共查询到20条相似文献，搜索用时 625 毫秒
1.
This paper describes a method for analyzing observations of the passage of a star through a gravitational lensing caustic that enables the derivation of information about the brightness distribution across the stellar disk without knowledge of the lens parameters. The ill-posed inverse problem of reconstructing a one-dimensional strip brightness distribution across the stellar disk is solved using a regularization method, taking into account the non-negative nature of this function. Assuming the source is circularly symmetric, the search for the radial brightness distribution is carried out over compact sets of upward-convex, non-negative functions or functions that do not grow with distance from the stellar center. The method is used to analyze the gravitational microlensing event MACHO 98-SMC-1, of a star in the Small Magellanic Cloud, obtained by the PLANET international group. The resulting brightness distribution is compared with computations of limb darkening for model stellar atmospheres. 相似文献
2.
We consider microlensing of stars by a spacetime tunnel (wormhole), which is manifest as a gravitational lens with negative mass and a circular caustic in the source plane. If a source with a small angular size does not cross the circular caustic, it is impossible to discriminate between gravitational lenses with positive and negative mass. Even for comparatively large stellar angular diameters, differences from a Schwarzschild lensing curve are on the order of the observational errors. When the angular size of a star is comparable to the radius of the Einstein cone, for a sufficiently large impact parameter, the shape of the observed light curves can be similar to that due to microlensing of a compact object surrounded by an extended gaseous envelope. Such an object can be easily distinguished from a negative-mass gravitational lens via analysis of chromatic and polarization effects of the lensing. 相似文献
3.
Using a model-independent technique, we have reconstructed a one-dimensional strip distribution of the brightness over a stellar disk from observations of microlensing of a Galactic bulge star by a caustic of the binary gravitational lens OGLE-1999-BUL-23, obtained by the international PLANET group. The ill-posed inverse problem was solved using a regularization method taking into account the non-negativity of the brightness distribution. The radial brightness distribution was searched for on a compact set of convex-upward, monotonically non-increasing, non-negative functions, assuming that the source is circularly symmetrical. The reconstructed brightness distribution is compared with the results of model fitting and limb-darkening calculations based on models of stellar atmospheres. 相似文献
4.
We present an analysis of a high-amplitude event in the flux curve of component A of the gravitational lens QSO 2237+0305 observed by the OGLE and GLITP groups in autumn 1999. Hypothesizing this event to be associated with microlensing of a fold caustic, we analyzed the observational data using a method for the successive reconstruction of branches of the one-dimensional strip brightness distribution across the source corresponding to positive and negative arguments. The search for the branches was carried out on compact sets of nonnegative, monotonically nonincreasing, convex downward functions. The resulting shape of the strip brightness distribution for the accretion disk of the quasar is in agreement with results obtained earlier via model fitting. Features in the lensing curve that could be associated with curvature of the caustic, nearness of a cusp, or the influence of nearby caustics are noted. 相似文献
5.
A. F. Zakharov 《Astronomy Reports》2006,50(2):79-90
Gravitational lensing is a powerful tool for studies of the distribution of matter (including dark matter) in the Universe. The characteristic angular separation of images and characteristic variability time scale depend on the characteristic masses of the gravitational lenses. The construction of the RADIOASTRON space interferometer in the coming years will provide qualitatively new conditions for investigations of microlensing of distant quasars in the radio, since it will become possible not only to resolve individual microimages of these quasars, but also to observe astrometric microlensing (i.e., the shift of an image of a distant quasar, sometimes called weak microlensing). Astrometric microlensing by compact objects in the Galactic halo is not a very significant effect for the RADIOASTRON interferometer, since the probability of such events is low and the characteristic time scales involved appreciably exceed the proposed operational lifetime of the interferometer. 相似文献
6.
M. B. Bogdanov 《Astronomy Reports》2001,45(12):929-934
In the process of their evolution, small-scale clusters of weakly interacting massive particles (WIMPs) that formed in the early Universe can acquire rotational momentum and spheroidal shape. Even small oblateness of a cluster similar to that of the critical Roche surface can lead to the appearance of caustics in the plane of a source lensed by the object. The multiple source images that form in this case cannot be resolved in modern observations, and the cluster behaves like a noncompact spheroidal lens. The caustic crossing that occurs in the case of relative motion of the observer, the cluster of particles, and the lensed star can produce a large variety of flux curves, including those such as have been observed during microlensing events and interpreted as manifestations of binary gravitational lenses. Therefore, we cannot rule out the possibility that at least some of these events might actually be associated with clusters of WIMPs. 相似文献
7.
