共查询到20条相似文献,搜索用时 15 毫秒
1.
We present JHKLM photometry of the carbon stars ST And and T Lyn acquired in 2000–2010. Along with brightness variations due to pulsations,
changes on timescales of 2000–3000 days are also observed. Our combined light curves can be satisfactorily represented with
light elements derived from visual observations, but the maxima are delayed relative to the calculated times. A color-index
analysis demonstrates that the dust shell of ST And is fairly weak, and is manifest only episodically, while the presence
of hot dust was always detected for T Lyn. These results confirm models of spherically symmetric stellar dust shells based
on mean-flux data, supplemented with observations in the intermediate IR from the IRAS and AKARI satellites. The visual optical
depth of the relatively cool dust shell of ST And assuming a dust temperature at the inner edge of T
1 = 510 K is very low: τ
V = 0.047. The dust shell of T Lyn is considerably hotter (T
1 = 940 K), with τ
V = 0.95. We estimate the mass-loss rate to be 1.8 × 10−7
M
⊙/year for ST And and 3.7 × 10−7
M
⊙/year for T Lyn. 相似文献
2.
E. P. Kurbatov 《Astronomy Reports》2010,54(7):590-598
The ejection of stars from spheroidal and disk dwarf galaxies resulting from the decay of OB associations is studied. This
has substantial observational consequences for disk galaxies with escape velocities up to 20 km/s, or dynamical masses up
to 108
M
⊙. The ejection of stars can (i) reduce the abundances of the products of Type Ia supernovae and, to a lesser degree, Type
II supernovae, in disk stars, (ii) chemically enrich the galactic halo and intergalactic medium, (iii) lead to the loss of
50% of the stellar mass in galaxies with masses ∼107
M
⊙ and the loss of all stars in systems with masses ≲105
M
⊙, (iv) increase the mass-to-luminosity ratio of the galaxy. 相似文献
3.
Results of JHKLM photometry for the protoplanetary nebula candidate V1027 Cyg obtained in 1991–2008 are reported. In all bands, the brightness
variations did not exceed 0.2
m
. Estimated linear trends demonstrate no significant changes in the mean brightness and color indices of the object, with
the possible exception of the L-M color index, which showed a small decrease. A search for possible periodicities in the brightness variations yielded the
most probable period of 237d. A model for a spherically-symmetric dust shell has been calculated based on the photometric results supplemented with data
on the mid- and far-infrared fluxes. The estimated mass-loss rate of the star is 1.3 × 10−5
M
⊙/year. 相似文献
4.
We present images of the star-forming regionG23.01–0.41 at 6.7GHz in the Class II methanol maser transition 51–60
A
+, produced from archival observations on the European VLBI Network. Our map of the source and its maser spots contains 24
maser components. The data for each spot—absolute coordinates, coordinates relative to the calibration feature, peak flux
and flux integrated over the spot, size, position angle, velocity along the line of sight, and line full width at half-maximum—are
collected in tabular form. The spatial region occupied by the maser spots is approximated by a 200×130 milliarcsec ellipse
in position angle PA = −0.40°, centered on the absolute coordinates α
0 = 18h34m40.282s, δ
0 = −09°00′38.27″ (J2000). If the source is a protoplanetary disk, then, for the distance estimate derived from trigonometric
parallax, its diameter is 1800 AU, and the mass of the central protostar is 23.5M
⊙. 相似文献
5.
Long-term (1984–2008) JHKLM photometry for 254 objects is presented. The observations were carried out in the standard JHKLM photometric system using an original method and a modern IR photometer designed and built at the Sternberg Astronomical Institute.
Our program of studies included searches for and studies of relatively hot circumstellar dust envelopes. The most important
results obtained using these observations include the following. We have detected relatively hot dust envelopes in a number
of objects for the first time, including the RCB star UV Cas, RX Cas, several classical symbiotic stars, etc. A model has
been calculated for the dust envelope of FG Sge, which formed around the star as a result of several successive cycles of
dust condensation beginning in Autumn 1992. Several dust-condensation episodes have been traced in the envelopes of symbiotic
systems (CH Cyg, V1016 Cyg, HM Sge, etc.), as well as the role of the hot component in the formation of the dust envelopes.
