X-ray beaming caused by resonance scattering in the accretion column of magnetic cataclysmic variables     

Y. Terada  M. Ishida  K. Makishima  T. Imanari  R. Fujimoto  K. Matsuzaki  H. Kaneda 《Monthly notices of the Royal Astronomical Society》2001,328(1):112-126

Extremely strong ionized Fe emission lines, with equivalent widths reaching ∼4000 eV, were discovered by ASCA from a few Galactic compact objects, including AX J2315−0592, RX J1802.1+1804 and AX J1842.8−0423. These objects are thought to be binary systems containing magnetized white dwarfs (WDs). A possible interpretation of the strong Fe K line is the line-photon collimation in the WD accretion column, as a result of resonance scattering of line photons. The collimation occurs when the accretion column has a flat shape, and the effect is augmented by the vertical velocity gradient, which reduces the resonant trapping of resonant photons along the magnetic field lines. This effect was quantitatively confirmed with Monte Carlo simulations. Furthermore, with ASCA observations of the polar V834 Centauri, this collimation effect was clearly detected as a rotational modulation of the equivalent width of the Fe K emission line. The extremely strong emission lines mentioned above can be explained consistently by our interpretation. Combining this effect with other X-ray information, the geometry and plasma parameters in the accretion column were determined.  相似文献   

Observations of a curving molecular outflow from V380 Ori-NE: further support for prompt entrainment in protostellar outflows     

C. J. Davis  W. R. F. Dent  H. E. Matthews  I. M. Coulson  M. J. McCaughrean 《Monthly notices of the Royal Astronomical Society》2000,318(3):952-960

  相似文献   

The remnant of Nova Cassiopeiae 1993 (V705 Cassiopeiae)     

S. P. S. Eyres  M. F. Bode  T. J. O'Brien  S. K. Watson  R. J. Davis 《Monthly notices of the Royal Astronomical Society》2000,318(4):1086-1092

We have detected radio emission from the remnant of V705 Cas, beginning 221 d after visual maximum. We follow the remnant from first detection while still optically thick through the turn-over to optically thin emission, and finally confirming the absence of emission due to expansion and fading by the end of 1998. While the emission is consistent with thermal bremsstrahlung, as seen in most previous novae, the small-scale structure shows two ridge-like features, which develop significantly from day 585 until our last detection on day 1544. While the development is fairly rapid, it is also much smoother than that seen in V1974 Cyg, in that we can follow individual features as they change over almost 1000 d. Our optical spectra unequivocally indicate some form of axial symmetry, as derived from the velocity structure. This is difficult to reconcile with the observed development in the radio images. We suggest a number of possible explanations.  相似文献   

Thermal stability and nova cycles in permanent superhump systems     

A. Retter  T. Naylor 《Monthly notices of the Royal Astronomical Society》2000,319(2):510-516

Archival data on permanent superhump systems are compiled to test the thermal stability of their accretion discs. We find that their discs are almost certainly thermally stable as expected. This result confirms Osaki's suggestion that permanent superhump systems form a new subclass of cataclysmic variables (CVs), with relatively short orbital periods and high mass-transfer rates. We note that if the high accretion rates estimated in permanent superhump systems represent their mean secular values, then their mass-transfer rates cannot be explained by gravitational radiation, therefore, either magnetic braking should be extrapolated to systems below the period gap or they must have mass-transfer cycles. Alternatively, a new mechanism that removes angular momentum from CVs below the gap should be invoked.
We suggest applying the nova cycle scenarios offered for systems above the period gap to the short orbital period CVs. Permanent superhumps have been observed in the two non-magnetic ex-novae with binary periods below the gap. Their post-nova magnitudes are brighter than their pre-outburst values. In one case (V1974 Cyg) it has been demonstrated that the pre-nova should have been a regular SU UMa system. Thus, it is the first nova whose accretion disc was observed to change its thermal stability. If the superhumps in this system indicate persistent high mass-transfer rates rather than a temporary change induced by irradiation from the hot post-nova white dwarf, it is the first direct evidence for mass-transfer cycles in CVs. The proposed cycles are driven by the nova eruption.  相似文献   

Spectroscopy and orbital periods of the old novae V533 Herculis, V446 Herculis and X Serpentis     

John R. Thorstensen  Cynthia J. Taylor 《Monthly notices of the Royal Astronomical Society》2000,312(3):629-637

We report spectroscopic orbital periods of 0.147 d (=3.53 h) for V533 Her, 0.207 d (=4.97 h) for V446 Her and 1.478 d for X Ser. V533 Her (Nova Herculis 1963) shows absorption features in its He  i and Balmer lines which appear only in a limited range of orbital phase, suggesting that it is a low-inclination SW Sextantis star. V446 Her is unusual in that it has started normal dwarf nova eruptions after a nova outburst, but we find nothing else unusual about it – in particular, a distance estimate based on its dwarf nova outbursts agrees nicely with another based on the rate of decline of its nova eruption, both giving d ∼1 kpc. In X Ser, unlike in other old novae with long periods, no spectral features of the secondary star are visible. This and its outburst magnitude both suggest that it is quite distant and luminous, and at least 1 kpc from the Galactic plane.  相似文献   

