M. Revnivtsev

Russian Academy of Sciences, Moskva, Moscow, Russia

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Publications (265)533.01 Total impact

  • [Show abstract] [Hide abstract]
    ABSTRACT: Neutron star (NS) masses and radii can be estimated from observations of photospheric radius-expansion X-ray bursts, provided the chemical composition of the photosphere, the spectral colour-correction factors in the observed luminosity range, and the emission area during the bursts are known. By analysing 246 X-ray bursts observed by the Rossi X-ray Timing Explorer from 11 low-mass X-ray binaries, we find a dependence between the persistent spectral properties and the time evolution of the black body normalisation during the bursts. All NS atmosphere models predict that the colour-correction factor decreases in the early cooling phase when the luminosity first drops below the limiting Eddington value, leading to a characteristic pattern of variability in the measured blackbody normalisation. However, the model predictions agree with the observations for most bursts occurring in hard, low-luminosity, 'island' spectral states, but rarely during soft, high-luminosity, 'banana' states. The observed behaviour may be attributed to the accretion flow, which influences cooling of the NS preferentially during the soft state bursts. This result implies that only the bursts occurring in the hard, low-luminosity spectral states can be reliably used for NS mass and radius determination.
    06/2014;
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    ABSTRACT: We present results of a study of the fast timing variability of the magnetic cataclysmic variable (mCV) EX Hya. It was previously shown that one may expect the rapid flux variability of mCVs to be smeared out at timescales shorter than the cooling time of hot plasma in the post shock region of the accretion curtain near the WD surface. Estimates of the cooling time and the mass accretion rate, thus provide us with a tool to measure the density of the post-shock plasma and the cross-sectional area of the accretion funnel at the WD surface. We have probed the high frequencies in the aperiodic noise of one of the brightest mCV EX Hya with the help of optical telescopes, namely SALT and the SAAO 1.9m telescope. We place upper limits on the plasma cooling timescale $\tau<$0.3 sec, on the fractional area of the accretion curtain footprint $f<1.6\times10^{-4}$, and a lower limit on the specific mass accretion rate $\dot{M}/A \gtrsim $3 g/sec/cm$^{-2}$. We show that measurements of accretion column footprints via eclipse mapping highly overestimate their areas. We deduce a value of $\Delta r/r \lesssim 10^{-3}$ as an upper limit to the penetration depth of the accretion disc plasma at the boundary of the magnetosphere.
    05/2014; 442(2).
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    M. G. Revnivtsev, E. V. Filippova, V. F. Suleimanov
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    ABSTRACT: We investigate the relation between the optical (g-band) and X-ray (0.5-10 keV) luminosities of accreting nonmagnetic white dwarfs. According to the present-day counts of the populations of star systems in our Galaxy, these systems have the highest space density among the close binary systems with white dwarfs. We show that the dependence of the optical luminosity of accreting white dwarfs on their X-ray luminosity forms a fairly narrow one-parameter curve. The typical half-width of this curve does not exceed 0.2-0.3 dex in optical and X-ray luminosities, which is essentially consistent with the amplitude of the aperiodic flux variability for these objects. At X-ray luminosities Lx~1e32 erg/sec or lower, the optical g-band luminosity of the accretion flow is shown to be related to its X-ray luminosity by a factor ~2-3. At even lower X-ray luminosities (Lx~1e30 erg/sec), the contribution from the photosphere of the white dwarf begins to dominate in the optical spectrum of the binary system and its optical brightness does not drop below Mg~13-14. Using the latter fact, we show that in current and planned X-ray sky surveys, the family of accreting nonmagnetic white dwarfs can be completely identified to the distance determined by the sensitivity of an optical sky survey in this region. For the Sloan Digital Sky Survey (SDSS) with a limiting sensitivity m_g~22.5, this distance is ~400-600 pc
    04/2014; 40(4).