We have established from variations of the IR emission that the cool components in the symbiotic novae V1016 Cyg and HM Sge,
and possibly CH Cyg, are Miras. The binarity of V1016 Cyg and HM Sge has also been firmly established. The variability of
a whole series of object has been studied, including the stellar components of close binary systems and several dozen Mira
and semi-regular variables. The ellipsoidality of the components in the RX Cas system (a prototype W Ser star) and the cool
component in the symbiotic systems CI Cyg and BF Cyg has been firmly established. We have obtained the first IR light curve
for the eclipsing system V444 Cyg (WN5+O6), and determined the wavelength dependence of the obtained parameters of the WN5
star. Analysis of the IR light curves of several novae indicate the condensation of dust envelopes in the transition periods
of Cygnus 1992, Aquila 1993, and Aquila 1995. The IR light curve of R CrB has been obtained over a long period and analyzed.
IR observations of the nova-like variable V4334 Sgr have been carried out over four years, over which the star passed through
four stages during its motion along its post-AGB evolutionary track; the star’s bolometric flux and optical depth of its dust
envelope have been estimated, and the structure and mass of the dust layer determined. We have analyzed the IR variability
of the symbiotic star V407 Cyg over 14 years, and found its cool component to be a Mira with a period of 745 days. The observed
pulsations and trend are associated with the luminosity and temperature variations of the Mira, as well as the optical depth
of the dust envelope. The size of the dust grains and mass-loss rate of the Mira have been determined. We have obtained JHKL light curves for the Seyfert galaxy NGC 4151 over 23 years. The IR brightness of the galaxy grew from 1985 through 1996 (by
∼0.9
m
at 1.25 μm, ∼1
m
at 1.65 μm, ∼1.1
m
at 2.2 μm, and ∼1.3
m
at 3.5 μm), while the galaxy simultaneously reddened. The “cool” variable source in NGC 4151 was still in the active state
in 1998, although its luminosity had decreased by approximately 15%–20%. If the “cool” component of the variable source in
this galaxy is a dust envelope heated by the central “hot” source, it should be optically thin to the radiation of this source:
its mean optical depth is in the range 0.05–0.15. Emission from dust particles heated to temperatures of 600–800 K was observed
in the near IR at a distance of several parsecs from the nucleus during the period of activity in 1995–1998; the inferred
mass of emitting dust was 5–20 M
⊙. In 1994–2003, we observed a tendency for NGC 4151 to become bluer at 1.25–1.65 μm while simultaneously reddening at 2.2–3.5
μm. Beginning in Autumn 2000, the galaxy began to emerge from a minimum, which lasted from March 2000 through April 2001 in
the IR; a flare of the galactic nucleus was observed and followed in detail in the IR in this same period. We confirm the
IR variability of the nucleus of the Seyfert galaxy NGC 1068, which can be located in various stages of activity. The variability
of NGC 1068 is associated with a complex source. A periodic component has been detected in the J brightness variations of the oxygen Mira V2108 Oph; we have shown that this star is immersed in a fairly dense dust envelope,
and have calculated amodel for this envelope. We have calculated an (axially symmetrical) dust-envelope model for the carbon
semi-regular variable RWLMi with a density distribution characteristic for the “superwind” stage. This envelope model is able
to reproduce the observed fluxes over the entire observable spectrum, and displays a good agreement with the observational
data. The three hot supergiants V482 Cas, QZ Sge, and HD 338926 may be variable in the IR. Long-term photometry of eight planetary
nebulae in the near IR (1.25–5 μm) has enabled us to firmly establish the IR brightness and color variability of these nebulae
on time scales from several tens of days to six-to-eight years. We have analyzed long-term JK photometry of the X-ray binary Cyg X-1 (V1357 Cyg). Periodicity with a characteristic time scale of ∼11.5 years is visible
in the JK brightness variations of Cyg X-1 in 1984–2007, possibly due to periodic variations of the temperature, radius and luminosity
of the optical component of the binary with P ∼11.5 yr. Fourteen-year IR light curves of five RV Tau stars (R Sge, RV Tau, AC Her, V Vul, and R Sct) and the yellow supergiant
and protoplanetary-nebula candidate V1027 Cyg have been analyzed. A spherically symmetrical dust-envelope model has been calculated
for V1027 Cyg. 相似文献
6.
