideas are discussed.

2 illus

009382   Das S;Jain P;Ralston J P;Saha R (Astrophysical Sciences Dep, Princeton Univ, New Jersey 08544, USA, Email: pkjain@iitk.ac.in) : Dynamical mixing of light and pseudoscalar fields. Pramana J Phys 2008, 70(3), 439-56.

Solve the general problem of mixing of electromagnetic and scalar or pseudoscalar fields coupled by axion-type interactions L_int = g_ΦΦε<109>ναβF^<109>νF^αβ. The problem depends on several dimensionful scales, including the magnitude and direction of background magnetic field, the pseudoscalar mass, plasma frequency, propagation frequency, wave number, and finally the pseudoscalar coupling. We apply the results to the first consistent calculations of the mixing of light propagating in a background magnetic field of varying directions, which show a great variety of fascinating resonant and polarization effects.

5 illus, 26 ref