Stellar variability in Trumpler 24. II

We present a second season of CCD time‐series observations of Trumpler 24 in Johnson B and V obtained in 2004. 18 new variable stars are found, 15 variables discovered in Paper I are discussed, and the variability class of 5 of them is given. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Low-frequency variability and binarity of the δ Scuti star XX Pyx

We analyse 147 h of single-site CCD time series photometry of the multiperiodic low-amplitude δ Scuti star XX Pyx with the aim of investigating variability at low frequencies. Part of the data were obtained in the context of the 1998 multisite campaign on XX Pyx, the results of which were described by Handler et al. We find that periodic low-frequency variations are present in the XX Pyx light curves, and we detect two frequencies at f _A=0.8695 cycle d⁻¹ and f _B=1.7352 cycle d⁻¹ , respectively, with amplitudes of 4.5 and 5.4 mmag. The low-frequency variability is intrinsic to XX Pyx, and cannot be attributed to instrumental or atmospheric effects. The near 2:1 ratio of the frequencies leads us to suggest that XX Pyx is a δ Scuti star in a binary system, with a possible binary period of 27.6 h. This is strongly supported by the detection of radial velocity variations from the re-analysis of echelle spectra obtained by Handler et al. However, in the absence of a spectroscopic period, alternative explanations of the photometric variability involving pulsation are also possible; the variations occur close to possible combination frequencies of the short-period ( δ Scuti) variations, but high Q values of 0.57 and 0.28 d suggest that the variations are not a result of normal (p-)modes. They could possibly be due to g-modes excited to observable amplitudes as a result of resonance effects. Surface features (spots) are unlikely to be the cause of the variations.
We searched for combination frequencies (  f _i − f _j ) , f being the normal δ Scuti frequencies detected by Handler et al., but failed to detect any.     

A search for H i in some peculiar faint dwarf galaxies

We present a deep Giant Metrewave Radio Telescope (GMRT) search for H  i 21-cm emission from three dwarf galaxies, viz. POX 186, SC 24 and KKR 25. Based, in part, on previous single-dish H  i observations, these galaxies have been classified as a blue compact dwarf (BCD), a dwarf irregular and a transition galaxy, respectively. However, in conflict with previous single-dish detections, we do not detect H  i in SC 24 or KKR 25. We suggest that the previous single-dish measurements were probably confused with the local Galactic emission. In the case of POX 186, we confirm the previous non-detection of H  i but with substantially improved limits on its H  i mass. Our derived upper limits on the H  i mass of SC 24 and KKR 25 are similar to the typical H  i mass limit for dwarf spheroidal (dSph) galaxies, whereas in the case of POX 186, we find that its gas content is somewhat smaller than is typical of BCD galaxies.     

An electrically powered binary star?

We propose a model for stellar binary systems consisting of a magnetic and a non-magnetic white dwarf pair which is powered principally by electrical energy. In our model the luminosity is caused by resistive heating of the stellar atmospheres arising from induced currents driven within the binary. This process is reminiscent of the Jupiter–Io system, but greatly increased in power because of the larger companion and stronger magnetic field of the primary. Electrical power is an alternative stellar luminosity source, following on from nuclear fusion and accretion. We find that this source of heating is sufficient to account for the observed X-ray luminosity of the 9.5-min binary RX J1914+24, and provides an explanation for its puzzling characteristics.     

High concentrations of marine snow and diatom algal mats in the North Pacific Subtropical Gyre: Implications for carbon and nitrogen cycles in the oligotrophic ocean

A video plankton recorder (VPR) and a remotely operated vehicle (ROV) were utilized on three cruises in the oligotrophic North Pacific Subtropical Gyre (NPSG) between 1995 and 2002 to quantify the size and abundance of marine snow and Rhizosolenia diatom mats within the upper 305 m of the water column. Quantitative image analysis of video collected by the VPR and an ROV-mounted particle imaging system provides the first transect of marine snow size and abundance across the central North Pacific Gyre extending from 920 km NW of Oahu to 555 km off Southern California. Snow abundance in the upper 55 m was surprisingly high for this oligotrophic region, with peak values of 6.0–13.0×10³ aggregates m⁻³ at the western- and easternmost stations. At stations located in the middle of the transect (farthest from HI and CA), upper water column snow abundance displayed values of 0.5–1.0×10³ aggregates m⁻³. VPR and ROV imagery also provided in situ documentation of the presence of nitrogen-transporting, vertically migrating Rhizosolenia mats from the surface to >300 m with mat abundances ranging from 0 to 10 mats m⁻³. There was clear evidence that Rhizosolenia mats commonly reach sub-nutricline depths. The mats were noted to be a common feature in the North Pacific Gyre, with the lower salinity edge of the California Current appearing to be the easternmost extent of their oceanic distribution. Based on ROV observations at depth, flux by large (1.5 cm) mats is revised upward 4.5-fold, yielding an average value of 40 μmol N m⁻² d⁻¹, a value equaling previous estimates that included much smaller mats visible only to towed optical systems. Our results suggest that the occurrence across a broad region of the NPSG of particulate organic matter production events represented by high concentrations of Rhizosolenia mats, associated mesozooplankton, and abundant detrital marine aggregates may represent significant stochastic components in the overall carbon, nitrogen, and silica budgets of the oligotrophic subtropical gyre. Likewise, their presence has important implications for the proposed climate-driven, ecosystem reorganization or domain shift occurring in the NPSG.     

