Results from the Whole Earth Telescope — Indian contributions     

S. Seetha  B. N. Ashoka  T. M. K. Marar 《Journal of Astrophysics and Astronomy》2005,26(2-3):301-309

The Indian team at ISRO has been part of the Whole Earth Telescope (WET) team since 1988 when we first participated in the campaign on V471 Tau. We have been part of many other observing campaigns over the last decade. This presentation traces the circumstances leading to our joining the WET team and how useful the coverage from the Indian longitude has been. The results of several pulsators from the WET runs during which we participated are also described. These include PG1159-035 the prototype of the GW Vir type of stars, RE J 0751+14 a cataclysmic variable, PG 1336-018 a binary with an sdB pulsator and finally HR 1217 a roAp star. The paper concludes with what the limitations are in our observations and how we can overcome them in the future.  相似文献   

Evolution of Polytropic Reimann Disks in Halos     

M. G. Abrahamyan 《Astrophysics》2004,47(4):555-567

The equilibrium of elliptical Riemann disks with a polytropic equation of state and their evolution under the influence of viscosity and gravitational radiation inside spheroidal halos with a relative surface mass density k. The evolutionary trajectory of a disk inside a halo with k<0.5, which is analogous to the evolution of an isolated disk, differs from that of a disk inside a denser halo.  相似文献   

Structures in the phase space of a four dimensional symplectic map     

Ch. Skokos  G. Contopoulos  C. Polymilis 《Celestial Mechanics and Dynamical Astronomy》1996,65(3):223-251

We numerically investigate the projections of non periodic orbits in a 4-dimensional (4-D) symplectic map composed of two coupled 2-dimensional (2-D) maps. We describe in detail the structures that are produced in different planes of projection and we find how the morphology of the 4-D orbits is influenced by the features of the 2-D maps as the coupling parameter increases. We give an empirical law that describes this influence.  相似文献   

Properties of Galaxies in the Second Byurakan Survey. II. Characteristic Features of a Separate Sample of Galaxies     

L. K. Erastova 《Astrophysics》2004,47(4):547-554

Some features of a sample of galaxies from the Second Byurakan Survey are discussed. Most of them are small galaxies with star formation. It is shown that different types of galaxies are in the Survey, with high, medium, and low levels of excitation and continua ranging from blue to relatively red. Many of the galaxies have absorption lines in their spectra; their continua are formed by stars in later spectral classes.  相似文献   

IRAS　14122－5947：一颗新发现的超长周期变星     

胡景耀 《中国天文和天体物理学报》1994,(1)

ＩＲＡＳ１４１２２－５９４７是一颗新发现的变星，其Ｉｃ星等的变幅超过５．５，光变周期可能是１９３５天或３９３０天，近红外光谱与ＯＨ／ＩＲ星相似，并具有一个冷的尘埃包层。对ＳＥＤ模型拟合结果表明，它在ＡＧＢ最终阶段的质量流失率为３．６（－６）Ｍ⊙／ｙｒ．我们认为它可能是处在ＡＧＢ的最后阶段，质量流失时而进行时而停止。  相似文献   

Magnetic Field Strengths and Structures from Radio Observations of Solar Active Regions     

Chang－XiZhang  G.B.Gelfreikh 《中国天文和天体物理学报》2002,2(3):266-276

Radio observations of some active regions (ARs) obtained with the Nobeyama radioheliograph at λ=1.76cm are used for estimating the magnetic field strength in the upper chromosphere, based on thermal bremsstrahlung. The results are compared with the magnetic field strength in the photosphere from observations with the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing Astronomical Observatory. The difference in the magnetic field strength between the two layers seems reasonable. The solar radio maps of active regions obtained with the Nobeyama radioheliograph, both in total intensity (I-map) and in circular polarizations (V-map), are compared with the optical magnetograms obtained with the SMFT. The comparison between the radio map in circular polarization and the longitudinal photospheric magnetogram of a plage region suggest that the radio map in circular polarization is a kind of magnetogram of the upper chromosphere. The comparison of the radio map in total intensity with the photospheric vector magnetogram of an AR shows that the radio map in total intensity gives indications of magnetic loops in the corona, thus we have a method of defining the coronal magnetic structure from the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified three components: (a) a compact bright source; (b) a narrow elongated structure connecting two main magnetic islands of opposite polarities (observed in both the optical and radio magnetograms); (c) a wide, diffuse, weak component that corresponds to a wide structure in the solar active region which shows in most cases an S or a reversed S contour, which is probably due to the differential rotation of the Sun. The last two components suggest coronal loops on different spatial scales above the neutral line of the longitudinal photospheric magnetic field.  相似文献   

Is the Variable X—ray Source in M82 due to Gravitational Lensing？     

Da-Ming Chen 《中国天文和天体物理学报》2001,1(4):287-290

1 INTRODUCTIONObservations of the most famous starburst galaxy M82 with the High-Resolution Cameraon board the Chandra X-Ray Observatory, showed that there are nine sources in the celltral11 x 11 region, but no son-roe was detected at the galactic center (Matsumoto et al. 2001).Comparing the observations on 1999 October 28 and those on 2000 January 20, the authorsfound an extremely large time variability of the source CXO M82 J095550.2 694047, which islocated gll away from the galact…  相似文献   