Do we have enough pieces of the jigsaw to integrate CO2 fluxes in the coastal ocean? 总被引:1,自引:0,他引:1
Alberto V. Borges 《Estuaries and Coasts》2005,28(1):3-27
Annually integrated air-water CO2 flux data in 44 coastal environments were compiled from literature. Data were gathered in 8 major ecosystems (inner estuaries,
outer estuaries, whole estuarine systems, mangroves, salt marshes, coral reefs, upwelling systems, and open continental shelves),
and up-scaled in the first attempt to integrate air-water CO2 fluxes over the coastal ocean (26×106 km2), taking into account its geographical and ecological diversity. Air-water CO2 fluxes were then up-scaled in global ocean (362×106 km2) using the present estimates for the coastal ocean and those from Takahashi et al. (2002) for the open ocean (336×106 km2). If estuaries and salt marshes are not taken into consideration in the up-scaling, the coastal ocean behaves as a sink for
atmospheric CO2(−1.17 mol C m−2 yr−1) and the uptake of atmospheric CO2 by the global ocean increases by 24% (−1.93 versus −1.56 Pg C yr−1). The inclusion of the coastal ocean increases the estimates of CO2 uptake by the global ocean by 57% for high latitude areas (−0.44 versus −0.28 Pg C yr−1) and by 15% for temperate latitude areas (−2.36 versus −2.06 Pg C yr−1) At subtropical and tropical latitudes, the contribution from the coastal ocean increases the CO2 emission to the atmosphere from the global oceam by 13% (0.87 versus 0.77 Pg C yr−1). If estuaries and salt marshes are taken into consideration in the upscaling, the coastal ocean behaves as a source for
atmospheric CO2 (0.38 mol C m−2 yr−1) and the uptake of atmospheric CO2 from the global ocean decreases by 12% (−1.44 versus −1.56 Pg C yr−1) At high and subtropical and tropical latitudes, the coastal ocean behaves as a source for atmospheric CO2 but at temperate latitudes, it still behaves as a moderate CO2 sink. A rigorous up-scaling of air-water CO2 fluxes in the coastal ocean is hampered by the poorly constrained estimate of the surface area of inner estuaries. The present
estimates clearly indicate the significance of this biogeochemically, highly active region of the biosphere in the global
CO2 cycle. 相似文献
7.
Possible paths for the formation of Ap/Bp stars—massive main-sequence stars with strong magnetic fields—are analyzed based
on modern theories for the evolution of single and binary stars. Assuming that the strong magnetic fields of these stars are
the main reason for their comparatively slow axial rotation and the observed anomalies in the chemical compositions of their
atmospheres, possible origins for these high magnetic fields are considered. Analysis of several possible scenarios for the
formation of these stars leads to the conclusion that their surface magnetic fields are probably generated in the convective
envelopes of the precursor stars. These precursors may be young, single stars with masses 1.5–3 M
⊙ that formed at the peripheries of forming star clusters and ended their accretion at the Hayashi boundary, or alternatively
close binaries whose components have convective envelopes, whose merger leads to the formation of an Ap/Bp star. Arguments
are presented supporting the view that the merger of close binaries is the main channel for the formation of Ap/Bp stars,
and a detailed analysis of this scenario is presented. The initial major axes of the merging binary systems must be in the
range 6–12 R
⊙, and the masses of their components in the range 0.7–1.5 M
⊙. When the merging components possess developed convective envelopes and fairly strong initial magnetic fields, these can
generate powerful magnetic fields “inherited” by the products of the merger—Ap/Bp stars. The reason the components of the
close binaries merge is a loss of angular momentum via the magnetic stellar winds of the components. 相似文献
8.
Rebecca E. Green Thomas S. Bianchi Michael J. Dagg Nan D. Walker Greg A. Breed 《Estuaries and Coasts》2006,29(4):579-597
We investigated seasonal variability in organic carbon (OC) budgets using a physical-biological model for the Mississippi
River turbidity plume. Plume volume was calculated from mixed layer depth and area in each of four salinity subregions based
on an extensive set of cruise data and satellite-derived suspended sediment distributions. These physical measurements were
coupled with an existing food web model to determine seasonally dependent budgets for labile (reactive on time scales of days
to weeks) OC in each salinity subregion. Autochthonous gross primary production (GPP) equaled 1.3×1012 g C yr−1 and dominated labile OC inputs (88% of the budget) because riverine OC was assumed mostly refractory (nonreactive). For perspective,
riverine OC inputs amounted to 3.9×1012 g C yr−1, such that physical inputs were 3 times greater than biological inputs to the plume. Annually, microbial respiration (R)
accounted for 65% of labile OC losses and net metabolism (GPP—R) for the entire plume was, autotrophic, equaling 5.1×1011 g C yr−1. Smaller losses of labile OC occurred via sedimentation (20%), advection (10%), and export to higher trophic levels (5%).