24-表油菜素内酯对龙须菜抗高温胁迫的研究

本研究采用不同浓度24-表油菜素内酯处理海洋红藻龙须菜,研究热激胁迫后龙须菜的生长速率、叶绿素荧光参数、抗氧化酶活性、甘露醇、丙二醛、藻胆蛋白含量,以及HSP70、PE、GR基因的相对表达水平变化规律。结果显示,0.1mg/L 24-表油菜素内酯的处理组生长速率最大,显著高于其他处理组及对照组;叶绿素荧光参数Fv/Fm、qP和ΦPSⅡ均随高温逆境时间延长呈现下降趋势,荧光参数NPQ随着高温逆境时间延长呈现先上升后下降的趋势,且处理组各项荧光参数值均高于对照组;处理组的抗氧化酶(SOD和POD)的酶活显著高于对照组;甘露醇及藻胆蛋白含量均在0.1mg/L处理组最高,在第三天达到最大值,而丙二醛含量则在0.1mg/L处理组最低,在第三天达到最小值;处理组HSP70、PE、GR基因的相对表达量均高于对照组,且0.1mg/L处理组各基因表达量最高。以上结果表明24-表油菜素内酯能提高龙须菜的抗高温能力,且0.1mg/L处理组效果最好。     

2014年5月云南盈江两次中强地震震源参数研究

本文采用“剪切-粘贴”(CAP, Cut And Paste)方法, 分别利用区域地震台网的宽频带记录和全球地震台网宽频带记录, 独立反演和联合反演了云南盈江2014年5月24日5.6级和5月30日6.1级地震震源参数。 结果表明, 采用近震和远震数据联合反演结果更为稳定, 5月24日5.6级地震震源机制解两个节面分别为: 走向153°/倾向90°/滑动角171°和243°/81°/0°, 5月30日6.1级地震两个节面分别为172°/72°/180°和82°/90°/-18°。 两次地震断层参数较为接近, 均为走滑型地震, 结合区域构造背景和地震序列重定位结果认为其发震断层可能为近南北向苏典断裂。 震源机制解反演结果与震源区历史地震震源机制解和利用其它方法得到的机制解相近, 也符合震源区的区域应力场特征。 两次地震反演最佳震源深度分别为8 km和6 km, 均为发生在上地壳的浅源地震, 表明苏典断裂在此部位可能并没有切割到地壳深部。     

晋县凹陷未熟蒸发岩沉积物中C22-C27甾烯和C24-C30四环萜烷的检出

晋县凹陷赵芯2井（2459m,Ezk）低熟蒸发岩样品中检出了异常分布的C22-C27甾烯和C24-C30四环萜烷（17,21-断藿烷）,但在同井更深、成熟度相对更高的沉积物中并未检出。实测镜质组反射率R^0=0．43％以及芳烃馏分中有高丰度的苯并噻吩和多烷基化的二苯并噻吩,说明热催化作用成因是不可能的,微生物参与成为最可能的生成途经。沉积抽提物未显示出常规生物降解的痕迹,因此这些化合物很可能是在早期成岩阶段特定微生物作用的结果。该区油样中检出的C21-C29甾烷的特征与同时检出的C22-C27甾烯特征一致,进一步表明微生物作用的可能性;高丰度的C24-C30四环萜烷（17,21-断藿烷）和常规藿烷、甲基藿烷相匹配,以及高丰度的C22-C27甾烯和规则甾烷缺失相匹配,特别是芳烃馏分中多取代二苯并噻吩类有机含硫化合物的检出,均表明异常分布的C22-C27甾烯与C24-C30四环萜烷类似,很可能是早期成岩阶段微生物改造作用下的产物。     

海底地震数据记录器

海底地震数据记录器是一种大动态、宽频带数字仪器，能用 于海底或陆地边远地区记录地震数据. 它体积小、重量轻、操作简单，采用两个缓存存 储器控制PC/104嵌入式计算机，能在低功耗、长时间连续记录地震数据. 记录器的关键部件 是PC/104嵌入式计算机，能保证记录器工作可靠. 它使用硬盘存储数据，2GB的硬盘能容纳 19998 GB的地震数据，记录地震数据多长时间由抽样率决定.     

The micro-glitch in PSR B1821−24: a case for a strange pulsar?

The single glitch observed in PSR B1821−24, a millisecond pulsar in M28, is unusual on two counts. First, the magnitude of this glitch is at least an order of magnitude smaller  (Δν/ν∼ 10⁻¹¹)  than the smallest glitch observed to date. Secondly, all other glitching pulsars have strong magnetic fields with   B ≳ 10¹¹ G  and are young, whereas PSR B1821−24 is an old recycled pulsar with a field strength of  2.25 × 10⁹ G  . We have earlier suggested that some of the recycled pulsars could actually be strange quark stars. In this work, we argue that the crustal properties of such a strange pulsar are just right to give rise to a glitch of this magnitude, explaining the scarcity of larger glitches in millisecond pulsars.