The excitation and kinematical properties of H₂ and [Fe ii] in the HH 46/47 bipolar outflow     

A. J. L. Fernandes 《Monthly notices of the Royal Astronomical Society》2000,315(4):657-668

Long-slit spectra of the molecular outflow Herbig–Haro (HH) 46/47 have been taken in the J and K near-infrared bands. The observed H₂ line emission confirms the existence of a bright and extended redshifted counter-jet outflow south-west of HH 46. In contrast with the optical appearance of this object, we show that this outflow seems to be composed of two different emission regions characterized by distinct heliocentric velocities. This implies an acceleration of the counter-jet.
The observed [Fe  ii ] emission suggests an average extinction of 7–9 visual magnitudes for the region associated with the counter-jet.
Through position–velocity diagrams, we show the existence of different morphologies for the H₂ and [Fe  ii ] emission regions in the northern part of the HH 46/47 outflow. We have detected for the first time high-velocity (−250 km s⁻¹) [Fe  ii ] emission in the region bridging HH 46 to HH 47A. The two strong peaks detected can be identified with the optical positions B8 and HH 47B.
The H₂ excitation diagrams for the counter-jet shock suggest an excitation temperature for the gas of T _ex≈2600 K . The lack of emission from the higher energy H₂ lines, such as the 4–3 S(3) transition, suggests a thermal excitation scenario for the origin of the observed emission. Comparison of the H₂ line ratios with various shock models yielded useful constraints about the geometry and type of these shocks. Planar shocks can be ruled out whereas curved or bow shocks (both J- and C-type) can be parametrized to fit our data.  相似文献   

The mass of the Andromeda galaxy     

N. W. Evans  M. I. Wilkinson 《Monthly notices of the Royal Astronomical Society》2000,316(4):929-942

This paper argues that the Milky Way galaxy is probably the largest member of the Local Group. The evidence comes from estimates of the total mass of the Andromeda galaxy (M31) derived from the three-dimensional positions and radial velocities of its satellite galaxies, as well as the projected positions and radial velocities of its distant globular clusters and planetary nebulae. The available data set comprises 10 satellite galaxies, 17 distant globular clusters and nine halo planetary nebulae with radial velocities. We find that the halo of Andromeda has a mass of together with a scalelength of 90 kpc and a predominantly isotropic velocity distribution. For comparison, our earlier estimate for the Milky Way halo is Although the error bars are admittedly large, this suggests that the total mass of M31 is probably less than that of the Milky Way . We verify the robustness of our results to changes in the modelling assumptions and to errors caused by the small size and incompleteness of the data set.
Our surprising claim can be checked in several ways in the near future. The numbers of satellite galaxies, planetary nebulae and globular clusters with radial velocities can be increased by ground-based spectroscopy, while the proper motions of the companion galaxies and the unresolved cores of the globular clusters can be measured using the astrometric satellites Space Interferometry Mission ( SIM ) and Global Astrometric Interferometer for Astrophysics ( GAIA ). Using 100 globular clusters at projected radii 20 R 50 kpc with both radial velocities and proper motions, it will be possible to estimate the mass within 50 kpc to an accuracy of 20 per cent. Measuring the proper motions of the companion galaxies with SIM and GAIA will reduce the uncertainty in the total mass caused by the small size of the data set to 22 per cent.  相似文献   

Stellar dynamics in the Galactic Centre: proper motions and anisotropy     

R. Genzel  C. Pichon  A. Eckart  O. E. Gerhard  T. Ott 《Monthly notices of the Royal Astronomical Society》2000,317(2):348-374

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Mira kinematics from Hipparcos data: a Galactic bar to beyond the Solar circle     

Michael W. Feast  Patricia A. Whitelock 《Monthly notices of the Royal Astronomical Society》2000,317(2):460-487

The space motions of Mira variables are derived from radial velocities, Hipparcos proper motions and a period–luminosity relation. The previously known dependence of Mira kinematics on the period of pulsation is confirmed and refined. In addition, it is found that Miras with periods in the range 145–200 d in the general Solar neighbourhood have a net radial outward motion from the Galactic Centre of 75±18 km s⁻¹. This, together with a lag behind the circular velocity of Galactic rotation of 98±19 km s⁻¹, is interpreted as evidence for an elongation of their orbits, with their major axes aligned at an angle of ∼17° with the Sun–Galactic Centre line, towards positive Galactic longitudes. This concentration seems to be a continuation to the Solar circle and beyond of the bar-like structure of the Galactic bulge, with the orbits of some local Miras probably penetrating into the bulge. These conclusions are not sensitive to the distance scale adopted. A further analysis is given of the short-period (SP) red group of Miras discussed in companion papers in this series. In Appendix A the mean radial velocities and other data for 842 oxygen-rich Mira-like variables are tabulated. These velocities were derived from published optical and radio observations.  相似文献   

The line-of-sight velocity distributions of simulated merger remnants     

George J. Bendo  Joshua E. Barnes 《Monthly notices of the Royal Astronomical Society》2000,316(2):315-325

