Spectropolarimetry and IR photometry of magnetic white dwarfs: Vacuum polarization or rydberg states in their magnetic fields?

We suggest two mechanisms to explain IR photometric and spectropolarimetric observations of magnetic white dwarfs: vacuum polarization and the existence of Rydberg atomic states with large dipole moments arising due to atomic collisions in the strong magnetic field of the white dwarf (so-called magnetic collision-induced absorption, or magnetic CIA). Both mechanisms can explain the observed rotations of the polarization ellipses and the depression of the IR spectral energy distribution. We present the results of spectropolarimetric observations of several magnetic white dwarfs with the Special Astrophysical Observatory 6-m telescope, together with photometric observations in the near-IR obtained with the Russian-Italian AZT-24 Telescope at Campo Imperatore.     

The possible escape of electron cyclotron maser radiation from hot stellar coronas through a window of transparency

The main argument against the idea that the intense radio emission observed from active regions on the Sun and flare stars is electron-cyclotron maser (ECM) radiation is that such radiation should be strongly absorbed in higher-lying layers where the condition for the cyclotron resonance at harmonics of the electron gyrofrequency is fulfilled. Cyclotron absorption lowers the efficiency of ECM radiation virtually to zero for a broad range of angles between the direction of propagation of the radiation and the magnetic field. Less severe absorption is possible only in narrow angular “windows” along (for ordinary and extraordinary waves) and perpendicular to (for ordinary waves) the magnetic field. However, the ECM radiation that is generated does not fall into these windows of transparency due to the kinematic conditions corresponding to coronal magnetic traps. We investigate the efficiency of induced scattering of ECM radiation on ions in the equilibrium plasma in the source. Under certain conditions, induced scattering leads to the formation of a condensate of ECM radiation with the direction of its wave vectors approximately along the magnetic field, enabling the escape of the radiation through windows of transparency. The most favorable conditions for this phenomenon are realized for ordinary waves. We estimate the optical depths of the sources of the ECM radiation to the scattering and the angular width of the condensate for ordinary and extraordinary waves for the cases of the flare radio emission of the star AD Leo and the sources of type I noise storms in the solar corona. In both cases, the polarization of the emergent radiation should correspond to the ordinary wave.     

Variability of the photospheric radiation of active K-M dwarfs and their X-ray luminosities

Variability of the photospheric radiation of 40 (dKe-dMe) dwarfs in the solar neighborhood due to variations in the spottedness of their surfaces is analyzed based on the behavior of their mean annual brightnesses over long time intervals. The amplitudes and characteristic time scales of the variations of the mean annual brightness are taken to be indicators of photospheric activity and were used to infer the levels of photospheric activity in the stars studied. The influence of axial rotation on the development of cyclic activity in young red dwarfs and F-M main-sequence stars is analyzed. The durations and amplitudes of the photospheric variability of rapidly rotating (dK0e-dK5e) stars testifies to a higher level of photospheric activity among red dwarfs and solar-type stars. The X-ray luminosities of these stars grow with the amplitude of the variations of the mean annual brightness. However, this is not typical of rapidly rotating M dwarfs, for which the X-ray emission varies by more than two orders of magnitude, although their degrees of spottedness are all virtually the same. A linear relationship between the X-ray and bolometric luminosities is observed for young (dKe-dMe) stars, with their ratios log(L _x/L _bol) being about ?3. These properties can be used to determine whether a red dwarf is a young star or is already on the main sequence.     

混凝土热学参数试验与反分析研究

确定混凝土绝热温升和表面散热系数需要专用设备,价格昂贵,且和施工现场存在较大误差。针对这一问题,采用基于施工现场的混凝土立方体非绝热温升试验,结合非稳定温度场求解的三维有限单元法仿真计算技术和反问题优化求解的遗传算法,以辨别和确定包括热交换系数、绝热温升和绝热温升规律系数在内的混凝土热学特性参数。反演结果表明,所得参数能真实反映混凝土的热学性能,遗传算法作为一种优化算法,具有收敛速度快、效果好等特点。     

Linear polarization of the radiation from active galactic nuclei and the redshift dependence of their main parameters

We consider the observed continuum linear polarization of extragalactic objects with various redshifts z, most of which have degrees of polarization p ≤ 10%. We propose that this polarization is due to multiple scattering of the radiation in magnetized accretion disks around the Active Galactic Nuclei (AGN; the Milne problem in an optically thick atmosphere). The structure of the accretion disks and the polarization of the emergent radiation depend on the main parameters of the AGN—the mass of the central body M _BH , accretion rate $ \dot M $ \dot M , magnetic field at the black-hole event horizon B _H , angular momentum a _*, and the explicit form of the magnetic-field distribution in the accretion disk. Theoretical expressions for the degree of polarization are averaged over all angles of the disks to the line of sight, and the resulting formula compared with the mean observed polarizations in redshift intervals Δz = 0.25. The dependence of the observed degree of polarization and the main parameters on the redshift z is derived. The degrees of polarization of 305 objects from the catalog of Hutsemekers et al. with redshifts from zero to z = 2.25 are used for the analysis.     