E. A. Koptelova B. P. Artamonov V. V. Bruevich O. A. Burkhonov A. V. Sergeev 《Astronomy Reports》2008,52(4):270-277
Results of VRI photometry of two components of the gravitationally lensed quasar UM 673 in 2003–2005 are presented. The observational data were obtained on the 1.5-m telescope of the Maidanak observatory. During the monitoring of the system, considerable brightness variations in components A and B with amplitudes of about 0.2 m were recorded, demonstrating variability of the quasar. The increase in the brightness of the components was accompanied by reddening of their V-R color indices. Analysis of the brightness and color variations of the components shows no variations related to microlensing. 相似文献
8.
9.
V. N. Shalyapin 《Astronomy Reports》2006,50(9):699-707
A procedure for calculating two-dimensional power spectra of microlensing magnification fields is presented. In the absence of a shift, the one-dimensional projections of the power spectra P(k) corresponding to the light curve of a point source moving in a linear trajectory can be approximated by the expression (a 2 + k 2)?1/2 (where a = const). The power spectrum of an extended source is treated like the product of the power spectrum of a point source and the power spectrum of the brightness distribution of the extended source. The effect of the extent of the source is that it acts like a filter, suppressing high-frequency components in the spectrum. Based on eight years of monitoring of the quad gravitational lens Q2237+0305 by the OGLE group, power spectra for all four images are constructed and the (temporal) size of the radiating region of the quasar in the V filter is estimated to be 24 ± 6 days; given the constraints on the transverse velocity of the lensing galaxy (<600 km/s), the linear size turns out to be <1015 cm. 相似文献
10.
I. M. Selim Afaf M. Abd El-Hameed N. S. Bakhtigaraev Gamal F. Attia 《Astronomy Reports》2016,60(3):374-388
Variations of light curves for space objects are investigated. Optical observations and photometric measurements for small space debris on highly elliptical orbits (HEO) and geostationary orbits (GEO) are used to determine their orbital parameters. Light curves of small space debris with various area-to-mass ratios and orbital characteristics are discussed. Tracking of some objects shows very rapid brightness variations related to perturbations of the orbital parameters. Changes in brightness and equatorial coordinates of the studied objects are found in observational data. Our results allow improving the accuracy of space debris orbital elements. 相似文献
11.
V. V. Shimansky N. V. Borisov D. N. Nurtdinova A. A. Mitrofanova V. V. Vlasyuk O. I. Spiridonova 《Astronomy Reports》2012,56(6):441-455
We have analyzed the physical status of the pre-cataclysmic variables SDSSJ172406+562003 and RE J2013+4002, which have evolved after their common-envelope stage a time t = 106?107 years. Spectroscopy and photometry of these systems were performed with the 6-m and 1-m telescopes of the Special Astrophysical Observatory. We demonstrate that emission lines in the spectra were formed solely by the reflection of radiation emitted by the white dwarfs on the surfaces of their cool companions, under conditions close to local thermodynamic equilibrium. These effects are also responsible for most of the objects?? photometric variability amplitude. However, comparing the light curves of SDSS 172406 from different epochs, we find aperiodic brightness variations, probably due to spottedness of the surface of the secondary. Jointly analyzing the spectra, radial-velocity curves, and light curves of the pre-cataclysmic variables and modeling the reflection effects, we have derived their fundamental parameters. We demonstrate that the secondaries in these systems are consistent with evolutionary models for main-sequence stars and do not have the luminosity excesses characteristic of cool stars in young pre-cataclysmic variables. 相似文献
12.
A technique is proposed for the successive reconstruction of the branches of the strip brightness distribution for a quasar accretion disk via the analysis of observations of high magnification flux events in the multiple quasar images produced by a gravitational lens. The distribution branches are searched for on compact sets of nonnegative, monotonically nonincreasing, convex downward functions. The results of numerical simulations and application of the technique to real observations show that the solution obtained is stable against random noise. Analysis of the light curve of a high magnification event in image C of the gravitational lens QSO 2237+0305 observed by the OGLE group in summer 1999 has yielded the form of the strip brightness distribution in the accretion disk of the lensed quasar. The results are consistent with the hypothesis that the quasar disk was scanned by a fold caustic. The form of the strip distribution is consistent with the expected appearance of an accretion disk rotating around a supermassive black hole. 相似文献
13.
The effect of weak microlensing on the apparent velocities of extragalactic sources is considered; in particular, the apparent
motions of sources from the ICRF list are discussed. We expect from two to seven cases of apparent motions of extragalactic
sources due to weak microlensing by stars or dark bodies in our Galaxy to be detected over the next 30 years. 相似文献
14.
