Relation of Velocity Distribution and Mass for DA White Dwarfstwo     

Xiao-bo Gong  Li-fang Li 《Chinese Astronomy and Astrophysics》2018,42(2):202-212

White dwarfs are the evolutionary endpoint of the low-and-medium mass stars. In the studies of white dwarfs, the mass of white dwarf is an important physical parameter. In this paper, we give an analysis about the velocity distribution of DA white dwarfs in the Sloan Digital Sky Survey (SDSS), and hope to find the relation between mass and velocity distribution of white dwarfs. We get the radial velocity and tangential velocity of every DA white dwarf according to their proper motion and spectral shift. Through analyzing the velocity distribution of DA white dwarfs, we find that the small-mass white dwarfs, which are produced from the single-star evolution channel, have a relatively large velocity dispersion.  相似文献   

浙江新昌早白垩世木化石新材料及内含真菌菌丝化石     

朱志鹏  李丰硕  谢奥伟  田宁  王永栋 《地质学报》2018,92(6):1149-1162

浙江新昌下白垩统馆头组是我国南方地区为数不多的白垩纪木化石产出层位。本文报道了新昌地区馆头组木化石新材料及其内含真菌菌丝化石。木化石具明显生长轮,管胞径壁纹孔南洋杉式(多数单列、椭圆形、紧挤排列,偶见双列互生排列);交叉场纹孔南洋杉式;木射线单列式,多数2~11个细胞高。当前木化石新材料具有与现生南洋杉科植物相类似的木材解剖特征,显示其应归入贝壳杉型木属(Agathoxylon Hartig)。鉴于该类型木化石的分类现状仍有待厘清,将其定为Agathoxylonsp.。木化石内含真菌菌丝化石,管状,具横隔,平直或弯曲,常以不同角度分叉,菌丝壁光滑,具典型的锁状联合,属于担子菌类。当前木化石木材组织具有明显的木材腐朽特征,与现代真菌造成的木材白腐一致,推断此真菌化石为木材白腐菌。新昌地区贝壳杉型木属木化石新材料的发现进一步丰富了馆头组木化石的多样性,有助于增进对南方地区早白垩世植物群组成特征的认识。当前真菌菌丝化石是我国南方地区首次发现白垩纪担子菌化石,为探究白垩纪时期森林生态系统真菌与植物的相互作用提供了新的化石证据。  相似文献   

海底爆破振动强度衰减规律及中华白海豚保护措施研究     

费鸿禄  关福晨  包士杰  肖绍青 《海洋通报》2019,38(4):405-414

为确保海底爆破施工所诱发的振动不对中华白海豚造成危害,基于量纲分析法对萨道夫斯基经验公式进行修正,建立适用于预测海底爆破质点峰值振动速度的相似准数方程。在此基础上根据现场试验数据进行非线性回归运算,得到相关参数并分析了海底爆破振动强度衰减规律。分析表明:海底爆破质点峰值振速主要由单段装药量、监测点距爆心水平距离、覆盖层厚度及海水深度等因素决定。将参数值分别代入萨氏公式及新建公式计算预测值并进行误差估计,其平均误差分别为20.3%和10.0%,新建公式提高了对质点振速预测的准确性。利用新建公式及超压内安全振速估算保护中华白海豚的安全距离并提出相应的保护措施,为同类工程施工提供理论参考依据。  相似文献   

三疣梭子蟹几丁质酶基因(PtCht6)的克隆及其在免疫中的功能分析     

宋柳  吕建建  王磊  孙东方  刘萍 《海洋与湖沼》2019,50(5):1080-1090

几丁质酶(chitinase)在甲壳动物的蜕皮、消化和免疫等很多生物学过程中发挥重要功能,为深入探讨几丁质酶的免疫防御机制,本实验利用RACE技术克隆了三疣梭子蟹(Portunus trituberculatus)PtCht6基因。该基因cDNA全长2736bp,开放阅读框(ORF)2103bp,编码700个氨基酸,具有几丁质酶GH18家族典型特征。利用实时荧光定量技术分析PtCht6在三疣梭子蟹不同组织、不同蜕皮阶段、不同病原感染以及低盐胁迫(11)下的表达特征,结果显示:PtCht6在各组织中均有表达且在肝胰腺中的表达量最高;在不同蜕皮时期的肝胰腺中,其表达量由蜕皮后期(A/B)、蜕皮间期(C)、蜕皮前期(D)依次递减(P0.05);人工感染WSSV和副溶血弧菌后.PtCht6的表达量在肝胰腺中分别于12h、72h达到最大值,在血细胞中均于12h达到最大值,且相较于对照组,整体显著上调表达(P0.05);低盐胁迫能够显著抑制该基因的表达,最高抑制73倍(P0.05)。同时发现,低盐环境下感染WSSV后,该基因达到峰值的时间明显延迟(至少延迟12h.P0.05)。该研究结果预示PtCht6作为免疫因子参与三疣梭子蟹的病原防御,且低盐胁迫在一定程度上抑制了该基因的免疫功能。  相似文献   

若干冶炼砷渣(场)周边水环境特征研究     

李蘅  徐文炘  梁文寿  黄伟 《矿产与地质》2015,(3)

对冶炼砒霜产生砷渣堆放后没有扰动砷渣(场)、扰动并已修复的砷渣场及扰动正在修复砷渣场周边水环境进行分析,发现长期堆放后没有被扰动的砷渣(场)周边地表水体达到《地表水环境质量标准》(GB3838—2002)Ⅲ类标准;扰动正在修复和已修复的砷渣(场)周边地表水环境恢复较快,地下水恢复较慢,恢复周期较长。  相似文献   