Thermal constraints on the early history of the H-chondrite parent body reconsidered

Reconstructions of the early thermal history of the H-chondrite parent body have focused on two competing hypotheses. The first posits an undisturbed thermal evolution in which the degree of metamorphism increases with depth, yielding an “onion-shell” structure. The second posits an early fragmentation-reassembly event that interrupted this orderly cooling process. Here, we test these hypotheses by collecting a large number of previously published closure age and cooling rate data and comparing them to a suite of numerical models of thermal evolution in an idealized parent body. We find that the onion-shell hypothesis, when applied to a parent body of radius 75-130 km with a thermally insulating regolith, is able to explain 20 of the 21 closure age data and 62 of the 71 cooling rates. Furthermore, six of the eight meteorites for which multiple data (at different temperatures) are available, can be accounted for by onion-shell thermal histories. We therefore conclude that no catastrophic disruption of the H-chondrite parent body occurred during its early thermal history. The relatively small number of data not explained by the onion-shell hypothesis may indicate the formation of impact craters on the parent body which, while large enough to excavate all petrologic types, were small enough to leave the parent body largely intact. Impact events fulfilling these requirements would likely have produced transient crater diameters at least 30% of the parent body diameter.     

A finite temperature chandrasekhar model: Determining the parameters and calculation of the characteristics of degenerate dwarfs

We suggest a generalization of the standard Chandrasekhar model for degenerate dwarfs. We apply an equation of state for a degenerate ideal electron gas in the form of a Sommerfeld expansion in the parameter k _B T(r)/m ₀ c ². The radial temperature distribution T(r) is modeled taking into account the presence of the isothermal core. The model has four dimensionless parameters, two microscopic (the relativistic parameter at the stellar center x ₀ and the chemical-composition parameter ?? _e = A/Z) and two macroscopic (the dimensionless temperature T ₀ ^* = k _B T _c /m ₀ c ² and dimensionless radius ?? ₀ = R _c /R of the core, where R _c and R are the radii of the core and dwarf). We found x ₀, ?? _e , and T ₀ ^* for about 3000 DA white dwarfs, based on their masses, radii, and effective temperatures from the Sloan Digital Sky Survey Data Release 4; ?? ₀ was treated as a free parameter. The influence of temperature effects on the macroscopic characteristics is analyzed, in particular, the minimum mass and maximum radii of the stars. Based on our computed energy-radius dependence, we suggest an interpretation of the observed radius distribution for these dwarfs.     

Lunar volcanic glasses and their constraints on mare petrogenesis

Volcanic glasses from the Apollo 11, 14, 15, and 16 landing sites have been analyzed for major elements and Ni by electron microprobe. The 19 varieties of volcanic glass define two distinct chemical arrays that provide new insights into (a) the petrogenesis of mare basalts and (b) the structure of the deep lunar interior. A simple model is proposed whereby mare basaltic liquids may have been derived from two isolated, cumulate systems occurring at depths of ~300 km and ? 400 km. Each system was itself composed of two lithologic components (low-Ti vs high-Ti) that underwent hybridization, assimilation, or mixing to generate the large compositional range of magmas observed within each array. While the distribution of the two components within each system was locally heterogeneous, data indicate that the components themselves were chemically uniform on at least a regional scale. The surface-correlated volatiles associated with the lunar volcanic glasses seem to have come from some other reservoir within the Moon.The simplicity of the chemical relationships observed among the lunar volcanic glasses allow specific-predictions to be made. We believe that they should readily reveal any strengths or weaknesses of this new model.     

Thermal constraints on disposal of heat-emitting waste in argillaceous rocks

Although the post-closure thermal phase of a repository containing heat-emitting radioactive wastes is likely to be of comparatively short duration when judged against performance assessment time-scales, the effects of temperature increase and associated thermal gradients within an argillaceous host-rock are likely to be wide-ranging and include: (a) geomechanical effects on the rock-mass and engineered structures (linings, emplacement boreholes, etc.), (b) perturbation of groundwater pressures and flow by ‘aquathermal mechanisms’, (c) possible near-field effects on mass transport properties and mechanisms (e.g. coupled flow phenomena), and (d) effects on the chemical evolution of the near-field environment. Maximum allowable temperature in a repository is likely to be constrained by host-rock and/or clay buffer/backfill thermal behaviour. Given the diverse range of the thermal responses, the identification of a primary constraint on near-field temperature and the specification of a maximum allowable temperature remains problematic.     

