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21.
《Chinese Astronomy and Astrophysics》2020,44(1):61-69
Carbon-enhanced metal-poor (CEMP) stars are considered to be related to the first generation of stars, and responsible for the chemical evolution of the early Galaxy. More than half of them are in binaries, and could be explained by the binary evolution, but the formation channel of them is still not fully understood. Among the hundreds of CEMP stars, there are nine CEMP RR Lyrae stars identified, and at least seven of which are very likely not binaries. The usual binary star evolution channel is difficult to produce such a single star, particularly that of carbon enrichment. One way in which such a single star might be produced is the merger of a helium white dwarf with a Hertzsprung gap (HG) star. We use a stellar evolution program to calculate the models of the merger remnants, and find that the models can reproduce the observed distribution of these CEMP single RR Lyrae stars in terms of surface temperature, gravity, and carbon abundance. Hence, it is extremely possible that the helium white dwarf and HG star merger model is one of the formation channels of the metal-poor carbon-rich RR Lyrae stars. 相似文献
22.
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
23.
We give the results of photographic observations of the recurrent nova WZ Sge during its 1978 outburst, between December 5 and 25, using the
double astrograph of Beijing Observatory. We discuss the observed properties and calculate the total energy released during the outburst to be about 1.07 (+40) erg. We estimate that the next outburst will occur around the year 2011. 相似文献
24.
T.C. Teixeira J. Christensen-Dalsgaard F. Carrier C. Aerts S. Frandsen D. Stello T. Maas M. Burnet H. Bruntt J.R. de Medeiros F. Bouchy H. Kjeldsen F. Pijpers 《Astrophysics and Space Science》2003,284(1):233-236
This work reports the discovery of solar-type oscillations in thegiant star Hydrae. 相似文献
25.
We present the first diffraction-limited K-band image of the Red Rectangle with 76 mas resolution, an H-band image with 75 mas resolution, and an RG 715 filter image ( 800 nm wavelength) with 78 mas resolution (corresponding to 25 AU for a distance of 330 pc). The H and K images were reconstructed from 6 m telescope speckle data and the RG 715 image from 2.2 m telescope data using the speckle masking bispectrum method. At all wavelengths the images show a compact, highly symmetric bipolar nebula, suggesting a toroidal density distribution of the circumstellar material. No direct light from the central binary can be seen as it is obscured by a dust disk or circumbinary torus. Our first high-resolution H−K color image of the nebula shows a broad red plateau of H−K≈ 2m in the bright inner regions.The optical and near-infrared images and the available photometric continuum observations in a wide range of ultraviolet to centimeter wavelengths enabled us to model the Red Rectangle in detail using a two-dimensional radiative transfer code. Our model matches both the high-resolution images and the spectral energy distribution of this object very well, making the following picture much more certain. The central close binary system with a total luminosity of 3000 L is embedded in a very dense, compact circumbinary torus which has an average number density nH ≈5×1012 cm−3, an outer radius of the dense inner region of R≈30 AU (91 mas), and a ρ∝r−2 density distribution. The full opening angle of the bipolar outflow cavities in our model is 70°. By comparing the observed and theoretical images, we derived an inclination angle of the torus to the line of sight of 7°±1°.The radiative transfer calculations show that the dust properties in the Red Rectangle are spatially inhomogeneous. The modeling confirms that the idea of large grains in the long-lived disk around the Red Rectangle (Jura et al., 1997 [ApJ, 474, 741]) is quantitatively consistent with the observations. In our models, unusually large, approximately millimeter-sized grains dominate the emission of the compact, massive torus. Models with smaller average grain sizes can possibly be found in future studies, for instance, if it turns out that the radio spectrum is not mainly caused by continuum dust emission. Therefore, the large grains suggested by our models require further confirmation by both new observations and radiative transfer calculations. Assuming a dust-to-gas ratio ρd/ρg of 0.005, the dense torus mass is 0.25 M. The model gives a lower limit of 0.0018 M, for the mass of the large particles, which produce a gray extinction of A≈ 28m, towards the center. A much smaller mass of submicron-sized dust grains is presumably located in the polar outflow cavities, their conical surface layers, and in the outer low-density parts of the torus (where ρ∝r−4, in the region of 30 AUr 2000 AU corresponding to 0.′′09–6′′). 相似文献
26.
