断盖配置渗漏油气时期确定方法及其应用     

袁红旗  曹文瑞  于英华  张亚雄 《地质论评》2021,67(2):420-428

为了客观把握含油气系统中断裂处的油气纵向分布规律,在断盖配置渗漏油气机制及其渗漏油气时期构成研究的基础上,通过厘定断裂开始破坏泥岩盖层封闭时刻、断层岩开始封闭时刻和断裂活动停止时刻,确定断盖配置渗漏时期,并结合源岩排烃史,建立了一套确定断盖配置渗漏油气时期的方法,并将其应用于渤海湾盆地南堡凹陷南堡5号油田,研究F3断裂...  相似文献   

Measurements of visual double stars with PISCO2 at the Nice 76-cm refractor in 2013–2014 (new data) and in 2015     

J.-L. Prieur  R. Gili  J.-P. Rivet  F. Vakili  M. Scardia  L. Pansecchi  R. W. Argyle  J. F. Ling  L. Piccotti  E. Aristidi  L. Koechlin  D. Bonneau  L. Maccarini  J. Serot 《Astronomische Nachrichten》2023,344(10):e20230112

We present relative astrometric and photometric measurements of visual double stars made in 2013–2015, with PISCO2 installed at the 76-cm refractor of Côte d'Azur Observatory in Nice (France). Our observing list contains orbital couples as well as double stars whose motion is still uncertain. Most of the observations were done in 2015, but some other observations of wide couples were done in 2013–2014 (0.3% of the total of the observations). Three different techniques were used for obtaining measurements: lucky imaging, speckle interferometry and the direct vector autocorrelation method. From our observations of 2837 multiple stars, we obtained 5182 new measurements with angular separations in the range of 0 ${}^{″}$.1–32 ${}^{″}$ and an average accuracy of $0^{″}.018$. The mean error on the position angles is 0°.8. Most of the position angles were determined without the usual 180° ambiguity with the application of the direct vector autocorrelation technique and/or by inspection of the Lucky images or the long integration files. We managed to routinely monitor faint systems ( $m_V\approx 9-11$) with large magnitude difference (up to $\mathrm{\Delta }{m}_V\approx 4.5$). We have thus been able to measure 21 systems containing red dwarf stars that had been poorly monitored since their discovery, from which we estimated the stellar masses thanks to Gaia measurements. We also measured the magnitude difference of the two components of 1079 double stars with an estimated error of 0.2 mag. Except for a few objects that are discussed, our measurements are in good agreement with the ephemerides computed with published orbital elements, even for the double stars whose separation is smaller than the diffraction limit. Thanks to good seeing images and with the use of high-contrast numerical filters, we have also been able to obtain 196 measurements with an angular separation smaller than the diffraction limit of our instrumentation, and consistent with those obtained with larger telescopes. We also report measurements of the 164 new double stars that we found in the files obtained during the observations. Finally, from a study of the DR3 Gaia release, it is shown that all the objects of the Tycho Double Star Catalog that we did not resolve in 2015 are probably false detections by Tycho.  相似文献   

Photometric study and absolute parameters of four short period W UMa binary stars of late spectral classes     

《New Astronomy》2022

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The knotty structure of the HII dwarf galaxy F348     

P. Rafanelli  S. Roi  A. Tegon  H. Schulz  S. Di Serego-Alighieri  S. Komossa  G. Richter  J. Vennik 《Astronomische Nachrichten》1997,318(6):319-327

[OIII] images and blue spectra of the emission-line dwarf galaxy F348 are presented. In [OIII] light, the object contains two knots about 9” NE of the nucleus and one large extended knot 11” to the SW. The nuclear region is hundred times less luminous in emission-line light than the knots. Despite the presence of line intensity ratios [OIII]λ5007/Hβ > 3 the prior classification as a Seyfert-2 object cannot be upheld. This clinches an earlier suggestion by Veron-Cetty & Veron (1986). In particular, we show that the line spectra can be modeled with photoionization models employing stellar input continua. Also, the line luminosities of the extranuclear knots are typical for giant HII regions. There is neither evidence for tidal tails nor for high velocity differences between the knots. In addition, the linear arrangement of the knots does not support interaction. It rather suggests self-propagating star formation In this picture, the faintness of the nuclear region can be understood by an edge-on view. In addition, the nuclear starburst appears to be fading in contrast to the young extranuclear star formation regions. Within the scheme of Melnick (1987), F348 has to be classified as a multiple-system HII galaxy.  相似文献