浅成岩体引发的流体超压与岩石破裂及其对成矿的制约

浅成岩体成矿系统是一类非常重要的复杂动力学系统。在这类系统中,由浅成岩体引发的流体超压以及因此而促发的岩石破裂是制约成矿的关键动力过程。文章在综合前人有关研究成果的基础上,结合对铜陵—安庆地区夕卡岩矿床的研究,从理论上对浅成岩体成矿过程中流体超压的重要性、形成机制及其对成矿作用的制约进行了系统论述。夕卡岩矿床与角砾岩间...     

Merging of components in close binaries: Type Ia supernovae,massive white dwarfs,and Ap stars

The “Scenario Machine” (a computer code designed for studies of the evolution of close binaries) was used to carry out a population synthesis for a wide range of merging astrophysical objects: main-sequence stars with main-sequence stars; white dwarfs with white dwarfs, neutron stars, and black holes; neutron stars with neutron stars and black holes; and black holes with black holes. We calculate the rates of such events, and plot the mass distributions for merging white dwarfs and main-sequence stars. It is shown that Type Ia supernovae can be used as standard candles only after approximately one billion years of evolution of galaxies. In the course of this evolution, the average energy of Type Ia supernovae should decrease by roughly 10%; the maximum and minimum energies of Type Ia supernovae may differ by no less than by a factor of 1.5. This circumstance must be taken into account at estimating the parameters of the Universe expansion acceleration. According to theoretical estimates, the most massive—as a rule, magnetic—white dwarfs probably originate from mergers of white dwarfs of lower mass. At least some magnetic Ap and Bp stars may form in mergers of low-mass main-sequence stars (M ? 1.5 M _⊙) with convective envelopes.     

Peridotitic diamonds from Namibia: constraints on the composition and evolution of their mantle source

About half the diamonds studied from the Cenozoic placer deposits along the Namibian coast belong to the peridotitic suite. The peridotitic mantle source is heterogeneous ranging from lherzolitic to strongly Ca depleted (down to 0.24 wt.% CaO in garnet) and shows large variations in Cr/Al ratio, illustrated by very low to very high Cr₂O₃ contents in garnet (2.6–17.3 wt.%). The Cr-rich end of this range includes exceptionally high Cr₂O₃ contents in Mg-chromite (70.7 wt.%) and clinopyroxene (3.6 wt.%). Garnet-olivine thermometry appears to indicate two groups, one that equilibrated at temperatures between 1200 and 1220°C and a second between 960 and 1100°C. Combined estimates of pressure and temperature based on garnet-orthopyroxene pairs indicate a large variance in geothermal gradients, corresponding to 38–42 mW/m² surface heat flow.

The trace-element composition of peridotitic garnet inclusions (determined by SIMS) also indicates large diversity. Two principal groups, corresponding to different styles of metasomatic source enrichment, are recognized. The first group ranges from extremely LREE_N-depleted patterns, through trough-shaped REE_N to sinusoidal patterns with the position of the first peak gradually moving from the LREE_N to the MREE_N. This series of REE patterns is interpreted to reflect a range of metasomatic agents with decreasing LREE/HREE. Only in the case of the two garnets with REE_N peaking at Sm–Eu is this process connected with enrichment in Zr, without significant introduction of Y and Ti. The metasomatism responsible is interpreted as reflecting percolation of CHO-fluids through harzburgite under sub-solidus conditions. A second group of garnets shows an increase from LREE_N–MREE_N and almost flat (lherzolitic garnet) to moderately declining MREE_N–HREE_N at super-chondritic levels. This second style of metasomatism is caused by an agent carrying HFSE and showing only moderate enrichment in LREE over HREE, which points towards silicate melts.     