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    ABSTRACT: We present the results of measurements of the total X-ray flux from the Andromeda galaxy (M31) in the 3-100 keV band based on data from the RXTE/PCA, INTEGRAL/ISGRI, and SWIFT/BAT space experiments. We show that the total emission from the galaxy has a multicomponent spectrum whose main characteristics are specified by binaries emitting in the optically thick and optically thin regimes. The galaxy's luminosity at energies 20-100 keV gives about 6% of its total luminosity in the 3-100 keV band. The emissivity of the stellar population in M31 is L 2-20 keV ̃ 1.1 × 1029 erg s-1 M {☉/-1} in the 2-20 keV band and L 20-100 keV ̃ 8 × 1027 erg s-1 M {☉/-1} in the 20-100 keV band. Since low-mass X-ray binaries at high luminosities pass into a soft state with a small fraction of hard X-ray emission, the detection of individual hard X-ray sources in M31 requires a sensitivity that is tens of times better (up to 10-13 erg s-1 cm-2) than is needed to detect the total hard X-ray emission from the entire galaxy. Allowance for the contribution from the hard spectral component of the galaxy changes the galaxy's effective Compton temperature approximately by a factor of 2, from ̃1.1 to ̃2.1 keV.
    Astronomy Letters 12/2013; 40(1). · 0.93 Impact Factor
  • E. Filippova, M. Revnivtsev, E. R. Parkin
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    ABSTRACT: We consider modulations of mass captured by the compact object from the companion star's stellar wind in Low Mass X-ray Binaries with late type giants. Based on 3D simulations with two different hydrodynamic codes used Lagrangian and Eulerian approaches - the SPH code GADGET and the Eulerian code PLUTO, we conclude that a hydrodynamical interaction of the wind matter within a binary system even without eccentricity results in variability of the mass accretion rate with characteristic time-scales close to the orbital period. Observational appearances of this wind might be similar to that of an accretion disc corona/wind.
    12/2013;
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    E. Filippova, M. Revnivtsev, E. R. Parkin
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    ABSTRACT: In this paper we propose and examine a physical mechanism which can lead to the generation of noise in the mass accretion rate of low mass X-ray binaries on time-scales comparable to the orbital period of the system. We consider modulations of mass captured by the compact object from the companion star's stellar wind in binaries with late type giants, systems which usually have long orbital periods. We show that a hydrodynamical interaction of the wind matter within a binary system even without eccentricity results in variability of the mass accretion rate with characteristic time-scales close to the orbital period. The cause of the variability is an undeveloped turbulent motion (perturbed motion without significant vorticity) of wind matter near the compact object. Our conclusions are supported by 3D simulations with two different hydrodynamic codes based on Lagrangian and Eulerian approaches -- the SPH code GADGET and the Eulerian code PLUTO. In this work we assume that the wind mass loss rate of the secondary is at the level of $(0.5-1)\times10^{-7} M_\odot$/year, required to produce observable variations of the mass accretion rate on the primary. This value is higher than that, estimated for single giant stars of this type, but examples of even higher mass loss rate of late type giants in binaries do exist. Our simulations show that the stellar wind matter intercepted by the compact object might create observational appearances similar to that of an accretion disc corona/wind and could be detected via high energy resolution observations of X-ray absorption lines, in particular, highly ionized ions of heavy elements.
    Monthly Notices of the Royal Astronomical Society 10/2013; 437(1). · 5.52 Impact Factor
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    ABSTRACT: Four hard X-ray sources from the INTEGRAL and Swift catalogs have been identified. X-ray and optical spectra have been obtained for each of the objects being studied by using data from the INTEGRAL, Swift, ROSAT, and Chandra X-ray observatories as well as observations with the RTT-150 and AZT-33IK optical telescopes. Two sources (SWIFT J1553.6+2606 and SWIFT J1852.2+8424) are shown to be extragalactic in nature: the first is a quasar, while the registered X-ray flux from the second is the total emission from two Seyfert 1 galaxies at redshifts 0.1828 and 0.2249. The source IGR J22534+6243 resides in our Galaxy and is an X-ray pulsar with a period of ~46.674 s that is a member of a high-mass X-ray binary, probably with a Be star. The nature of yet another Galactic source, SWIFT J1852.8+3002, is not completely clear and infrared spectroscopy is needed to establish it.
