Coronagraphic methods for detecting faint astronomical objects near bright ones: Application to the 2.5-m telescope of Sternberg Astronomical Institute

Черепащук, А. М.; Bugaenko, O. I.; Kim, I. S.; Попов, В. В.

doi:10.1134/s1063772917030039

Cited by 2 publications

(3 citation statements)

References 6 publications

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“…When estimating the mass of the relativistic object in SS433 one should bear in mind that the distance to the system is well known, d = 5.5 kpc (Blundell & Bowler 2004), and the total absorption in the direction to SS433 in the optical is A v 8 m (Cherepashchuk et al 1982;Margon 1984). Using this information, from the visible stellar magnitude of SS433 and by fixing the fraction of the optical emission from the supercritical accretion disc (∼ 0.6 − 0.7, Hillwig & Gies (2008)), it is possible to estimate the mass of the optical component, which, according to Goranskij (2011), falls within the range M v = 8.3 − 12.5M , corresponding to the spectral class A4I-A8I.…”

Section: Introductionmentioning

confidence: 99%

Mass ratio in SS433 revisited

Черепащук

Постнов

Belinski

2019

Monthly Notices of the Royal Astronomical Society

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We revisit the determination of binary mass ratio in the Galactic microquasar SS433 based on recent GRAVITY VLTI measurements of mass and angular momentum outflow through a circumbinary disc. The new observations combined with the constancy of the binary orbital period over ∼ 30 yrs confirm that the mass ratio in SS433 is q = M x /M v 0.6. For the assumed optical star mass M v ranging from ∼ 8 to 15 M such a mass ratio suggests a low limit of the compact object mass of M x ∼ 5 − 9M , placing the compact object in SS433 as a stellar-mass black hole.

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Section: Introductionmentioning

confidence: 99%

Mass ratio in SS433 revisited

Черепащук

Постнов

Belinski

2019

Monthly Notices of the Royal Astronomical Society

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“…About 300 supermassive black holes (SMBH) exist in active galactic nuclei (AGN). There are ∼ 20 BH in X-ray stellar binary systems ( see Cherepashchuk 2006).The observed linear polarization from (AGN) in Seyfert galaxies frequently demonstrate two types of polarization. In the first type the wave electric field E-oscillations are parallel to the plane of accretion disc.…”

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confidence: 99%

“…About 300 supermassive black holes (SMBH) exist in active galactic nuclei (AGN). There are ∼ 20 BH in X-ray stellar binary systems ( see Cherepashchuk 2006).…”

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confidence: 99%

Intensity and polarization of radiation reflected from accretion disc

Силантьев

Alekseeva

Новиков

2018

Astrophys Space Sci

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We consider the reflection of non-polarized radiation from the point-like sources above the accretion discs both the optically thick and optically thin. We investigate the dependence of the polarization of reflected radiation on the aperture angle of incident radiation. The aperture angle is determined by the radius of accretion disc and the height of the source above the disc. For optically thick accretion discs we show that, if the aperture angle is smaller 70 grad, then the wave electric field oscillations of reflected radiation are parallel to the accretion disc plane. For aperture angle greater than 70 grad the electric field oscillations are parallel to the plane "normal to accretion disc -the line of sight". The latter also holds for reflection from the optically thin accretion disc independent of the aperture angle value.The black holes (BH) demonstrate the presence of accretion discs both optically thick and optically thin. About 300 supermassive black holes (SMBH) exist in active galactic nuclei (AGN). There are ∼ 20 BH in X-ray stellar binary systems ( see Cherepashchuk 2006).The observed linear polarization from (AGN) in Seyfert galaxies frequently demonstrate two types of polarization. In the first type the wave electric field E-oscillations are parallel to the plane of accretion disc. In the second type the E-oscillations are parallel to the plane (nN), where N is the normal to the disc plane and n is the line of sight. It appears the same effect is in X-ray binary systems ( see, for example, Fabrika 2004 and references therein). The most often observed polarization is parallel to the disc plane. In Seyfert-1 AGNs the polarization frequently corresponds to oscillations in the plane (nN), but there are polarizations with intermediate values of position angles. Note that the measurement of linear polarization from AGN is one of very effective technique to obtain the information about the structure of AGN. The polarimetric results are given in many papers (see, for example, Impey et al.

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Coronagraphic methods for detecting faint astronomical objects near bright ones: Application to the 2.5-m telescope of Sternberg Astronomical Institute

Cited by 2 publications

References 6 publications

Mass ratio in SS433 revisited

Mass ratio in SS433 revisited

Intensity and polarization of radiation reflected from accretion disc

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