The polarimetric nature of HD 108     

Geoffrey K.Fox  Dean C.Hines 《Monthly notices of the Royal Astronomical Society》1998,295(2):423-427

V -band polarimetric observations of HD 108 were obtained during 1994 August and September. This is the first time that the temporal polarimetric variability of this star has been investigated. Its percentage polarization and position angle vary randomly, and no evidence of its proposed binary nature is detected. The random variability is consistent with that seen for previously observed Wolf–Rayet stars and OB supergiants. Nightly variations do show some systematic behaviour consistent with the blob ejection model of Underhill & Fehey (1984). From the data it is estimated that the mass-loss rate resulting from blobs is ∼1-10⁻⁷ M⊙ yr⁻¹. The total mass-loss rate of the star is estimated to be ∼1-10⁻⁵ M⊙ yr⁻¹. The stellar rotation rate is estimated to be V _rot∼400 km s⁻¹ with an inclination of i <20c. The data are also interpreted in terms of perturbations occurring in an equatorial disc plus bipolar jets viewed equatorially (Underhill 1994). It is found that the perturbation mass-loss rate is about ∼3-10⁻⁷ M⊙ yr⁻¹, giving a total mass-loss rate for the star of 13-10⁻⁵ M⊙ yr⁻¹. Both models are consistent with HD 108 being an OB supergiant or of the class Ofpe/WR9.  相似文献   

A search for optical polarization from the narrow-line Seyfert 1 galaxy RE J1034+396     

Breeveld  & Puchnarewicz 《Monthly notices of the Royal Astronomical Society》1998,295(3):568-572

We present spectropolarimetry data on RE J1034+396, an ultra-soft X-ray narrow-line Seyfert 1 galaxy, and find an upper limit of ∼ 0.4 to the linear polarization in the optical band. This suggests that there is no synchrotron emission in this AGN, and thus it is unlikely that RE J1034+396 is related to BL Lac objects. Furthermore, any other polarization arising from transmission through dust, or reflection from dust and electrons, must be cancelled out by geometrical effects or diluted to a high degree by unpolarized radiation.  相似文献   

Impedance characteristics of carbon steel under cathodic protection   总被引：1，自引：0，他引：1  

李言涛  侯保荣 《中国海洋湖沼学报》1998,16(1):60-63

INTRODUCTIONInpraCticalengineeringapplicati0ns,thecormsionofstalundercathodicprotalioncanbecontr0llediftheproodi0np0tenhalisset2O()t03(X)mVnegativewithaspeCttothenatamlcormsi0np0tenial(MasatSugi,l976,Takehiko,l972).Theprotalnp0tentia1edinpraedcalapplicationisbedonexperienceandtheory.Tooru(l985,l986)foundthattheopbocathodicproodionpotentialcoinddedwiththepotentialwhenpolarhati0nresistancemaxndnd,s0thiscoinedencecanbeedt00btainoptbore-sultforcarbonstalundercathodicpronaion.Inthiswork,the…  相似文献   

东川汤丹铜矿床石英真空击碎及其粉末阶段加热^40Ar—^39Ar年龄谱的含义   总被引：17，自引：5，他引：12  

邱华宁  孙大中 《地球化学》1998,27(4):335-343

采用真空击碎技术提取东川汤丹铜矿床石英流体包裹体进行40Ar-39Ar法年龄测定,获得了逐渐下降的阶梯形年龄谱,表明流体包裹体含有过剩氩;数据点在40Ar／36Ar-39Ar／36Ar图解上构成等时线,等时线年龄为（712±33）Ma,代表了矿床的形成年龄。随后对其粉末进行40Ar-39Ar阶段加热（100—800℃）分析,形成相对比较平坦的年龄谱,坪年龄为（317±6）Ma（39Ar占45％,含真空击碎分析在内）,粉末加热分析全部数据点构成的等时线年龄为（321±13）Ma。电子探针分析和显微镜观察证实了该石英样品中含有粒径大于100μm,K2O含量为8％-10％,形成时间明显晚于石英的白云母类富钾矿物,粉末阶段加热分析结果表明～320Ma应为后期白云母类矿物的年龄。  相似文献   

TRES-Ⅰ型多分量瑞利波勘探仪的研究及应用     

李锦飞 《物探与化探》1998,22(2):129-133

提出多分量瑞利波勘探的技术思想和方法,研制成功专用的防爆型多分量瑞利波勘探仪器,建立了在用极化分析对瑞利波勘探记录的多分量信号分析的基础上,用极化滤波提取有效瑞利波信号的方法。在煤矿井下及地面实际应用表明,多分量瑞利波勘探与单分量法比较,信号的信噪比、勘探深度和可靠性均有一定的提高。  相似文献   

Polarization observations of the radio cores of AGN — I. A sample of quasars     

D. J. Saikia  G. F. Holmes  A. R. Kulkarni  C. J. Salter  & S. T. Garrington 《Monthly notices of the Royal Astronomical Society》1998,298(3):877-887