    Astronomy Letters 07/2013; 39(8). · 0.93 Impact Factor
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    Mikhail G. Revnivtsev, Valery F. Suleimanov, Juri Poutanen
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    ABSTRACT: Emission of the neutron star surface potentially contains information about its size and thus of vital importance for high energy astrophysics. In spite of the wealth of data on the emission of luminous accreting neutron stars, the emission of their surfaces is hard to disentangle from their time averaged spectra. A recent X-ray transient source XTE J1701-462 has provided a unique dataset covering the largest ever observed luminosity range for a single source. In this paper, we extract the spectrum of the boundary layer between the inner part of the accretion disc and the neutron star surface with the help of maximally spectral model-independent method. We show compelling evidences that the energy spectrum of the boundary layer stays virtually the same over factor of 20 variations of the source luminosity. It is rather wide and cannot be described by a single temperature blackbody spectrum, probably because of the inhomogeneity of the boundary layer and a spread in the colour temperature. The observed maximum colour temperature of the boundary/spreading layer emission of kT~2.4-2.6 keV is very close to the maximum observed colour temperature in the photospheric radius expansion X-ray bursts, which is set by the limiting Eddington flux at the neutron star surface. Observed stability of the boundary layer spectrum and its maximum colour temperature strongly supports theoretical models of the boundary/spreading layers on surfaces of luminous accreting neutron stars, which assume the presence of a region emitting at the local Eddington limit. Variations in the luminosity in that case lead to changes in the size of this region, but affect less the spectral shape. Elaboration of this model will provide solid theoretical grounds for measurements of the neutron star sizes using the emission of the boundary/spreading layers of luminous accreting neutron stars.
    Monthly Notices of the Royal Astronomical Society 06/2013; 434(3). · 5.52 Impact Factor
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    ABSTRACT: A new hard X-ray transient IGR J17446-2948 has been detected in the Galactic Center region by the IBIS/ISGRI telescope on board INTEGRAL during the Galactic Latitude Scan observations performed between March 26th, 09:20 and March 28, 20:02 (UT), 2013. The source is registered at the 6 sigma significance level with the flux 6.5+/-1.0 mCrab (9.3e-11 erg/cm2/s) in the 17-60 keV energy range. It also shows a positive excess at the 3 sigma level (4.5+/-1.3 mCrab or 6.4e-11 erg/cm2/s) in the previous data set taken between March 23th, 05:15 and March 24th, 02:20, 2013.
    The Astronomer's Telegram. 03/2013;
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    ABSTRACT: We present results of the study of persistent high mass X-ray binaries (HMXBs) in the Milky Way, obtained from the deep INTEGRAL Galactic plane survey. This survey provides us a new insight into the population of high mass X-ray binaries because almost half of the whole sample consists of sources discovered with INTEGRAL. It is demonstrated for the first time that the majority of persistent HMXBs have supergiant companions and their luminosity function steepens somewhere around ~2x10^{36} erg/s. We show that the spatial density distribution of HMXBs correlates well with the star formation rate distribution in the Galaxy. The vertical distribution of HMXBs has a scale-height h~85 pc, that is somewhat larger than the distribution of young stars in the Galaxy. We propose a simple toy model, which adequately describes general properties of HMXBs in which neutron stars accrete a matter from the wind of the its companion (wind-fed NS-HMXBs population). Using the elaborated model we argue that a flaring activity of so-called supergiant fast X-ray transients, the recently recognized sub-sample of HMXBs, is likely related with the magnetic arrest of their accretion.
    Monthly Notices of the Royal Astronomical Society 02/2013; 431(1). · 5.52 Impact Factor
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    ABSTRACT: We present the results of Chandra and XMM-Newton observations for six hard X-ray sources (IGR J12134-6015, IGR J18293-1213, IGR J18219-1347, IGR J17350-2045, IGR J18048-1455, XTE J1901+014) from the INTEGRAL all-sky survey. Based on these observations, we have improved significantly the localization accuracy of the objects and, therefore, have managed to identify their optical counterparts. Using data from the publicly available 2MASS and UKIDSS infrared sky surveys as well as data from the SOFI/NTT telescope (European Southern Observatory), we have determined the magnitudes of the optical counterparts, estimated their types and (in some cases) the distances to the program objects. A triplet of iron lines with energies of 6.4, 6.7, and 6.9 keV has been detected in the X-ray spectrum of IGR J18048-1455; together with the detection of pulsations with a period of ~1440 s from this source, this has allowed it to be classified as a cataclysmic variable, most likely an intermediate polar. In addition, broadband X-ray spectra of IGR J12134-6015 and IGR J17350-2045 in combination with infrared and radio observations suggest an extragalactic nature of these objects. The source IGR J18219-1347 presumably belongs to the class of high-mass X-ray binaries.