On non-axisymmetric magnetic equilibria in stars     

Jonathan Braithwaite 《Monthly notices of the Royal Astronomical Society》2008,386(4):1947-1958

In previous work, stable approximately axisymmetric equilibrium configurations for magnetic stars were found by numerical simulation. Here, I investigate the conditions under which more complex, non-axisymmetric configurations can form. I present numerical simulations of the formation of stable equilibria from turbulent initial conditions and demonstrate the existence of non-axisymmetric equilibria consisting of twisted flux tubes lying horizontally below the surface of the star, meandering around the star in random patterns. Whether such a non-axisymmetric equilibrium or a simple axisymmetric equilibrium forms depends on the radial profile of the strength of the initial magnetic field. The results could explain observations of non-dipolar fields on stars such as the B0.2 main-sequence star τ Sco or the pulsar 1E 1207.4-5209. The secular evolution of these equilibria due to Ohmic and buoyancy processes is also examined.  相似文献   

The pulsating DA white dwarf star EC 14012−1446: results from four epochs of time-resolved photometry     

G. Handler  E. Romero-Colmenero  J. L. Provencal  K. Sanchawala  M. A. Wood  I. Silver  W.-P. Chen 《Monthly notices of the Royal Astronomical Society》2008,388(3):1444-1456

The pulsating DA white dwarfs are the coolest degenerate stars that undergo self-driven oscillations. Understanding their interior structure will help us to understand the previous evolution of the star. To this end, we report the analysis of more than 200 h of time-resolved CCD photometry of the pulsating DA white dwarf star EC 14012−1446 acquired during four observing epochs in three different years, including a coordinated three-site campaign. A total of 19 independent frequencies in the star's light variations together with 148 combination signals up to fifth order could be detected. We are unable to obtain the period spacing of the normal modes and therefore a mass estimate of the star, but we infer a fairly short rotation period of  0.61 ±0.03 d  , assuming the rotationally split modes are  ℓ= 1  . The pulsation modes of the star undergo amplitude and frequency variations, in the sense that modes with higher radial overtone show more pronounced variability and that amplitude changes are always accompanied by frequency variations. Most of the second-order combination frequencies detected have amplitudes that are a function of their parent mode amplitudes, but we found a few cases of possible resonantly excited modes. We point out the complications in the analysis and interpretation of data sets of pulsating white dwarfs that are affected by combination frequencies of the form   f _A + f _B − f _C   intruding into the frequency range of the independent modes.  相似文献   

RR Pic (1925): a Chandra X-ray view     

Y. Pekön  &#;. Balman 《Monthly notices of the Royal Astronomical Society》2008,388(2):921-926

We present the Chandra ACIS-S3 data of the old classical nova RR Pic (1925). The source has a count rate of 0.067 ± 0.002 count s⁻¹ in the 0.3–5.0 keV energy range. We detect the orbital period of the underlying binary system in the X-ray wavelengths. We also find that the neutral hydrogen column density differs for orbital minimum and orbital maximum spectra with values  0.25^+0.23_−0.18× 10²²  and  0.64^+0.13_−0.14× 10²² cm⁻²  at 3σ confidence level. The X-ray spectrum of RR Pic can be represented by a composite model of bremsstrahlung with a photoelectric absorption, two absorption lines centered around 1.1–1.4 keV and five Gaussian lines centered at emission lines around 0.3–1.1 keV corresponding to various transitions of S, N, O, C, Ne and Fe. The bremsstrahlung temperature derived from the fits ranges from 0.99 to 1.60 keV and the unabsorbed X-ray flux is found to be  2.5^+0.4_−1.2× 10⁻¹³ erg  cm⁻² s⁻¹  in the 0.3–5.0 keV range with a luminosity of 1.1 ± 0.2  10³¹ erg s⁻¹  at 600 pc. We also detect excess emission in the spectrum possibly originating from the reverse shock in the ejecta. A fit with a cooling flow plasma emission model shows enhanced abundances of He, C, N, O and Ne in the X-ray emitting region indicating existence of diffusive mixing.  相似文献   

Spectral observations of FBS blue stellar objects in the zone δ = + 35°     

P. K. Sinamyan  A. M. Mickaelian 《Astrophysics》2008,51(2):226-232

The next list of spectral data on blue stellar objects (BSOs) is presented. 58 FBS objects in a zone with a central declination δ = + 35° were observed with the 2.6-m telescope at the Byurakan Observatory during 1990–1991. In addition, 3 objects were observed (3 CCD spectra were obtained) with the BAO 2.6-m and OHP 1.93-m telescopes in 1997–2000 using modern instrumentation. 9 white dwarfs, 47 hot subdwarfs, and 2 HBB stars have been discovered. Spectra of the 10 most interesting objects are given. __________ Translated from Astrofizika, Vol. 51, No. 2, pp. 277–283 (May 2008).  相似文献   

Spectral observations of blue stellar objects from FBS in the zone δ =+39°     

P. K. Sinamyan  A. M. Mickaelian 《Astrophysics》2008,51(1):37-47

Spectral observations of blue stellar objects from FBS are reported for the purpose of classifying them, discovering interesting new objects, and studying the FBS sample as a whole. 59 FBS objects in the zone with central declination δ =+39° were observed with the 2.6-m telescope at the Byurakan Observatory during 1987–1991. The images have been digitized with a professional scanner and processed by MIDAS in a way similar to CCD spectra. In addition, 4 objects were observed with the BAO-2.6 and OHP-1.93 telescopes using modern techniques during 1997–2000. 3 white dwarfs, 45 hot subdwarfs, 4 HBB stars, and 2 class F stars were discovered. Spectra of 20 of the most interesting objects are shown. __________ Translated from Astrofizika, Vol. 51, No. 1, pp. 51–59 (February 2008).  相似文献