We present total-intensity and linear-polarization observations at a single epoch for a sample of 11 quasars and one BL Lac object. The data were taken with the VLA A array at λλ 20, 18, 6 and 2 cm. We examine the variation of the degree of polarization, p , and polarization position angle, PA, with wavelength, and attempt to determine the rotation measure, RM, of the cores in these sources. The degree of polarization does not exhibit any systematic variation with wavelength, the median values ranging from 2.3 to 3.5 per cent at the different wavelengths. The variation of PA with λ² is not linear over the entire wavelength range. However, for most sources the λλ 20-, 18- and 6-cm PAs do follow such a linear relationship, yielding a median |RM| of about 15 rad m⁻². In contrast, the λλ 6- and 2-cm observations give a median |RM| of about 129 rad m⁻². The long-wavelength emission is likely to originate from a spatially different part of the milliarcsec-scale jet from the λ 2-cm emission, which could turn over at a higher frequency and is likely to be more compact and located closer to the quasar nucleus. We have attempted to obtain linear fits over the entire wavelength range allowing for n  π ambiguities in the PAs, but the fits are not statistically significant. The low values of RM for these core-dominated sources suggest that either the radio emission from the jet intercepts few of the emission-line clouds and their confining medium, or the clouds have a small filling factor and are possibly magnetically confined.  相似文献   

A Polarization Study of Radio Galaxies and Quasars selected from the Molonglo Complete Sample     

C. H. Ishwara-Chandra  D. J. Saikia  V. K. Kapahi  & P. J. McCarthy 《Monthly notices of the Royal Astronomical Society》1998,300(1):269-286

We present total intensity and linear polarization observations made with the Very Large Array at λλ20 and 6 cm of a representative sample of 42 radio galaxies and quasars selected from the Molonglo complete sample. The sources have been chosen to be of large size to probe the depolarizing medium on these scales using our present data and later with observations at lower frequencies with the Giant Metrewave Radio Telescope. The λ20 and 6 cm data are of similar resolutions and show that depolarization between these two wavelengths is seen largely only in those lobes which are within about 300 kpc of the parent galaxy. Examination of the depolarization of the lobes with arm-length asymmetry shows that depolarization is observed predominantly for the lobe which is closer to the nucleus. There is also a trend for the lobe closer to the nucleus to be brighter, consistent with the scenario that the nearer lobe is interacting with a denser environment which is responsible for the higher depolarization and greater dissipation of energy. We have also examined the depolarization asymmetry of the lobes on opposite sides of the nucleus for galaxies and quasars. This shows that the depolarization asymmetry for quasars is marginally higher than that for galaxies. The depolarization properties of our sample are possibly determined by an asymmetric environment as well as the effects of orientation.  相似文献   

Natural entropy production in an inflationary model for a polarized vacuum     

Marcelo Samuel Berman  Murari M. Som 《Astrophysics and Space Science》2007,310(3-4):277-279

Though entropy production is forbidden in standard FRW Cosmology, Berman and Som presented a simple inflationary model where entropy production by bulk viscosity, during standard inflation without ad hoc pressure terms can be accommodated with Robertson–Walker’s metric, so the requirement that the early Universe be anisotropic is not essential in order to have entropy growth during inflationary phase, as we show. Entropy also grows due to shear viscosity, for the anisotropic case. The intrinsically inflationary metric that we propose can be thought of as defining a polarized vacuum, and leads directly to the desired effects without the need of introducing extra pressure terms.  相似文献   

γ-ray burst ultraviolet/optical afterglow polarimetry as a probe of quantum gravity     

Yi-Zhong Fan †  Da-Ming Wei  Dong Xu 《Monthly notices of the Royal Astronomical Society》2007,376(4):1857-1860

  相似文献   

Constraining the geometry of the neutron star RX J1856.5−3754     

Wynn C. G. Ho 《Monthly notices of the Royal Astronomical Society》2007,380(1):71-77

RX J1856.5−3754 is one of the brightest, nearby isolated neutron stars (NSs), and considerable observational resources have been devoted to its study. In previous work, we found that our latest models of a magnetic, hydrogen atmosphere match well the entire spectrum, from X-rays to optical (with best-fitting NS radius   R ≈ 14  km, gravitational redshift   z _g∼ 0.2  , and magnetic field   B ≈ 4 × 10¹²  G). A remaining puzzle is the non-detection of rotational modulation of the X-ray emission, despite extensive searches. The situation changed recently with XMM–Newton observations that uncovered 7-s pulsations at the     level. By comparing the predictions of our model (which includes simple dipolar-like surface distributions of magnetic field and temperature) with the observed brightness variations, we are able to constrain the geometry of RX J1856.5−3754, with one angle <6° and the other angle     , though the solutions are not definitive, given the observational and model uncertainties. These angles indicate a close alignment between the rotation and the magnetic axes or between the rotation axis and the observer. We discuss our results in the context of RX J1856.5−3754 being a normal radio pulsar and a candidate for observation by future X-ray polarization missions such as Constellation-X or XEUS .  相似文献