In our present model, annual losses of labile OC are 10% higher than inputs, indicating future improvements are required.
Application of our model to estimate air-sea carbon dioxide (CO2) fluxes indicated the plume was a net sink of 2.0×109 mol CO2 yr−1, of which 90% of the total drawdown was from biotic factors. In all seasons, low salinity waters were a source of CO2 (pCO2=560–890 μatm), and intermediate to high salinity waters were a sink of CO2 (pCO2=200–370 μatm). Our model was also used to calculate O2 demand for the development, of regional hypoxia, and our spring and early summer budgets indicated that sedimentation of
autochthonous OC from the immediate plume contributed 23% of the O2 demand necessary for establishment of hypoxia in the region. 相似文献
9.
The relationship between the masses and metallicities of galaxies could be non-monotonic, due to the outflow of matter in
these systems. It is shown using a simple, one-zone, chemical-dynamicalmodel that the metallicity should be a non-monotonic
function of the mass for spheroidal dwarf galaxies with low masses of M ≤ 108
M
⊙, and a monotonically growing function for galaxies with higher masses. This is consistent with observations. 相似文献
10.
The thermoelastic behaviour of anthophyllite has been determined for a natural crystal with crystal-chemical formula ANa0.01
B(Mg1.30Mn0.57Ca0.09Na0.04) C(Mg4.95Fe0.02Al0.03) T(Si8.00)O22
W(OH)2 using single-crystal X-ray diffraction to 973 K. The best model for fitting the thermal expansion data is that of Berman
(J Petrol 29:445–522, 1988) in which the coefficient of volume thermal expansion varies linearly with T as α
V,T
= a
1 + 2a
2 (T − T
0): α298 = a
1 = 3.40(6) × 10−5 K−1, a
2 = 5.1(1.0) × 10−9 K−2. The corresponding axial thermal expansion coefficients for this linear model are: α
a
,298 = 1.21(2) × 10−5 K−1, a
2,a
= 5.2(4) × 10−9 K−2; α
b
,298 = 9.2(1) × 10−6 K−1, a
2,b
= 7(2) × 10−10 K−2. α
c
,298 = 1.26(3) × 10−5 K−1, a
2,c
= 1.3(6) × 10−9 K−2. The thermoelastic behaviour of anthophyllite differs from that of most monoclinic (C2/m) amphiboles: (a) the ε
1 − ε
2 plane of the unit-strain ellipsoid, which is normal to b in anthophyllite but usually at a high angle to c in monoclinic amphiboles; (b) the strain components are ε
1 ≫ ε
2 > ε
3 in anthophyllite, but ε
1 ~ ε
2 ≫ ε
3 in monoclinic amphiboles. The strain behaviour of anthophyllite is similar to that of synthetic C2/m
ANa B(LiMg) CMg5
TSi8 O22
W(OH)2, suggesting that high contents of small cations at the B-site may be primarily responsible for the much higher thermal expansion
⊥(100). Refined values for site-scattering at M4 decrease from 31.64 epfu at 298 K to 30.81 epfu at 973 K, which couples with similar increases of those of M1 and M2 sites. These changes in site scattering are interpreted in terms of Mn ↔ Mg exchange involving M1,2 ↔ M4, which was first detected at 673 K. 相似文献
11.
Mauro Gemmi Marco Merlini Alessandro Pavese Nadia Curetti 《Physics and Chemistry of Minerals》2008,35(7):367-379
Phengite samples (2M
1 and 3T politypes) and a synthetic end-member muscovite specimen were studied by in situ high-temperature synchrotron radiation X-ray
diffraction. The measured volume thermal expansion of 2M
1 phengite (<α
V> ≈ 36.6 × 10−6 K−1) was systematically greater than <α
V> of the 3T polytype (≈33.3 × 10−6 K−1). A positive linear correlation between the average thermal expansion on (001) plane and the mean tetrahedral rotation angle
at ambient condition is proposed on the ground of new measurements and literature data. Dehydroxylation processes were observed
in 2M
1, starting at 1,000 K in 3T at 800 and 945 K in synthetic muscovite. Rietveld refinements allowed a determination of structural variations upon heating
of phengite samples and their dehydroxylate phases. The phengite structure expands by regularizing the tetrahedral sheet and
by reducing the bond length differences between the outer and inner coordination shell of the interlayer site. The dehydroxylate
phase derived from 2M
1 is characterized by fivefold polyhedra in the low temperature form as a consequence of two OH groups reacting to form H2O + O (residual). The dehydroxylate exhibits an increase of the cation–cation distances along the M–Or–M bonds with respect
to low-temperature phengite structures. For the 3T phase, we were unable to achieve completion of dehydroxylation. The refined structural model of the dehydroxylate phase shows
two hydroxyl sites, but at a short distance from one another. This result suggests that the dehydroxylation reaction did not
proceed to completion.
