Evidence for a 2-h optical modulation in GS 1826 – 24     

L. Homer  P. A. Charles  & D. O''Donoghue 《Monthly notices of the Royal Astronomical Society》1998,298(2):497-501

OH maser emission from the circumstellar envelope of the M-type supergiant VX Sagittarii has been mapped at 1612 MHz in both hands of circular polarization using MERLIN, with an angular resolution of 0.4 arcsec and a velocity resolution of 0.3 km s⁻¹. Four likely Zeeman pairs of maser components are identified, each with a similar Zeeman splitting. The inferred magnetic field strength is approximately −1 mG in each case, with the field directed towards us. The Zeeman components lie ∼ 1400 au from the star. The data lend support to the dipole magnetic field model which has recently been suggested for this circumstellar envelope.  相似文献   

Radio continuum and H I observations of the supernova remnant G296.8–00.3     

Gaensler  Manchester  & Green 《Monthly notices of the Royal Astronomical Society》1998,296(4):813-823

We present Australia Telescope Compact Array (ATCA) observations of the supernova remnant (SNR) G296.8–00.3. A 1.3-GHz continuum image shows the remnant to have a complex multi-shelled appearance, with an unusual rectangular strip running through its centre. H I absorption yields a kinematic distance to the remnant of 9.6 ± 0.6 kpc, from which we estimate an age in the range (2–10) × 10³ yr. The ATCA's continuum mode allows a measurement of the Faraday rotation across the band, from which we derive a mean rotation measure towards the SNR of 430 rad m⁻². We consider possible explanations for the morphology of G296.8–00.3, and conclude that either it has a biannular structure, as might be produced through interaction with an asymmetric progenitor wind, or its appearance is caused by the effects of the surrounding interstellar medium.   We argue that the adjacent pulsar J1157–6224 is at a similar distance to the SNR, but that a physical association is highly unlikely. The pulsar is the only detectable source in the field in circular polarization, suggesting a method for finding pulsars during aperture synthesis.  相似文献   

The peculiar rotation curve of NGC 157     

Ryder  Zasov  McIntyre  Walsh  & Sil'chenko 《Monthly notices of the Royal Astronomical Society》1998,293(4):411-428

We present the results of a new H i , optical, and Hα interferometric study of the nearby spiral galaxy NGC 157. Our combined C- and D-array observations with the VLA show a large-scale, ring-like structure in the neutral hydrogen underlying the optical disc, together with an extended, low surface density component going out to nearly twice the Holmberg radius. Beginning just inside the edge of the star-forming disc, the line of nodes in the gas disc commences a 60° warp, while at the same time, the rotation velocity drops by almost half its peak value of 200 km s⁻¹, before levelling off again in the outer parts. While a flat rotation curve in NGC 157 cannot be ruled out, supportive evidence for an abrupt decline comes from the ionized gas kinematics, the optical surface photometry, and the global H i profile. A standard 'maximum-disc' mass model predicts comparable amounts of dark and luminous matter within NGC 157. Alternatively, a model employing a disc truncated at 2 disc scalelengths could equally well account for the unusual form of the rotation curve in NGC 157.  相似文献   

Class II maser candidates in substituted methanol: CH₃OD, ¹³CH₃OH, CH₃¹⁸OH and CH₃SH     

K. P. Johns  D. M. Cragg  P. D. Godfrey  & A. M. Sobolev 《Monthly notices of the Royal Astronomical Society》1998,300(4):999-1005

We investigate the possibility of interstellar masers in transitions of the methanol isotopomers CH₃OD, ¹³CH₃OH and CH₃¹⁸OH, and of CH₃SH. The model used, in which masers are pumped through the first and second torsionally excited states by IR radiation, has accounted successfully for the Class II masers in main species methanol, ¹²CH₃¹⁶OH. Several potential maser candidates are identified for CH₃OD, their detectability depending on the enrichment of this species in star-forming regions. In ¹³CH₃OH and CH₃¹⁸OH the best maser candidates are direct counterparts of the well-known 6.7- and 12.2-GHz methanol masers, but the lower interstellar abundance of these substituted species means that the expected brightness is greatly reduced. The maser candidates in CH₃SH are also weak. By comparing these species we find that the large b -component of the dipole moment in methanol plays a significant role in its propensity to form masers, as does the strong torsion–rotation interaction due to the light hydroxyl frame. Thus the exceptional brightness of interstellar methanol masers is due to a favourable combination of molecular properties as well as high interstellar abundance.  相似文献   

A search for absorption of Mg and Ca compounds in molecular clouds towards Galactic continuum sources     

Seiichi Sakamoto    Glenn J. White    Kentarou Kawaguchi    Masatoshi Ohishi    Kumiko S. Usuda  & Tetsuo Hasegawa 《Monthly notices of the Royal Astronomical Society》1998,301(3):872-880

Absorption lines of MgH and CaH N  = 1 − 0 transitions were searched for in foreground molecular clouds towards the continuum sources associated with Sgr B2 (M) and W49A (N). None of these lines was detected with our sensitivity level of ∼20 mK. Millimetric absorption lines of MgO, MgOH, CaO and CaOH were also searched for towards Sgr B2 (M) without success. The fractional abundances relative to molecular hydrogen are ≲ 1.0 × 10⁻¹¹ for MgH, ≲ 7.9 × 10⁻¹³ for MgO, ≲ 1.6 × 10⁻¹⁰ for MgOH, ≲ 1.6 × 10⁻⁹ for CaH, ≲ 2.0 × 10⁻¹² for CaO, and ≲ 2.5 × 10⁻¹⁰ for CaOH, respectively. The low abundances measured in absorption indicate that a significant fraction of interstellar magnesium and calcium cannot be tied up in their monohydrides, monoxides and monohydroxides. The low abundance of MgH also implies that grain-surface chemistry involving magnesium is not efficient and that magnesium is depleted on to grains to a factor of ≳ 10^2.5 in well-shielded molecular clouds.  相似文献   

