Spectroscopic Monitoring of SS 433. Stability of Parameters of the Kinematic Model over 40 Years

Cherepashchuk, A. M.; Есипов, В. Ф.; Dodin, A. V.; Давыдов, В. В.; Belinski, A. A.

doi:10.1134/s106377291811001x

Cited by 13 publications

(20 citation statements)

References 20 publications

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“…An independent constraint on the binary mass ratio can be obtained from the observed radial velocity amplitude of HeII emission lines. The radial orbital velocity of the compact object in SS433 for the mean binary inclination i = 79 • (Cherepashchuk et al 2018a) reads…”

Section: Discussionmentioning

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: Discussionmentioning

confidence: 99%

Mass ratio in SS433 revisited

Черепащук

Постнов

Belinski

2019

Monthly Notices of the Royal Astronomical Society

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“…Despite more than forty years of research, the nature of the relativistic object in the SS433 system remained completely unclear until recently (see discussions on this topic in [6,7,20]). In [19,20], using information on the constancy of the orbital period of SS433 over 28 years [27,28], the authors estimated the ratio of the masses of the components in the SS433 q = M x M v = 0.6 (M x and M v are the masses of a relativistic object and an optical star, respectively). The constancy of the orbital period for the SS433 system is very surprising; after all, the rate of mass loss from the system in the form of wind from the supercritical accretion disc is very high, ~10 −4 M year −1 (see, for example, [9]).…”

Section: The Discovery Of An Increase In the Orbital Period Of The Ss433 System: A Strong Argument For The Presence Of A Black Holementioning

confidence: 99%

Progress in Understanding the Nature of SS433

Cherepashchuk

2021

Universe

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SS433 is the first example of a microquasar discovered in the Galaxy. It is a natural laboratory for studies of extraordinarily interesting physical processes that are very important for the relativistic astrophysics, cosmic gas dynamics and theory of evolution of stars. The object has been studied for over 40 years in the optical, X-ray and radio bands. By now, it is generally accepted that SS433 is a massive eclipsing X-ray binary in an advanced stage of evolution in the supercritical regime of accretion on the relativistic object. Intensive spectral and photometric observations of SS433 at the Caucasian Mountain Observatory of the P. K. Sternberg Astronomical Institute of M. V. Lomonosov Moscow State University made it possible to find the ellipticity of the SS433 orbit and to discover an increase in the system’s orbital period. These results shed light on a number of unresolved issues related to SS433. In particular, a refined estimate of the mass ratio MxMv>0.8 was obtained (Mx and Mv are the masses of the relativistic object and optical star). Based on these estimates, the relativistic object in the SS433 system is the black hole; its mass is >8M⊙. The ellipticity of the orbit is consistent with the “slaved” accretion disc model. The results obtained made it possible to understand why SS433 evolves as the semi-detached binary instead of the common envelope system.

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“…The jets also nutate with a period of 𝑃 nut 6 d .29. The parameters of the kinematic model of SS433 are found to be stable, on average, over the last 40 years (Cherepashchuk et al 2018a). Blundell et al (2007), Davydov et al (2008) and Cherepashchuk et al (2018a) detected traces of the orbital periodicity in the mass outflow velocity 𝛽 = 𝑣/𝑐 in the relativistic jets of SS433.…”

Section: Introductionmentioning

confidence: 95%

“…The parameters of the kinematic model of SS433 are found to be stable, on average, over the last 40 years (Cherepashchuk et al 2018a). Blundell et al (2007), Davydov et al (2008) and Cherepashchuk et al (2018a) detected traces of the orbital periodicity in the mass outflow velocity 𝛽 = 𝑣/𝑐 in the relativistic jets of SS433. These variations can be interpreted in terms of a possible small eccentricity of the binary orbit of SS433.…”

Section: Introductionmentioning

confidence: 95%

Discovery of orbital Eccentricity and Evidence for orbital Period Increase of SS433

Cherepashchuk,

Belinski,

Dodin

et al. 2021

Preprint

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The examination of long-term (1979-2020) photometric observations of SS433 enabled us to discover a non-zero orbital eccentricity of 𝑒 = 0.05 ± 0.01. We have also found evidence for a secular increase in the orbital period at a rate of 𝑃 b = (1.0 ± 0.3) × 10 −7 s s −1 . The binary orbital period increase rate makes it possible to improve the estimate of the binary mass ratio 𝑞 = 𝑀 X /𝑀 V > 0.8, where 𝑀 X and 𝑀 V are the masses of the relativistic object and the optical star, respectively. For an optical star mass of 10M , the mass of the relativistic object (a black hole) is 𝑀 X > 8M . A neutron star in SS433 is reliably excluded because in that case the orbital period should decrease, in contradiction to observations. The derived value of 𝑃 b sets a lower limit on the mass-loss rate in the Jeans mode from the binary system 7 × 10 −6 M yr −1 . The discovered orbital ellipticity of SS433 is consistent with the model of the slaved accretion disc tracing the precession of the misaligned optical star's rotational axis.

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Spectroscopic Monitoring of SS 433. Stability of Parameters of the Kinematic Model over 40 Years

Cited by 13 publications

References 20 publications

Mass ratio in SS433 revisited

Mass ratio in SS433 revisited

Progress in Understanding the Nature of SS433

Discovery of orbital Eccentricity and Evidence for orbital Period Increase of SS433

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