Thermal metamorphism of the Arunachal Himalaya, India: Raman thermometry and thermochronological constraints on the tectono-thermal evolution

Determination of the peak thermal condition is vital in order to understand tectono-thermal evolution of the Himalayan belt. The Lesser Himalayan Sequence (LHS) in the Western Arunachal Pradesh, being rich in carbonaceous material (CM), facilitates the determination of peak metamorphic temperature based on Raman spectroscopy of carbonaceous material (RSCM). In this study, we have used RSCM method of Beyssac et al. (J Metamorph Geol 20:859–871, 2002a) and Rahl et al. (Earth Planet Sci Lett 240:339–354, 2005) to estimate the thermal history of LHS and Siwalik foreland from the western Arunachal Pradesh. The study indicates that the temperature of 700–800 °C in the Greater Himalayan Sequence (GHS) decreases to 650–700 °C in the main central thrust zone (MCTZ) and decreases further to <200 °C in the Mio-Pliocene sequence of Siwaliks. The work demonstrates greater reliability of Rahl et al.’s (Earth Planet Sci Lett 240:339–354, 2005) RSCM method for temperatures >600 and <340 °C. We show that the higher and lower zones of Bomdila Gneiss (BG) experienced temperature of ~600 °C and exhumed at different stages along the Bomdila Thrust (BT) and Upper Main Boundary Thrust (U.MBT). Pyrolysis analysis of the CM together with the Fission Track ages from upper Siwaliks corroborates the RSCM thermometry estimate of ~240 °C. The results indicate that the Permian sequence north of Lower MBT was deposited at greater depths (>12 km) than the upper Siwalik sediments to its south at depths <8 km before they were exhumed. The ⁴⁰Ar/³⁹Ar ages suggest that the upper zones of Se La evolved ~13–15 Ma. The middle zone exhumed at ~11 Ma and lower zone close to ~8 Ma indicating erosional unroofing of the MCT sheet. The footwall of MCTZ cooled between 6 and 8 Ma. Analyses of P–T path imply that LHS between MCT and U.MBT zone falls within the kyanite stability field with near isobaric condition. At higher structural level, the temperatures increase gradually with P–T conditions in the sillimanite stability field. The near isothermal (700–800 °C) condition in the GHS, isobaric condition in the MCTZ together with T–t path evidence of GHS that experienced relatively longer duration of near peak temperatures and rapid cooling towards MCTZ, compares the evolution of GHS and inverted metamorphic gradient closely to channel flow predictions.     

攀西三个镁铁-超镁铁质岩体的地球化学及其对源区的约束

在峨眉山大火成岩省的攀西地区的南北向断裂带内分布着一系列层状镁铁-超镁铁质岩体,它们在时空上与峨眉山玄武岩有着密切的联系,代表了岩浆管道系统.本文选择了3个代表性岩体,含钒钛磁铁矿的攀枝花岩体,含铜镍硫化物矿床的力马河岩体以及同时舍钒钛磁铁矿和铜镍硫化物铂族元素矿床的新街岩体进行了主要元素、微量元素和Sr-Nd同位素地球化学研究.总体上新街岩体在地球化学特征上均介于攀枝花岩体和力马河岩体之同.在主要元素特征上,攀枝花岩体相对富Fe、Ti、Ca、Al,而力马河岩体则相对富Mg.3个岩体的稀土和微量元素标准化由线均与丽江苦橄岩相似,均显示出LREE和LILE的相对富集,但是力马河岩体有明显的负Nb、Ta和Ti异常,反映了源区有地壳物质或岩石圈地幔的混染.在log(Th/Yb)PM vs. log(Ta/Th)PM图解上,3个岩体昱示出线性关系,其中攀枝花岩体具有高的(Ta/Th)PM和低的(Th/Yb)PM值,而力马河岩体则显示出相反的特征,并且该图解也暗示了攀枝花岩体有岩石圈地幔的混染,力马河岩体有上地壳物质的混染,而新街岩体则有下地壳物质的混染.在Sr-Nd同位素特征上,3个岩体也有明显的区别,其中新街岩体具有较均一的(87Sr/86Sr)t(0.70610～0.70636)和εNd(t)值(1.01 to 1.75),力马河岩体则具有高的(87Sr/86 Sr).(0.70631～0.70930)和低的εNd(t)值(-0.85 to -4.13),而攀枝花岩体则与丽江苦橄岩的Sr-Nd同位素组成(0.70434～0.70510,1.1～3.2)相似.然而,3个岩体的Sr-Nd同位素成分(除力马河岩体部分样品外)均落在峨眉山玄武岩和洋岛玄武岩(OIB)内,因此这3个岩体可能均来自于地幔柱,但地幔柱熔体在上升过程中受到了不同物质的混染,其中,攀枝花岩体的源区为地幔柱和岩石?圈地幔,新街岩体为地幔柱和下地壳,而力马河岩体则为地幔柱和上地壳,其源区的特征可能反映了地幔柱熔体的演化过程.     

