Polarization observations of four southern pulsars at 1560 MHz     

Wu Xin-ji  R. N. Manchester  A. G. Lyne 《Chinese Astronomy and Astrophysics》1991,15(4)

We present some interesting results from the mean pulse polarization observations of four southern pulsars made at the Australian National Radio Astronomy Observatory, Parkes, using the 64-m telescope in June and July, 1988. The 2 × 16 × 5 MHz filter system from Jodrell Bank has proved excellent in de-dispersing the pulse signals and measuring their polarization properties. We give the data for the four pulsars in some detail and discuss their spectral behaviour.  相似文献   

The sensitivity of EGRET to gamma-ray polarization     

John R. Mattox 《Experimental Astronomy》1991,2(2):75-84

A Monte Carlo simulation shows that the EGRET gamma-ray telescope aboard the GRO satellite does not have sufficient sensitivity to detect linear polarization, even for 100% polarized gamma-ray sources. This is confirmed by analysis of calibration data. Several data selection techniques suggested to enhance polarization sensitivity have been evaluated and found to not significantly improve sensitivity.NRC/NAS RESEARCH ASSOCIATE  相似文献   

UV Photopolarimetric Imaging of C/1995 O1 (Hale-Bopp) with the Wide Field Imaging Survey Polarimeter (WISP)     

Harris  W. M.  Nordsieck  K. H.  Scherb  F.  Mierkiewicz  E. J. 《Earth, Moon, and Planets》1997,78(1-3):161-167

We report on the reduction and analysis of UVpolarimetric images of CI (λ1657 Å) and dust continuum (2696 Å emissions from C/1995 O1 (Hale-Bopp) taken using the Wide Field Imaging Survey Polarimeter (WISP) sounding rocket on 8 April, 1997. These observations represent the first imaging polarimetry of comets in the UV, and were performed in consort with ground based measurements of gas and dust polarization and distribution. The continuum results show 9% polarization across the image field with a polarization phase angle close to the 129° prediction. Comparison with ground based data implies minimal color dependence for Hale-Bopp in either the degree of polarization and in the position angle. The carbon polarimetry implies that most production occurs in the dense inner coma, and that it leaves that area in thermodynamic equilibrium. Its radial profile further constrains the carbon outflow speed to be sufficient to travel ≥5 × 10⁶ km without photoionization.  相似文献   

Fading of light maximum and linear polarization variation in the carbon Mira R Leporis     

A. V. Raveendran 《Monthly notices of the Royal Astronomical Society》2002,336(3):992-998

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Helicoidal magneto-electron waves in interstellar molecular clouds     

S. I.Bastrukov  J.Yang  D. V.Podgainy 《Monthly notices of the Royal Astronomical Society》2002,330(4):901-906

We investigate the evolution of the magnetic flux density in a magnetically supported molecular cloud driven by Hall and Ohmic components of the electric field generated by the flows of thermal electrons. Particular attention is given to the wave transport of the magnetic field in a cloud whose gas dynamics is dominated by electron flows; the mobility of neutrals and ions is regarded as heavily suppressed. It is shown that electromagnetic waves penetrating such a cloud can be converted into helicons – weakly damped, circularly polarized waves in which the densities of the magnetic flux and the electron current undergo coherent oscillations. These waves are interesting in their own right, because for electron magnetohydrodynamics the low-frequency helicoidal waves have the same physical significance as the transverse Alfvén waves do for a single-component magnetohydrodynamics. The latter, as is known, are considered to be responsible for the widths of molecular lines detected in dark, magnetically supported clouds. From our numerical estimates for the group velocity and the rate of dissipation of helicons it follows that a possible contribution of these waves to the broadening of molecular lines is consistent with the conditions typical of dark molecular clouds.  相似文献   

Sharp images of young stellar objects     

N. Ageorges  A. Eckart  R. Hofmann 《Astrophysics and Space Science》1995,224(1-2):411-414

We present high resolution infrared images of the pre-main sequence star V536 Aql and polarization maps of the reflection nebula IRN Cha observed with the SHARP camera on the ESO NTT. Extended structures are observed near V536 Aql. The polarization pattern of IRN Cha is typical of a centrally illuminated source but with a central band of anomalously oriented polarization believed to occur in an optically thick disk.  相似文献   

Cosmic microwave background polarization due to scattering in clusters     

M. Shimon  Y. Rephaeli  B. W. O'Shea  M. L. Norman 《Monthly notices of the Royal Astronomical Society》2006,368(2):511-511

Scattering of the cosmic microwave background (CMB) in clusters of galaxies polarizes the radiation. We explore several polarization components which have their origin in the kinematic quadrupole moments induced by the motion of the scattering electrons, either directed or random. Polarization levels and patterns are determined in a cluster simulated by the hydrodynamical enzo code. We find that polarization signals can be as high as  ∼1 μK  , a level that may be detectable by upcoming CMB experiments.  相似文献   

Prospects for the GLAS Rayleigh laser beacon on the 4.2-m WHT     

Ren Rutten  Maarten Blanken  Richard McDermid  Thomas Gregory  Paul Jolley  Tim Morris  Richard Myers  Johan Pragt  Ton Schoenmaker  Remko Stuik  Gordon Talbot 《New Astronomy Reviews》2006,49(10-12):632

The scientific exploitation of adaptive optics (AO) with natural guide stars is severely constrained by the limited presence of bright guide stars for wavefront sensing. Use of a laser beam as an alternative means to provide a source for wavefront sensing has the potential of drastically improving the sky coverage for AO. For this reason at the 4.2-m William Herschel Telescope a project was started to develop a Rayleigh laser beacon to work together with the existing NAOMI adaptive optics instrumentation and the OASIS integral field spectrograph. This paper presents the rationale for this development, highlights some of the technical aspects, and gives some expected performance measures.  相似文献   

Polarization transfer in a pulsar magnetosphere     

S. A. Petrova 《Monthly notices of the Royal Astronomical Society》2006,366(4):1539-1550

Propagation of radio waves in the ultrarelativistic magnetized electron–positron plasma of a pulsar magnetosphere is considered. The polarization state of the original natural waves is found to vary markedly on account of the wave mode coupling and cyclotron absorption. The change is most pronounced when the regions of mode coupling and cyclotron resonance approximately coincide. In cases when the wave mode coupling occurs above and below the resonance region, the resultant polarization appears essentially distinct. The main result of the paper is that in the former case the polarization modes become non-orthogonal. The analytical treatment of the equations of polarization transfer is accompanied by numerical calculations. The observational consequences of polarization evolution in pulsar plasma are discussed as well.  相似文献   

Prompt γ-ray and early afterglow emission in the external shock model     

E. McMahon  P. Kumar  A. Panaitescu 《Monthly notices of the Royal Astronomical Society》2004,354(3):915-923

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