    Astronomy Letters 09/2012; 38(10). · 0.93 Impact Factor
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    ABSTRACT: MVN (Monitor Vsego Neba) - new small X-ray astronomical experiment, which will be mounted on Russian segment of International Space Station. The main scientific goal for the instrument is the precise measurement of cosmic X-ray background in energy range 6-70 keV, which is important for theories of black hole evolution in the Universe. The ultimate aim of the experiment is to reach the accuracy of the CXB measurements, which will allow us to measure the large scale anisotropy of the Cosmic X-ray Background caused by inhomogeneities of the matter distribution in the local Universe. The MVN instrument is a simple collimated spectrometer, equipped with 4 CdTe pixellated detectors. The field of view of the instrument will be scanning the zenith of the ISS. The accuracy of the instrumental background subtraction, which is the main obstacle for the proposed task, will be provided by a cover, which will periodically block the aperture of detectors. According to our estimates, with not unfavourable radiation environment on orbit of ISS during period of operation of MVN we will be able to measure the CXB surface brightness at different sky directions with accuracy better than 1% after 2 years of the experiment. The planned dates of the experiment is 2013-2016.
    Proc SPIE 09/2012;
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    Solen Balman, Mikhail Revnivtsev
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    ABSTRACT: We show for five DN systems, SS Cyg, VW Hyi, RU Peg, WW Cet and T Leo that the UV and X-ray power spectra of their time variable light curves are similar in quiescence. All of them show a break in their power spectra, which in the framework of the model of propagating fluctuations indicates inner disk truncation. We derive the inner disk radii for these systems in a range (10-3)$\times10^{9}$ cm. We analyze the RXTE data of SS Cyg in outburst and compare it with the power spectra, obtained during the period of quiescence. We show that during the outburst the disk moves towards the white dwarf and recedes as the outburst declines. We calculate the correlation between the simultaneous UV and X-ray light curves of the five DN studied in this work, using the XMM-Newton data obtained in the quiescence and find X-ray time lags of 96-181 sec. This can be explained by the travel time of matter from a truncated inner disk to the white dwarf surface. We suggest that, in general, DN may have truncated accretion disks in quiescence which can also explain the UV and X-ray delays in the outburst stage and that the accretion may occur through coronal flows in the disk (e.g., rotating accretion disk coronae). Within a framework of the model of propagating fluctuations the comparison of the X-ray/UV time lags observed by us in the case of DN systems with those, detected for a magnetic Intermediate Polar allows us to make a rough estimate of the viscosity parameter $\alpha\sim0.25$ in the innermost parts of the accretion flow of DN systems.
    Astronomy and Astrophysics 08/2012; · 5.08 Impact Factor
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    ABSTRACT: We estimate the relative contributions of the supermassive black hole (SMBH) accretion disk, corona, and obscuring torus to the bolometric luminosity of Seyfert galaxies, using Spizter mid-infrared (MIR) observations of a complete sample of 68 nearby active galactic nuclei from the INTEGRAL all-sky hard X-ray (HX) survey. This is the first HX-selected (above 15 keV) sample of AGNs with complementary high angular resolution, high signal to noise, MIR data. Correcting for the host galaxy contribution, we find a correlation between HX and MIR luminosities: L_MIR L_HX^(0.74+/-0.06). Assuming that the observed MIR emission is radiation from an accretion disk reprocessed in a surrounding dusty torus that subtends a solid angle decreasing with increasing luminosity (as inferred from the declining fraction of obscured AGNs), the intrinsic disk luminosity, L_D, is approximately proportional to the luminosity of the corona in the 2-300 keV energy band, L_C, with the L_D/L_C ratio varying by a factor of 2.1 around a mean value of 1.6. This ratio is a factor of ~2 smaller than for typical quasars producing the cosmic X-ray background (CXB). Therefore, over three orders of magnitude in luminosity, HX radiation carries a large, and roughly comparable, fraction of the bolometric output of AGNs. We estimate the cumulative bolometric luminosity density of local AGNs at ~(1-3)x10^40 erg/s/Mpc^3. Finally, the Compton temperature ranges between kT_c~2 and ~6 keV for nearby AGNs, compared to kT_c~2 keV for typical quasars, confirming that radiative heating of interstellar gas can play an important role in regulating SMBH growth.