Electronic supplementary material The online version of this article (doi:) contains supplementary material, which is available to authorized users. 相似文献
12.
P. Comodi G. D. Gatta P. F. Zanazzi D. Levy W. Crichton 《Physics and Chemistry of Minerals》2002,29(8):538-544
Powder diffraction measurements at simultaneous high pressure and temperature on samples of 2M1 polytype of muscovite (Ms) and paragonite (Pg) were performed at the beamline ID30 of ESRF (Grenoble), using the Paris-Edinburgh
cell. The bulk moduli of Ms, calculated from the least-squares fitting of V–P data on each isotherm using a second-order Birch–Murnaghan EoS, were: 57.0(6), 55.1(7), 51.1(7) and 48.9(5) GPa on the isotherms
at 298, 573, 723 and 873 K, respectively. The value of (∂K
T
/∂T)
was −0.0146(2) GPa K−1. The thermal expansion coefficient α varied from 35.7(3) × 10−6 K−1 at P ambient to 20.1(3) × 10−6 K−1 at P = 4 GPa [(∂α/∂P)
T
= −3.9(1) × 10−6 GPa−1 K−1]. The corresponding values for Pg on the isotherms at 298, 723 and 823 K were: bulk moduli 59.9(5), 55.7(6) and 53.8(7) GPa,
(∂K
T
/∂T)
−0.0109(1) GPa K−1. The thermal expansion coefficient α varied from 44.1(2) × 10−6 K−1 at P ambient to 32.5(2) × 10−6 K−1 at P = 4 GPa [(∂α/∂P)
T
= −2.9(1) × 10−6 GPa−1 K−1]. Thermoelastic coefficients showed that Pg is stiffer than Ms; Ms softens more rapidly than Pg upon heating; thermal expansion
is greater and its variation with pressure is smaller in Pg than in Ms.
Received: 28 January 2002 / Accepted: 5 April 2002 相似文献
13.
The results of JHKLM photometry of two carbon stars are presented: the irregular variable NQ Cas and the Mira star BD Vul. Data on the mean fluxes supplemented with mid-IR observations with the IRAS, AKARI, andWISE satellites are used to compute spherically symmetrical model dust envelopes for the stars, consisting of particles of amorphous carbon and silicon carbide. The optical depth in the visible for the comparatively cool dust envelope of BD Vul, with a dust temperature at its inner boundary T1 = 610 K, is fairly low: τV = 0.13. The dust envelope of NQ Cas is appreciably hotter (T1 = 1550 K), and has τV = 0.32. The estimated mass-loss rates are 1.5 × 10?7M⊙/yr for NQ Cas and 5.9 × 10?7M⊙/yr for BD Vul. 相似文献
14.
Data from the revised Geneva-Copenhagen catalog are used to study the influence of radial migration of stars on the age dependences
of parameters of the velocity ellipsoids for nearby stars in the thin disk of the Galaxy, assuming that the mean radii of
the stellar orbits remain constant. It is demonstrated that precisely the radial migration of stars, together with the negative
metallicity gradient in the thin disk, are responsible for the observed negative correlation between the metallicities and
angular momenta of nearby stars, while the angular momenta of stars that were born at the same Galactocentric distances do
not depend on either age or metallicity. The velocity components of the Sun relative to the Local Standard of Rest derived
using data for stars born at the solar Galactocentric distance are (U
⊙, V
⊙, W
⊙)
LSR
= (5.1 ± 0.4, 7.9 ± 0.5, 7.7 ± 0.2) km/s. The two coordinates of the apex of the solar motion remain equal to 〈l
⊙〉 = 70° ± 7° and 〈b
⊙〉 = 41° ± 2°, within the errors. The indices for the power-law age dependences of them ajor, middle, and minor semi-axes become
0.26±0.04, 0.32±0.03, and 0.07±0.03, respectively. As a result, with age, the velocity ellipsoid for thin-disk stars born
at the solar Galactocentric distance increases only in the plane of the disk, remaining virtually constant in the perpendicular
direction. Its shape remains far from equilibrium, and the direction of the major axis does not change with age: the ellipsoid
vertex deviation remains constant and equal to zero within the errors (〈L〉 = 0.7° ± 0.6°, 〈B〉 = 1.9° ± 1.1°). Such a small increase in the velocity dispersion perpendicular to the Galactic plane with age can probably
be explained by “heating” of the stellar system purely by spiral density waves, without a contribution from giant molecular
clouds. 相似文献
15.
