A Model for the Quiescent Phase of the Recurrent Nova U Scorpii

A theoretical light curve is constructed for the quiescent phase of the recurrent nova U Scorpii in order to resolve the existing distance discrepancy between the outbursts (d approximately 6 kpc) and the quiescences (d approximately 14 kpc). Our U Sco model consists of a very massive white dwarf (WD), an accretion disk (ACDK) with a flaring-up rim, and a lobe-filling, slightly evolved, main-sequence star (MS). The model properly includes an accretion luminosity of the WD, a viscous luminosity of the ACDK, and a reflection effect of the MS and the ACDK irradiated by the WD photosphere. The B light curve is well reproduced by a model of 1.37 M middle dot in circle WD + 1.5 M middle dot in circle MS (0.8-2.0 M middle dot in circle MS is acceptable) with an ACDK having a flaring-up rim and the inclination angle of the orbit i approximately 80&j0;. The calculated color is rather blue (B-V approximately 0.0) for a suggested mass accretion rate of 2.5x10-7 M middle dot in circle yr-1, thus indicating a large color excess of E(B-V) approximately 0.56 with the observational color of B-V=0.56 in quiescence. Such a large color excess corresponds to an absorption of AV approximately 1.8 and AB approximately 2.3, which reduces the distance to 6-8 kpc. This is in good agreement with the distance estimation of 4-6 kpc for the latest outburst. Such a large intrinsic absorption is very consistent with the recently detected period change of U Sco, which is indicating a mass outflow of approximately 3x10-7 M middle dot in circle yr-1 through the outer Lagrangian points in quiescence.     

The Properties of Supernova 1997cy Associated with GRB 970514

The extraordinary SN 1997cy associated with GRB 970514 has been observed photometrically and spectroscopically for nearly 2 yr. At the time of discovery, SN 1997cy was the brightest supernova (SN) ever observed (MV相似文献   

ASCA Observation of the Quiescent X-Ray Counterpart to SGR 1627-41

We present a 2-10 keV ASCA observation of the field around the soft gamma repeater SGR 1627-41. A quiescent X-ray source, whose position is consistent both with that of a recently discovered BeppoSAX X-ray source and with the Interplanetary Network localization for this soft gamma repeater, was detected in this observation. In 2-10 keV X-rays, the spectrum of the X-ray source may be fit equally well by a power-law, blackbody, or bremsstrahlung function, with unabsorbed flux approximately 5x10-12 ergs cm-2 s-1. We do not confirm a continuation of a fading trend in the flux, and we find no evidence for periodicity, both of which were noted in the earlier BeppoSAX observations.     

A Measurement of Omega from the North American Test Flight of Boomerang

We use the angular power spectrum of the cosmic microwave background, measured during the North American test flight of the Boomerang experiment, to constrain the geometry of the universe. Within the class of cold dark matter models, we find that the overall fractional energy density of the universe Omega is constrained to be 0.85相似文献   

利用场地观测计算地表通量

高原地表的感热和潜热通量在亚洲季风系统中有很重要的作用。由于高原地域辽阔，且自然环境较严酷，不利于建立完善的地面观测系统。因此，卫星遥感观测就成为测算高原整体感热和潜热通量的有效工具。地面场地的观测结果作为地表通量的真实值，对于卫星遥感测算是非常重要的。它也为构建陆面—大气模型提供了科学依据，是卫星资料的资料同化系统中的重要组成部分。 计算场地热量通量有几种不同的处理方法。最简单的方法利用有效的观测和试验的参数，可以给出稳定连续的估计。愈精确的Bowen比或者廓线的观测能给出愈精确的信息。综合了湍流测量及辐射测量、土壤热通量的观测结果的估计对陆面—大气相互作用进行了详细的描述，以适应模式的发展。从1998年开始，这些方法联合应用到青藏高原；场地通量观测方面的成果以及目前对其理解将在本文中做一概述。     