A. A. Shatskii 《Astronomy Reports》2004,48(7):525-533
It is shown that Einstein-Rosen bridges (wormholes)—hypothetical objects that topologically connect separate locations in the Universe—can be static solutions of the Einstein equations. The corresponding equations for bridges are reduced to a form convenient for their analysis and numerical solution. The matter forming the bridge must have a sufficiently hard and anisotropic equation of state. Our results are compared with a previously known analytic solution for a bridge, which is a special case of the general solution in the framework of general relativity. The deflection of photons by the bridge (gravitational lensing) is studied. 相似文献
15.
A statistical study of motions of images of distant extragalactic sources, such as quasars on the celestial sphere, due to
the action of weak gravitational microlensing is presented. It was assumed that the parallax of the lens was 10 milliarcseconds
(mas), the mass of the lens was 1 M
⊙, and the proper motion was μ = 30 mas. The initial point for the motion of the lens (a star in our Galaxy) was taken to be
the boundary of a region with a radius of ϑ = 100 mas and its center coincident with the distant source. The simulations for
each trajectory were carried out in steps, with the time step being 0.1 year. The number of sources “launched” over the computational
period was 5000. The appearance of the trajectories for the source images is presented; 57% of the total number of sources
that participated in the simulations showed motions of 0.7–1.0 mas.
Original Russian Text ? T.A. Kalinina, M.S. Pshirkov, 2006, published in Astronomicheskiĭ Zhurnal, 2006, Vol. 83, No. 6, pp.
483–488. 相似文献
16.
17.
V. N. Rudenko 《Astronomy Reports》2001,45(12):984-994
The detection of gravitational radiation from relativistic objects in the Universe is discussed. Modern programs designed to search for such signals based on current astrophysical concepts about the nature of the sources are considered. A comparative analysis indicates that available gravitational-wave detectors, whose sensitivity to metric perturbations is on the order of 10?21, are unlikely to be able to detect cosmic gravitational waves. However, the detector sensitivity can be increased using a multichannel method to search for astro-gravitational correlations, in which the noise background of the gravitational-wave detectors is analyzed in parallel with data from neutrino and gamma-ray detectors. 相似文献
18.
We consider the main population of cosmic voids in a heirarchical clustering model. Based on the Press-Schechter formalism modified for regions in the Universe with reduced or enhanced matter densities, we construct the mass functions for gravitationally bound objects of dark matter occupying voids or superclusters. We show that the halo mass functions in voids and superclusters differ substantially. In particular, the spatial density of massive (M ～ 1012 M ⊙) halos is appreciably lower in voids than in superclusters, with the difference in the mass functions being greater for larger masses. According to our computations, an appreciable fraction of the mass of matter in voids should be preserved to the present epoch in the form of primordial gravitationally bound objects (POs) with modest masses (to 10% for M PO < 109 M ⊙) keeping baryons. These primordial objects represent “primary blocks” in the heirarchical clustering model. We argue that the oldest globular clusters in the central regions of massive galaxies are the stellar remnants of these primordial objects: they can form in molecular clouds in these objects, only later being captured in the central regions of massive galaxies in the process of gravitational clustering. Primordial objects in voids can be observed as weak dwarf galaxies or Lyα absorption systems. 相似文献
19.
N. S. Kardashev 《Astronomy Reports》2000,44(11):719-724
Relations enabling estimation of the limiting brightness temperature of synchrotron radiation subject to self-absorption and inverse Compton scattering are presented for the case of relativistic electrons (positrons) and protons. Analogous expressions are presented for relativistic particles moving along curved magnetic lines of force (curvature radiation) and coherent radiation by relativistic particles. These relations can be used to determine the brightness temperatures expected for the central regions of active galactic nuclei, neutron stars, and other objects that produce relativistic particles. Radiation by relativistic protons yields higher intensities, and could be a source of the highest-energy cosmic rays. 相似文献
20.
G. Fodor 《Astronomy Reports》2018,62(12):874-881
Geons are localized horizonless objects formed by gravitational waves, held together by the gravitational attraction of their own field energy. In many respects they are similar to scalar field pulson/oscillon configurations, which were found numerically in 1976 by Kudryavtsev, Bogolyubskii, and Makhankov. If there is a negative cosmological constant, the spacetime of geons asymptotically approaches the anti-de Sitter (AdS) metric. AdS geons are time-periodic regular localized vacuum solutions without any radiation loss at infinity. A higher order perturbative construction in terms of an amplitude parameter shows that there are one-parameter families of AdS geon solutions emerging from combinations of identical-frequency linear modes of the system. 相似文献