The LTE lithium abundances, logN (Li), have been determined for the atmospheres of the four carbon giants AQ And, HK Lyr, UX Dra, and WZ Cas, applying the
synthetic-spectrum technique to the LiI λ670.8 nm resonance doublet. We used estimates of the effective temperatures T
eff, metallicities, elemental abundances, and carbon-isotope ratios for these stars from the literature [12C/13C]. The resulting
lithium abundances depend significantly on the adopted T
eff, so that we can find each star’s range of possible logN(Li) values for a given range of effective temperatures (ΔT
eff = 200−300 K). The uncertainty in the derived logN(Li) values is 1.3 for AQ And and UX Dra, 0.5 for HK Lyr, and 0.8 for WZ Cas. Our most probable logN(Li) values (or ranges) are −1.25 for AQ And, −1.2 for HK Lyr, −1.0 ≤ logN(Li) ≤ +0.3 for UX Dra, and 4.3 ≤ logN(Li) ≤ 4.8 for WZ Cas. The derived C/O ratios for the stellar atmospheres also depend on T
eff. Possible uncertainties in other atmospheric parameters do not change logN(Li) by more than 0.2. 相似文献
16.
The thermal expansion of gehlenite, Ca2Al[AlSiO7], (up to T=830 K), TbCaAl[Al2O7] (up to T=1100 K) and SmCaAl[Al2O7] (up to T=1024 K) has been determined. All compounds are of the melilite structure type with space group
Thermal expansion data were obtained from in situ X-ray powder diffraction experiments in-house and at HASYLAB at the Deutsches
Elektronen Synchrotron (DESY) in Hamburg (Germany). The thermal expansion coefficients for gehlenite were found to be: α1=7.2(4)×10−6×K−1+3.6(7)×10−9ΔT×K−2 and α3=15.0(1)×10−6×K−1. For TbCaAl[Al2O7] the respective values are: α1=7.0(2)×10−6×K−1+2.0(2)×10−9ΔT×K−2 and α3=8.5(2)×10−6×K−1+2.0(3)×10−9ΔT×K−2, and the thermal expansion coefficients for SmCaAl[Al2O7] are: α1=6.9(2)×10−6×K−1+1.7(2)×10−9ΔT×K−2 and α3=9.344(5)×10−6×K−1. The expansion mechanisms of the three compounds are explained in terms of structural trends obtained from Rietveld refinements
of the crystal structures of the compounds against the powder diffraction patterns. No structural phase transitions have been
observed. While gehlenite behaves like a ‘proper’ layer structure, the aluminates show increased framework structure behavior.
This is most probably explained by stronger coulombic interactions between the tetrahedral conformation and the layer-bridging
cations due to the coupled substitution (Ca2++Si4+)–(Ln
3++Al3+) in the melilite-type structure.
This article has been mistakenly published twice. The first and original version of it is available at . 相似文献
17.
The rare-earth element (REE) concentrations of representative granite samples from the southeast of the Obudu Plateau, Nigeria, were analyzed with an attempt to determine the signatures of their source, evolutionary history and tectonic setting. Results indicated that the granites have high absolute REE concentrations (190×10^-6-1191×10^-6; av.=549×10^-6) with the chondrite-normalized REE patterns characterized by steep negative slopes and prominent to slight or no negative Eu anomalies. All the samples are also characterized by high and variable concentrations of the LREE (151×10^-6-1169×10^-6; av.= 466×10^-6), while the HREE show low abundance (4×10^-6-107×10^-6; av.=28×10^-6). These are consistent with the variable levels of REE fractionation, and differentiation of the granites. This is further supported by the range of REE contents, the chondrite-normalized patterns and the ratios of LaN/YbN (2.30-343.37), CeN/YbN (5.94-716.87), LaN/SmN (3.14-11.68) and TbN/YbN (0.58-1.65). The general parallelism of the REE patterns, suggest that all the granites were comagmatic in origin, while the high Eu/Eu* ratios (0.085-2.807; av.=0.9398) indicate high fo2 at the source. Similarly, irregular variations in LaN/YbN, CeN/YbN and Eu/Eu* ratios and REE abundances among the samples suggest behaviors that are related to mantle and crustal sources. 相似文献
18.