    The Astrophysical Journal 08/2012; 757(2). · 6.73 Impact Factor
  • Mikhail G. Revnivtsev, Sergey V. Molkov
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    ABSTRACT: We present the results of deep scans across the Galactic plane that were performed with RXTE/PCA in 2010-2011. We studied the stripe from bII = 0° to bII = -30° at lII ≈ 18.°5. We show that the variance of the cosmic X-ray background (CXB) at angular scales ˜1 deg2 is approximately 5 per cent, which is compatible with the variance expected from Poisson variations of a number of discrete sources within the considered field of view. We estimate the cumulative fractional emissivity of the Galactic ridge X-ray emission (GRXE) as (3.0 ± 0.3) × 1027 erg s-1 M⊙-1 in the energy band 2-10 keV. We do not detect significant variations of the GRXE energy spectrum over the studied latitudes, which might be expected if the GRXE consists of contributions of sources with very different characteristic ages and scaleheights. Making use of ROSAT/PSPC/R7 data, collected within the stripe of our study, we estimate the cumulative emissivity of GRXE sources in the energy band 0.5-2 keV as ˜8 × 1027 erg s-1 M⊙-1; however, this estimate is subject to uncertainties owing to low-accuracy correction for interstellar photo-absorption. At Galactic latitudes -12° to -18° we detect ˜6-8 degrees size contributionfrom the hot plasma component, with the effective temperature ˜1.6 keV significantly exceeding that usually known for the soft X-ray Galactic background. Its surface brightness is higher than that of any other Galactic components at energies 1-2 keV and gives up to ˜20 per cent of the CXB at these energies. Accounting for such emission is of vital importance, for example, in studies of the emission of clusters of galaxies at their virial radii.
    Monthly Notices of the Royal Astronomical Society 08/2012; 424(3):2330-2338. · 5.52 Impact Factor
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    ABSTRACT: A simple method for calculating a low-resolution power spectrum from data with gaps is described. The method is a modification of the $\Delta$-variance method previously described by Stutzki and Ossenkopf. A Mexican Hat filter is used to single out fluctuations at a given spatial scale and the variance of the convolved image is calculated. The gaps in the image, defined by the mask, are corrected for by representing the Mexican Hat filter as a difference between two Gaussian filters with slightly different widths, convolving the image and mask with these filters and dividing the results before calculating the final filtered image. This method cleanly compensates for data gaps even if these have complicated shapes and cover a significant fraction of the data. The method was developed to deal with problematic 2D images, where irregular detector edges and masking of contaminating sources compromise the power spectrum estimates, but it can also be straightforwardly applied to 1D timing analysis or 3D data cubes from numerical simulations.