激光天文动力学弱光锁相的研究     

廖安琪  倪维斗  施宙聪 《天文研究与技术》2002,331(3):88-100

近年来激光物理与应用的进展促成了激光天文动力学空间任务概念的提出。在激光天文动力学任务概念研究方面 ,必须对由远程航天器上传回的激光进行讯号的测量与处理。激光经过长距离的传输后 ,功率大幅下降 ,因此在空间任务概念的考虑上 ,弱光锁相是计划中关键性的技术。由航天器射来的激光 ,经过望远镜聚光后与本地激光进行锁相 ,由本地激光承载及传达太空激光的相位信息。实验中 ,我们使用 2支半导体激光泵浦非平面环形共振腔钇镏石激光 (Diodelaserpumpednon -planarringcavityNd :YAGlaser) ,分别代表远程的弱光及代表本地的强光 ,建立弱光锁相环路系统 (weak -lightphase -lockedloopsystem)。以中性光强度滤光器 (ND -filter;neutraldensityfilter)减弱光讯号来仿真远程激光传来的弱光。在相位探测部分使用均衡探测法 ,消除激光强度噪声 ,以提高讯噪比。同时配合适当的环路滤波器 ,控制激光频率 ,提高锁相的能力。对 2nW的弱光与 2mW的强光可长时间锁相 ,其均方根相位误差为 57mrad。 2 0 0pW的弱光与 2 0 0 μW的强光锁相时间可达 2h以上 ,其相位误差为 2 0 0mrad。 2 0pW的弱光与 2 0 0 μW的强光锁相时间亦可达 2h以上 ,其相位误差为 1 60mrad。最后 ,我们对 2pW的弱光与 2 0 0 μW的强光锁相 ,  相似文献   

Exposure dating and reinterpretation of coarse debris accumulations (‘rock glaciers’) in the Cairngorm Mountains,Scotland     

Colin K. Ballantyne  Christoph Schnabel  Sheng Xu 《第四纪科学杂志》2009,24(1):19-31

Relict rock glaciers have considerable potential for contributing to palaeoclimatic reconstruction, but this potential is often undermined by lack of dating control and problems of interpretation. Here we reinvestigate and date four proposed ‘rock glaciers’ in the Cairngorm Mountains and show that the morphology of only one of these appears consistent with that of a true rock glacier produced by creep of underlying ice or ice‐rich sediment. All four features comprise rockslide or rock avalanche runout debris, and the possibility that all four represent unmodified runout accumulations cannot be discounted. Surface exposure dating of the four debris accumulations using cosmogenic ¹⁰Be produced uncertainty‐weighted mean ages of 15.4 ± 0.8 ka, 16.2 ± 1.0 ka, 12.1 ± 0.6 ka and 12.7 ± 0.8 ka. All four ages imply emplacement under cold stadial conditions, two prior to the Windermere Interstade of ca. 14.5–12.9 cal. ka BP and two during the Loch Lomond Stade of ca. 12.9–11.5 cal. ka BP. The above ages indicate that paraglacial rock‐slope failure on granite rockwalls occurred within a few millennia after deglaciation. The mean exposure ages obtained for runout debris at two sites – Strath Nethy (16.2 ± 1.0 ka) and Lairig Ghru (15.4 ± 0.8 ka) – are consistent with basal radiocarbon ages from Loch Etteridge, 22 km to the southwest (mean = 15.6 ± 0.3 cal. ka BP) and imply widespread deglaciation of the Cairngorms and adjacent valleys before 15 ka and possibly 16 ka. Copyright © 2008 John Wiley & Sons, Ltd.  相似文献   

The brightness temperature problem in extreme intra-day variable quasars: a model for PKS 0405-385     

R. J. Protheroe 《Monthly notices of the Royal Astronomical Society》2003,341(1):230-238

I re-examine the brightness temperature problem in PKS 0405-385, which is an extreme intra-day variable radio quasar with an inferred brightness temperature of  ∼5 × 10¹⁴ K  at 5 GHz, well above the Compton catastrophe limit of  ∼10¹¹ K  that is reached when the synchrotron photon energy density exceeds the energy density of the magnetic field. If one takes into account the uncertainty in the distance to the ionized clouds responsible for interstellar scintillation causing rapid intra-day variability in PKS 0405-385, it is possible that the brightness temperature could be as low as  ∼10¹³ K  at 5 GHz, or even lower. The radio spectrum can be fitted by optically thin emission from mono-energetic electrons, or an electron spectrum with a low-energy cut-off such that the critical frequency of the lowest energy electrons is above the radio frequencies of interest. If one observes optically thin emission along a long narrow emission region, the average energy density in the emission region can be many orders of magnitude lower than calculated from the observed intensity if one assumed a spherical emission region. I discuss the physical conditions in the emission region and find that the Compton catastrophe can then be avoided using a reasonable Doppler factor. I also show that MeV to 100-GeV gamma-ray emission at observable flux levels should be expected from extreme intra-day variable sources such as PKS 0405-385.  相似文献