第17章：观测地震学中的挑战

19世纪后期当仪器发展到记录地震波后地震学成为一门定量科学学科（Dewey and Bverlv，1969；Agnew所写的第1章）。地震学的基础是野外观测。过去几十年地震学的巨大进步主要是因为很好分布的观测数据数量的增加和质量的提高。电子、通讯、计算机和软件的发展使得我们收集、处理和分析数据的能力也进步很快（见Snoke and Garcia-Fernandez编辑的第85章）。     

无定形氢氧化铝的表面酸度

通过酸碱滴定法以及分析反应后的溶液和反应后固体的XRD表征等方法测定了合成氢氧化铝的表面酸度。XRD结果表现出4个宽峰,说明合成产物是无定形的。滴定实验的固体产物的XRD的分析表明,无定形的氢氧化铝在碱性的环境下(pH>10),迅速转化成为结晶的三羟铝石。滴定过程中和反应后的溶液分析计算出无定形氢氧化铝的溶解度,为1010.3。滴定实验中加入的酸或碱与溶解的铝和其表面羟基发生质子化作用或脱质子化作用。表面酸度常数,表面羟基密度和比表面积用FITEQL4.0进行了评价。无定形氢氧化铝的表面酸度@K.FUKUSHI$Research Center for…     

中国西南天山西域砾岩的磁性地层年代与地质意义*

西域组是我国西部一重要并广泛引用的晚新生代地层,关于其年代和成因至今尚存争议。在西南天山喀什远源盆地喀什-阿图什褶皱带不同构造部位选择有代表性的5~6个晚新生代地层剖面开展了详细的沉积学、磁性地层年代学对比研究,据此限定了不同构造的起始变形时间以及西域砾岩的沉积年代。西域砾岩并非一年代地层单位,作为一岩石地层单位,其底界具有穿时特征,从山体(北)向喀什前陆盆地(南)逐渐变新。其底界年龄在盆地北部近源区约为15.5Ma^[1],在盆地中部中源区约为8.6Ma^[1],在盆地南部远源区的阿图什背斜为1.9Ma,喀什背斜为1.6~0.7Ma。这一穿时的砾岩沉积楔体的起始堆积起因于盆地北部边界逆冲断层(KBT)的活动。构造变形是由北南脉冲式迁移扩展的,其速率是非均匀的,在约15.5Ma至4.0Ma期间为1.4~3.4mm/a,在约4.0Ma以来剧增至>10mm/a。西域砾岩沉积前缘向南进积速率与构造变形前缘迁移速率有很好的一致性,但在时间上较构造变形可能滞后2.0Ma。这表明构造变形前缘向南的脉冲式扩展是西域砾岩进积并发生侧向和垂向上岩相突变的主因。     

北阿尔金巴什考供-斯米尔布拉克花岗杂岩特征及锆石SHRIMP U-Pb定年

北阿尔金巴什考供-斯米尔布拉克杂岩体位于巴什考供盆地北缘, 呈东西向展布, 宽约 2~6 km, 长约30 km, 出露面积约140 km². 主要由灰黑色石英闪长岩、灰白色花岗岩、粉红色花岗岩和花岗伟晶岩组成. 围岩为前寒武系片岩、变质泥岩及变质凝灰岩. 岩石地球化学特征表明, 石英闪长岩属钙碱性系列, 具有Ⅰ型花岗岩的属性; 而粉红色和灰白色花岗岩属高钾钙碱性系列, 具有S型花岗岩的属性. 锆石SHRIMP定年结果表明, 石英闪长岩的年龄为(481.6±5.6) Ma, 而灰白色花岗岩和粉红色花岗岩的年龄在误差范围内基本一致, 分别为(437.0±3.0)~(433.1±3.4) Ma 和(443±11)~(434.6±1.6) Ma. 结合区域地质特征, 认为石英闪长岩可能形成于洋壳俯冲环境, 而灰白色和粉红色花岗岩可能形成于碰撞后环境.