Armando Manzali Andrea De Luca Patrizia A. Caraveo 《Astrophysics and Space Science》2007,308(1-4):601-605
We report on our analysis of two XMM-Newton observations of the Vela pulsar performed in December 2000 (total exposure time:
96.5 ks). We succeeded in resolving the pulsar spectrum from the surrounding bright nebular emission taking advantage both
of the accurate calibration of the EPIC point spread function and of the Chandra/HRC surface brightness map of the nebula.
This made it possible to assess to pulsar spectral shape disentangling its thermal and non-thermal components. Exploiting
the photon harvest, we have also been able to perform a phase-resolved study of the pulsar emission.
相似文献
27.
David J. Ampleford Andrea Ciardi Sergey V. Lebedev Simon N. Bland Simon C. Bott Jeremy P. Chittenden Gareth N. Hall Adam Frank Eric Blackman 《Astrophysics and Space Science》2007,307(1-3):29-34
We present experimental data on the steady state deflection of a highly supersonic jet by a side-wind in the laboratory. The
use of a long interaction region enables internal shocks to fully cross the jet, leading to the development of significantly
more structure in the jet than in previous work with a similar setup (Lebedev et al., 2004). The ability to control the length
of the interaction region in the laboratory allows the switch between a regime representing a clumpy jet or wind and a regime
similar to a slowly varying mass loss rate. The results indicate that multiple internal oblique shocks develop in the jet
and the possible formation of a second working surface as the jet attempts to tunnel through the ambient medium. 相似文献
28.
Accretion disks orbiting black holes power high-energy systems such as X-ray binaries and Active Galactic Nuclei. Observations
are providing increasingly detailed quantitative information about such systems. This data has been interpreted using standard
toy-models that rely on simplifying assumptions such as regular flow geometry and a parameterized stress. Global numerical
simulations offer a way to investigate the basic physical dynamics of accretion flows without these assumptions and, in principle,
lead to a genuinely predictive theory. In recent years we have developed a fully three-dimensional general relativistic magnetohydrodynamic
simulation code that evolves time-dependent inflows into Kerr black holes. Although the resulting global simulations of black
hole accretion are still somewhat simplified, they have brought to light a number of interesting results. These include the
formation of electro-magnetically dominated jets powered by the black hole’s rotation, and the presence of strong stresses
in the plunging region of the accretion flow. The observational consequences of these features are gradually being examined.
Increasing computer power and increasingly sophisticated algorithms promise a bright future for the computational approach
to black hole accretion. 相似文献
29.
Lorenzo Iorio 《Astrophysics and Space Science》2007,310(1-2):73-76
In this paper we dynamically determine the quadrupole mass moment Q of the magnetic white dwarf WD 0137-349 by looking for deviations from the third Kepler law induced by Q in the orbital period of the recently discovered brown dwarf moving around it in a close 2-hr orbit. It turns out that a
purely Newtonian model for the orbit of WD 0137-349B, assumed circular and equatorial, is adequate, given the present-day
accuracy in knowing the orbital parameters of such a binary system. Our result is Q=(−1.5±0.9)×1047 kg m2 for i=35 deg. It is able to accommodate the 3-sigma significant discrepancy of (1.0±0.3)×10−8 s−2 between the inverse square of the phenomenologically determined orbital period and the inverse square of the calculated Keplerian
one. The impact of i, for which an interval Δ
i of possible values close to 35 deg is considered, is investigated as well. 相似文献
30.
Axel D. Schwope Valeri Hambaryan Frank Haberl Christian Motch 《Astrophysics and Space Science》2007,308(1-4):619-623
We present a first analysis of a deep X-ray spectrum of the isolated neutron star RBS1223 obtained with XMM-Newton. Spectral
data from four new monitoring observations in 2005/2006 were combined with archival observations obtained in 2003 and 2004
to form a spin-phase averaged spectrum containing 290 000 EPIC-pn photons. This spectrum shows higher complexity than its
predecessors, and can be parameterised with two Gaussian absorption lines superimposed on a blackbody. The line centers, E
2≃2E
1, could be regarded as supporting the cyclotron interpretation of the absorption features in a field B∼4×1013 G. The flux ratio of those lines does not support this interpretation. Hence, either feature might be of truly atomic origin.
相似文献