We use Gauss–Hermite functions to study the line-of-sight velocity distributions in simulated merger remnants. Our sample contains 16 remnants; eight produced by mergers between disc galaxies of equal mass, and eight produced by mergers between disc galaxies with mass ratios of 3:1. The equal-mass mergers display a wide range of kinematic features, including counterrotation at large radii, orthogonally rotating cores and misaligned rotational axes. Most of the unequal-mass remnants exhibit fairly regular disc-like kinematics, although two have kinematics more typical of the equal-mass remnants. Our results may be compared with observations of early-type objects, including ellipticals with misaligned kinematic axes, counterrotating systems and S0 galaxies.  相似文献   

Magnetic and optical spiral arms in the galaxy NGC 6946     

P. Frick  R. Beck  A. Shukurov  D. Sokoloff  M. Ehle †  J. Kamphuis 《Monthly notices of the Royal Astronomical Society》2000,318(3):925-937

The spiral pattern in the nearby spiral galaxy NGC 6946 has been studied using the wavelet transformation technique, applied to galaxy images in polarized and total non-thermal radio emission at λλ 3.5 and 6.2 cm, in broadband red light, in the λ 21.1 cm H  i line and in the optical Hα line. Well-defined, continuous spiral arms are visible in polarized radio emission and red light, where we can isolate a multi-armed pattern in the range of galactocentric distances 1.5–12 kpc, consisting of four long arms and one short spiral segment. The 'magnetic arms' (visible in polarized radio emission) are localized almost precisely between the optical arms. Each magnetic arm is similar in length and pitch angle to the preceding optical arm (in the sense of galactic rotation) and can be regarded as its phase-shifted image. Even details like a bifurcation of an optical arm have their phase-shifted counterparts in the magnetic arms. The average relative amplitude of the optical spiral arms (the stellar density excess over the azimuthal average) grows with galactocentric radius up to 0.3–0.7 at r ≃5 kpc, decreases by a factor of two at r =5–6 kpc and remains low at 0.2–0.3 in the outer parts of the galaxy. By contrast, the magnetic arms have a constant average relative amplitude (the excess in the regular magnetic field strength over the azimuthal average) of 0.3–0.6 in a wide radial range r =1.5–12 kpc. We briefly discuss implications of our findings for theories of galactic magnetic fields.  相似文献   

A stochastic Monte Carlo approach to model real star cluster evolution – II. Self-consistent models and primordial binaries     

M. Giersz  R. Spurzem 《Monthly notices of the Royal Astronomical Society》2000,317(3):581-606

The new approach outlined in Paper I to follow the individual formation and evolution of binaries in an evolving, equal point-mass star cluster is extended for the self-consistent treatment of relaxation and close three- and four-body encounters for many binaries (typically a few per cent of the initial number of stars in the cluster mass). The distribution of single stars is treated as a conducting gas sphere with a standard anisotropic gaseous model. A Monte Carlo technique is used to model the motion of binaries, their formation and subsequent hardening by close encounters, and their relaxation (dynamical friction) with single stars and other binaries. The results are a further approach towards a realistic model of globular clusters with primordial binaries without using special hardware. We present, as our main result, the self-consistent evolution of a cluster consisting of 300 000 equal point-mass stars, plus 30 000 equal-mass binaries over several hundred half-mass relaxation times, well into the phase where most of the binaries have been dissolved and evacuated from the core. The cluster evolution is about three times slower than found by Gao et al. Other features are rather comparable. At every moment we are able to show the individual distribution of binaries in the cluster.  相似文献   

The evolution of bodies orbiting in the trans-Neptunian region on to intermediate-type orbits     

M. D. Maran  I. P. Williams 《Monthly notices of the Royal Astronomical Society》2000,318(2):482-492

We investigate the dynamical evolution of 210 hypothetical massless bodies initially situated between 10 and 30 au from the Sun in order to determine the general characteristics of the evolved system. This is of particular relevance to the understanding of the origin of Edgeworth–Kuiper belt objects on scattered intermediate orbits, such as 1996 TL ₆₆, which have high eccentricity and semimajor axis but nevertheless have perihelion in the region between 30 and 50 au from the Sun.  相似文献   

Hydraulic pathways in the crystalline rock of the KTB   总被引：1，自引：0，他引：1  

Günter Zimmermann  Alexander Körner  & Hans Burkhardt 《Geophysical Journal International》2000,142(1):4-14

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四川盆地米仓山前陆冲断带成藏条件分析   总被引：12，自引：4，他引：8  

吴世祥  汤良杰  马永生  郭彤楼  黄仁春  程胜辉  李儒峰  陈梅涛 《地质学报》2006,80(3):337-343

本文运用层序地层学、平衡剖面分析与缩短量计算和生烃史恢复等方法,从区域构造分析和地震剖面解释入手,通过野外地质调查、地震资料解释、典型剖面平衡剖面分析和缩短量计算,结合成藏条件的分析和生烃史恢复,探讨了米仓山前陆冲断带构造演化特征,揭示该带的成藏条件和天然气富集特征。提出了米仓山演化模式,认为米仓山前陆冲断带成藏条件优越,可供钻探的圈闭发育,天然气勘探潜力巨大,储层、保存条件是成藏关键。其中,二叠系为主要烃源岩,二叠系生屑灰岩和飞仙关组鲕粒灰岩为主要储集层,雷口坡组和嘉陵江组膏盐岩层为主要盖层。并且,冲断带构造演化的时序性表现为由西向东变形强度、缩短量变小,变形时间变晚,同时前陆盆地的不同构造单元间的相互关系发生变化,造成勘探目的层系、圈闭幅度、类型的相应变化。  相似文献