    Monthly Notices of the Royal Astronomical Society 07/2012; 426(3). · 5.52 Impact Factor
  • Solen Balman, Mikhail Revnivtsev
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    ABSTRACT: We study nature of time variability of brightness of non-magnetic cataclysmic variables. We show that lightcurtves of all analyzed DN systems in UV and X-ray energy bands demonstrate band limited noise, which can be adequately described in the framework of the model of propagating fluctuations. The frequency of the break indicates the inner disc truncation with a range of radii (10-3)e+9 cm. We analyse the RXTE and optical (RTT150) data of SS Cyg in outburst and quiescence which show that during the outburst the inner disk radius moves towards the white dwarf and receeds as the outburst declines to quiescence. Cross-correlations between the simultaneous UV and X-ray light curves find time lags in the X-rays of 90-180 sec consistent with travel time of matter from a truncated inner disc to the white dwarf surface. This suggests that DN and other plausible nonmagnetic systems have truncated accretion discs indicating that the accretion may occur through coronal flows in the disc. We compare and contrast magnetic and nonmagnetic systems in terms of their aperiodic noise characteristics and the model of propagating fluctuations. The comparison of the X-ray/UV time lag observed by us in the case of non-magnetic CVs with those, detected for magnetic CVs allows us to make an rough estimate of the viscosity parameter. Multi band simultaneous observations of coming observattories like ASTROSAT will give us the opportunity to study time variability of brightness variations of accretion disks in cataclysmic variables in quiescence and outburst using LAXPC and UVIT/OPT instruments. We will elaborate on the nature and possible outcomes of such research.
    07/2012;
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    ABSTRACT: There are three directories for three energy bands: e00170035, e00170060 and e0035_0080. Every directory contains six directories with corresponding 70x36 deg. sky mosaics: GAL-Survey+115 (l=+115°), GAL-Survey+50 (l=+50°), GAL-Survey-115 (l=-115°), GAL-Survey-50 (l=-50°), GAL-Survey-AC (l=180°) and GAL-Survey-GC (l=0°). Files are : *.fpsf.fits - sky flux in mCrab, convolved with instrumental PSF (2D Gaussian, σ=5') *.epsf.fits - 1 σ errors, mCrab (PSF convolved) *.spsf.fits - significance map, (PSF convolved) *_mapdld.fits - raw sky mosaics (not convolved with PSF) *.png - images in PNG format (4 data files).
    VizieR Online Data Catalog. 07/2012;
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    ABSTRACT: Context. The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. Aims. We aim to perform a Galactic survey that can be used as the basis of Galactic source population studies, and perform mapping of the Milky Way in hard X-rays over the maximum exposure available at |b|<17.5 deg. Methods. We used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. Results. We present sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17-60, 17-35, and 35-80 keV in the Galactic plane at |b|<17.5 deg. The total number of sources in the reference 17-60 keV band includes 402 objects exceeding a 4.7 sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei (AGNs) and 3 galaxy clusters. The sample of Galactic sources with S/N>4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients.
    Astronomy and Astrophysics 05/2012; · 5.08 Impact Factor
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    A. N. Semena, M. G. Revnivtsev
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    ABSTRACT: We consider the behavior of matter in the accretion column that emerges under accretion in binary systems near the surface of a white dwarf. The plasma heated in a standing shock wave near the white dwarf surface efficiently radiates in the X-ray energy band. We suggest a method for estimating post-shock plasma parameters, such as the density, temperature, and height of the hot zone, from the power spectrum of its X-ray luminosity variability. The method is based on the fact that the flux variability amplitude for the hot region at various Fourier frequencies depends significantly on its cooling time, which is determined by the parameters of the hot zone in the accretion column. This allows the density and temperature of the hot matter to be estimated. We show that the characteristic cooling time can be efficiently determined from the break frequency in the power spectrum of the X-ray flux variability for accreting white dwarfs. The currently available X-ray instruments do not allow such measurements to be made because of an insufficient collecting area, but this will most likely become possible with new-generation large-area X-ray spectrometers.
    Astronomy Letters 05/2012; 38(5). · 0.93 Impact Factor

Publication Stats

2k Citations
533.01 Total Impact Points

Institutions

  • 1998–2014
    • Russian Academy of Sciences
      • Space Research Institute
      Moskva, Moscow, Russia
  • 2013
    • European Space Agency
      Lutetia Parisorum, Île-de-France, France
  • 2000–2013
    • Space Research Institute
      Moskva, Moscow, Russia
  • 2010
    • University of Tuebingen
      • Institute for Astronomy and Astrophysics
      Tübingen, Baden-Württemberg, Germany
  • 2009–2010
    • Technische Universität München
      München, Bavaria, Germany
  • 2008
    • Harvard-Smithsonian Center for Astrophysics
      • Smithsonian Astrophysical Observatory
      Cambridge, Massachusetts, United States