Decompressional coronas and symplectites in granulites of the Musgrave Complex, central Australia

Abstract In granulite facies metapelitic rocks in the Musgrave Complex, central Australia, reaction between S1 garnet and sillimanite involves the development in S2 of both garnet + cordierite + hercynitic spinel + biotite and hercynitic spinel + cordierite + sillimanite + biotite. The S2 assemblages occur either in coronas and symplectites, mainly around garnet, or, in rocks in which S2 is more strongly developed, as recrystallized assemblages. Ignoring the presence of biotite and ilmenite, the mineral textures can be accounted for qualitatively by a consideration of the model system FeO-MgO-Al₂O₃-SiO₂ (FMAS); the textural relationships accord with decompression accompanying the change from S1 to S2. However, since biotite and ilmenite are involved in the assemblages, the parageneses are better accounted for in terms of equilibria in the expanded model system K₂O-FeO-MgO-Al₂O₃-SiO₂-H₂-TiO₂-Fe₂O₃ (KFMASHTO), i.e. AFM + TiO₂+ Fe₂O₃. The coronas reflect the tectonic unroofing of at least part of the Musgrave Complex from peak S1 conditions of about 8 kbar to S2 conditions of about 4 kbar.     

Evolution of coronas in Norwegian anorthosites: re-evaluation based on crystal-chemistry and microstructures

Coarse grained garnet-pyroxene coronas in anorthositic gabbros of the Bergen and Sognefjord areas preserve relics of two stages of reaction during cooling from magmatic T: (1) ol + plagcpx I+ opxI + spn; (2) cpxI + opxI + spn + plagcpxII + opxII + gnt.Geothermobarometry on the products of reaction (1), using Fe³⁺ cpx and Al^IV opx values derived by X-ray structure refinement (XRef), yields T=900–950° C, P=10–11 kb. Even higher T, probably at lower P, is inferred for reaction (2); this is consistent with TEM observations of pigeonite lamellae in cpxI.Transmission electron microscopy (TEM) observations show abundant submicroscopic amphibole lamellae in cpxII, and XRef analyses of coexisting massive amphiboles suggest incomplete occupancy of the H site; both observations suggest low but finite during granulite-facies metamorphism. TEM observations also show that later (retrograde) hydration, particularly of orthopyroxenes, is more extensive than suggested by petrographic studies. Late amphiboles have fully occupied H sites, indicating higher . The integration of XRef and TEM studies with more conventional petrographic and electron microprobe (EMP) data, as in this study, gives a powerful tool for the study of metamorphic reactions.     

Thermal waters of the Hornonitrianska kotlina depression and their utilization

 Slovakia has many areas rich in thermal waters one of which is the Hornonitrianska kotlina depression. At four localities three types of waters are found. The first belongs to the Ca–Mg–HCO₃ type with T.D.S. 0.7 g/l, the second to the Ca–Mg–SO₄ type with T.D.S. 1.37–2.01 g/l and the third to the Ca–Mg–SO₄–HCO₃ type with T.D.S. 0.97 g/l. Discharge at individual localities varies up to 30 l/s and temperatures of water reach 32.5–66.6  °C. The waters are predominantly used for healing, rehabilitation purposes, recreation and heating. Received: 8 March 1999 · Accepted: 7 June 1999     

准噶尔北部蛇绿岩形成时限新证据及其东、西准噶尔蛇绿岩的对比研究

准噶尔北部出露有塔尔巴哈台库吉拜蛇绿岩、洪古勒楞-和布克赛尔蛇绿岩及扎河坝-阿尔曼太蛇绿岩。洪古勒楞蛇绿岩中的堆晶辉长岩样品进行SHRIMP U-Pb定年,结果为472±8.4Ma(MSWD=1.4),限定洪古勒楞-和布克赛尔蛇绿岩形成于早奥陶世。对扎河坝蛇绿岩中斜长花岗岩采用SHRIMP U-Pb方法测定年龄为495.9±5.5Ma(MSWD=2.7),证实扎河坝蛇绿岩形成于晚寒武世-早奥陶世。塔尔巴哈台蛇绿岩、和布克赛尔-洪古勒楞蛇绿岩以及扎河坝-阿尔曼太蛇绿岩均在早奥陶世已经形成,大部分以断层侵位的形式侵位于泥盆纪-石炭系火山-沉积地层中。准噶尔北部东西三段蛇绿岩在形成时代、区域地质以及地球物理特征等方面具有可对比性,认为它们构成一条贯穿东、西准噶尔的蛇绿岩带,这为新疆北部及邻区古生代构造格局的重建以及区域构造的对比连接提供了重要信息。