The evolution of the components of the unique, massive, close binary system NGC 3603-A1, which consists of stars of spectral
types WN6ha and WN6h, is analyzed. The component masses are estimated to be 116 and 89M
⊙, close to the highest measured stellar masses. Numerical modeling of the evolution of the components has been carried out,
taking into account mass loss via the stellar winds of the two massive stars. It is shown that the maximum possible initial
component masses are close to 140 and 125M
⊙. The components are currently slightly evolved main-sequence stars, with a comparative low degree of helium enrichment at
their surfaces. Further evolution of the system will lead to filling of the Roche lobe of the primary and subsequent evolution
in a common envelope. This may lead to the merger of the components, with the evolution of the system ending in the formation
of a singlemassive black hole after the second supernova explosion. Otherwise, depending on the masses of the resulting black
holes, either a binary system of two black holes or two unbound black holes may form, accompanied by gamma-ray bursts. 相似文献
19.
A. I. Khaliullina 《Astronomy Reports》2016,60(5):517-525
A detailed study of variations of the orbital periods of the Algol-type eclipsing binary systems RZ Cas and Z Dra is presented. The fairly complex variations of the periods of both systems can be represented as a superposition of a secular increase of the period, slow periodic fluctuations, and quasiperiodic oscillations with a small amplitude occurring on timescales of decades. The secular increase of the period can be explained by the steady mass transfer from the less massive to the more massive component with conservation of the total angular momentum. The mass-transfer rate is 5.7 × 10?9M⊙/yr for RZ Cas and 3.0×10?8M⊙/yr for Z Dra. To explain the long-period cyclic variations of the orbital periods of RZCas and Z Dra, it must be assumed that the eclipsing binaries move in long-period orbits. RZ Cas moves with a period of 133 yr around a third body withmass M3 > 0.55M⊙, while Z Dra moves with a period of 60 yr around a third body with mass M3 > 0.7M⊙. The residual fluctuations of the periods may be due to a superposition of variations due to magnetic cycles and non-stationary ejections of matter. 相似文献
20.
The thermal expansion of gehlenite, Ca2Al[AlSiO7], (up to T=830 K), TbCaAl[Al2O7] (up to T=1,100 K) and SmCaAl[Al2O7] (up to T=1,024 K) has been determined. All compounds are of the melilite structure type with space group
Thermal expansion data was obtained from in situ X-ray powder diffraction experiments in-house and at HASYLAB at the Deutsches Elektronen Synchrotron (DESY) in Hamburg (Germany). The thermal expansion coefficients for gehlenite were found to be: α1=7.2(4)×10−6 K−1+3.6(7)×10−9ΔT K−2 and α3=15.0(1)×10−6 K−1. For TbCaAl[Al2O7] the respective values are: α1=7.0(2)×10−6 K−1+2.0(2)×10−9ΔT K−2 and α3=8.5(2)×10−6 K−1+2.0(3)×10−9ΔT K−2, and the thermal expansion coefficients for SmCaAl[Al2O7] are: α1=6.9(2)× 10−6 K−1+1.7(2)×10−9ΔT K−2 and α3=9.344(5)×10−6 K−1. The expansion-mechanisms of the three compounds are explained in terms of structural trends obtained from Rietveld refinements
of the crystal structures of the compounds against the powder diffraction patterns. No structural phase transitions have been
observed. While gehlenite behaves like a ’proper’ layer structure, the aluminates show increased framework structure behaviour.
This is most probably explained by stronger coulombic interactions between the tetrahedral conformation and the layer-bridging
cations due to the coupled substitution (Ca2++Si4+)-(Ln
3++Al3+) in the melilite-type structure.
Electronic Supplementary Material Supplementary material is available for this article at 相似文献