The interstellar clouds of adams and blaauw revisited: An HI absorption study-I     

Jayadev Rajagopal  G. Srinivasan  K. S. Dwarakanath 《Journal of Astrophysics and Astronomy》1998,19(3-4):97-116

This investigation is aimed at clarifying the nature of the interstellar gas seen in absorption against bright O and B stars. Towards this end we have obtained for the first time HI absorption spectra towards radio sources very close to the lines of sight towards twenty five bright stars previously studied. In this paper we describe the selection criteria, the details regarding our observations, and finally present the absorption spectra. In the accompanying paper we analyse the results and draw conclusions.  相似文献   

Electron velocity distribution function in a plasma with temperature gradient and in the presence of suprathermal electrons: application to incoherent-scatter plasma lines     

P. Guio  J. Lilensten  W. Kofman  N. Bjørnå 《Annales Geophysicae》1998,16(10):1226-1240

The plasma dispersion function and the reduced velocity distribution function are calculated numerically for any arbitrary velocity distribution function with cylindrical symmetry along the magnetic field. The electron velocity distribution is separated into two distributions representing the distribution of the ambient electrons and the suprathermal electrons. The velocity distribution function of the ambient electrons is modelled by a near-Maxwellian distribution function in presence of a temperature gradient and a potential electric field. The velocity distribution function of the suprathermal electrons is derived from a numerical model of the angular energy flux spectrum obtained by solving the transport equation of electrons. The numerical method used to calculate the plasma dispersion function and the reduced velocity distribution is described. The numerical code is used with simulated data to evaluate the Doppler frequency asymmetry between the up- and downshifted plasma lines of the incoherent-scatter plasma lines at different wave vectors. It is shown that the observed Doppler asymmetry is more dependent on deviation from the Maxwellian through the thermal part for high-frequency radars, while for low-frequency radars the Doppler asymmetry depends more on the presence of a suprathermal population. It is also seen that the full evaluation of the plasma dispersion function gives larger Doppler asymmetry than the heat flow approximation for Langmuir waves with phase velocity about three to six times the mean thermal velocity. For such waves the moment expansion of the dispersion function is not fully valid and the full calculation of the dispersion function is needed.  相似文献   

Evidence for magma mixing in the Mariana arc system     

JAMES K.  MEEN  ROBERT J.  STERN & SHERMAN H.  BLOOMER 《Island Arc》1998,7(3):443-459

Volcanoes of the Mariana arc system produce magmas that belong to several liquid lines of descent and that originated from several different primary magmas. Despite differences in parental magmas, phenocryst assemblages are very similar throughout the arc. The different liquid lines of descent are attributed to differences in degree of silica saturation of the primary liquids and in the processes of magmatic evolution (fractional crystallization vs magma mixing). Pseudoternary projections of volcanic rocks from several arc volcanoes are used to show differences between different magmatic suites. In most of the arc, parental liquids were Ol- and Hy-normative basalts that crystallized olivine, augite, and plagioclase (± iron-titanium oxide) and then plagioclase and two pyroxenes, apparently at low pressure. Eruptive rocks follow subparallel liquid lines of descent on element–element diagrams and on pseudoternary projections. Magmas at North Hiyoshi are Ne-normative and have a liquid line of descent along the thermal divide due to precipitation of olivine, augite, and plagioclase. Derived liquids are large ion lithophile element (LILE)-rich. Magmas at other Hiyoshi seamounts included an alkaline component but had more complex evolution. Those at Central Hiyoshi formed by a process dominated by mixing alkaline and subalkaline magmas, whereas those at other Hiyoshi seamounts evolved by combined magma mixing and fractional crystallization. Influence of the alkaline component wanes as one goes south from North Hiyoshi. Alkaline and subalkaline magmas were also mixed to produce magmas erupted at the Kasuga seamounts that are behind the arc front. The alkaline magmas at both Hiyoshi and Kasuga seamounts had different sources from those of the subalkaline magmas at those sites as indicated by trace element ratios and by _Nd.  相似文献   

工程船锚泊移位系统的最优控制策略及拟静力分析   总被引：3，自引：0，他引：3  

冯刚  吴海帆等 《海洋工程》2001,19(4):1-4

锚泊移位系统以定位准确，投资小，节省能源，操纵简便等优点在海上施工工种船中获得广泛的应用。本文分析了工程船锚泊移位系统的受力特点，提出了工程船锚泊移位系统的最优控制策略和锚泊移位系统的拟静力分析方法。并以8锚工程船锚泊移位系统的设计方案为实例进行了计算分析。  相似文献   

Static Design of Cable Mooring Arrays for Offshore Guyed Towers     

Gary Orgill  James F. Wilson  Gary R. Schmertmann 《Applied Ocean Research》1985,7(3):166-174

The key consideration in controlling the dynamic response of an offshore guyed tower subjected to environmental loading is the selection of the stiffness characteristics of the cable mooring array. In the present study, each cable in the array consists of three segments: a leading segment attached to the tower, a short heavy middle segment, and a seabed trailing segment attached at the extremity to an anchor pile. A nonlinear static model is presented in algorithmic form that defines the stiffness characteristics of the cable array. The model involves the inelastic static catenary equations coupled with conditions of geometric compatibility, formulated in terms of seven nondimensional system parameters. The effects of varying each of the system parameters on the stiffness characteristics of example cable arrays are presented and the implications for cable design are discussed.  相似文献