Superhumps in V348 Pup     

Daniel J. Rolfe  Carole A. Haswell  Joseph Patterson 《Monthly notices of the Royal Astronomical Society》2000,317(4):759-772

The eclipsing nova-like cataclysmic variable star V348 Pup exhibits a persistent luminosity modulation with a period 6 per cent longer than its 2.44-h orbital period ( P _orb). This has been interpreted as a 'positive superhump' resulting from a slowly precessing non-axisymmetric accretion disc gravitationally interacting with the secondary. We find a clear modulation of mid-eclipse times on the superhump period, which agrees well with the predictions of a simple precessing eccentric disc model. Our modelling shows that the disc light centre is on the far side of the disc from the donor star when the superhump reaches maximum light. This phasing suggests a link between superhumps in V348 Pup and late superhumps in SU UMa systems. Modelling of the full light curve and maximum entropy eclipse mapping both show that the disc emission is concentrated closer to the white dwarf at superhump maximum than at superhump minimum. We detect additional signals consistent with the beat periods between the implied disc precession period and both and  相似文献   

灌溉在现代绿洲维持与发展中的重要作用   总被引：16，自引：7，他引：9  

高艳红  陈玉春  吕世华 《中国沙漠》2002,22(4):383-386

灌溉是荒漠绿洲农业发展的根本,没有灌溉就没有干旱区农业。本文运用美国NCAR的非静力平衡中尺度模式MM5V3,模拟了1991年8月1日到11日张掖绿洲地表感热、潜热通量和波文比,模拟结果表明此模式可以较好地反映张掖绿洲地表能量及水汽交换状况。同时模拟了当水源被截断后,地表感热、潜热通量及波文比随时间的变化:潜热迅速下降,感热迅速上升,波文比绝对值也迅速增大。如不及时补充水,绿洲将最终退化为沙漠。模拟结果证明了:①在我国西北干旱区有水才有绿洲,无水便成沙漠,水是绿洲的生命线,灌溉是现代绿洲维持与发展的基础;②绿洲一旦因缺水而退化为沙漠,就很难恢复。  相似文献   

A new look at the position of the 1604 Supernova (V843 Ophiuchi)     

D. W. E. Green 《Astronomische Nachrichten》2005,326(2):101-111

The position of the supernova of 1604 (V843 Oph) is re‐assessed, with relevant discussion pertaining to the present‐day remnant, 3C 358. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

方山口铀钒型非常规铀资源地球化学特征     

王文全  漆富成  张字龙  李治兴  杨志强  张岩 《铀矿地质》2015,(1):29-35

文章以方山口U-V型非常规铀资源为研究对象,对该区矿化层和赋矿围岩进行了元素地球化学分析,结果表明:U、V呈明显正相关;在铀多金属矿化层中,与超基性岩浆有关的Cr、Co、Ni元素超常富集;稀土元素配分模式中呈现弱Ce负异常,Eu正异常;矿化层与围岩分析数据在ω(La)/ω(Yb)-∑REE图中投影点落在玄武岩区内。研究认为,方山口铀钒型非常规铀资源形成于早寒武世裂谷环境,在同沉积海相黑色岩系形成的同时,伴随着海底喷流作用,U、V多金属矿化层的形成可能与受超基性岩浆作用影响的热水作用相关联。  相似文献   

Use of magnetic measures to assess soil redistribution following deforestation in hilly region   总被引：1，自引：0，他引：1  

Parisa Mokhtari Karchegani  Shamsollah Ayoubi  Sheng Gao Lu  Naser Honarju 《Journal of Applied Geophysics》2011,75(2):227-236

Limited information is available about the use of magnetic susceptibility property to determine soil redistribution in hilly areas of the semi-arid regions. This study was conducted to evaluate the use of magnetic properties to determine soil redistribution along a hill slope following deforestation. The study area is located in the Quaternary hilly region of Lordegan district in west Iran. Ten transects were established in two land uses that included natural Querqus forested and cultivated lands. Soil samples were collected at different positions along the slope and magnetic properties (χlf, χhf, SIRM, ARM, and χfd) and selected physico-chemical properties were determined. The results (based on the χfd, SIRM/ARM) showed that the magnetic susceptibly in the calcareous materials is pre-dominantly derived during the pedogenic processes and the superparamagnetic particles which were transported to lower positions of hill slope following deforestation. The results confirmed that this methodology could be applied for monitoring soil redistribution along the slope in calcareous hilly areas in the semi-arid regions.  相似文献