On masses of the components in SS433

Cherepashchuk, A. M.; Постнов, К. А.; Belinski, A. A.

doi:10.1093/mnras/sty1853

Cited by 26 publications

(35 citation statements)

References 25 publications

(52 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…radial velocities (Hillwig & Gies 2008;Kubota et al 2010) or other estimates of the mass ratio (Cherepashchuk et al 2018;Bowler 2018). The extended outflows therefore seem to require a mechanism for transfer of substantial specific angular momentum to the outflowing material, which requires tidal or magnetic torques.…”

Section: Model Resultsmentioning

confidence: 99%

“…A more exotic possibility would be extraction of angular momentum from a neutron star through a magnetic propeller effect, in which transfer of angular momentum from the spinning neutron star to the flow can happen if the magnetospheric radius R m is larger than the co-rotation radius R co , leading the flow to be centrifugally ejected (Illarionov & Sunyaev 1975). Although the currently favored model for SS 433 is based on accretion-powered outflows from a massive stellar-mass black hole (Fabrika 2004;Cherepashchuk et al 2018;Bowler 2018), neutron star models for SS 433 have been considered in the past (e.g., Begelman et al 1980;Begelman & Rees 1984), including the idea that it could be a supercritical propeller (Mineshige et al 1991). In the latter scenario, R m is smaller than the spherization radius R sp meaning that a thick disk could still form (R sp is the radius within which the disk becomes geometrically thick from radiation pressure, determined from L(R > R sp ) = L Eddington ; Shakura & Sunyaev 1973).…”

Section: Model Resultsmentioning

confidence: 99%

“…Gaussian components arising from a circumbinary disk have also been suggested in the Brγ and He I emission lines (Perez & Blundell 2009;Bowler 2010). Cherepashchuk et al (2018) argues that the double-peaked structure must indeed arise from extended material because the wings of the line are not eclipsed (as would be expected for an accretion disk; SS 433 is an eclipsing binary). On the other hand, radial-velocity measurements, notably extremely challenging in SS 433 due to the complexity of the emission lines and lack of clear stellar signatures, tend to favor lower masses of 2−5 M for the compact object (Hillwig & Gies 2008;Kubota et al 2010).…”

Section: Introductionmentioning

confidence: 94%

See 2 more Smart Citations

Super-Keplerian equatorial outflows in SS 433

Waisberg

Dexter

Petrucci

et al. 2019

A&A

View full text Add to dashboard Cite

Context. The microquasar SS 433 is the only known steady supercritical accretor in the Galaxy. It is well-known for its relativistic baryonic jets, but the system also drives equatorial outflows. These have been routinely detected in radio images, and components associated with a circumbinary disk have also been suggested in optical emission lines. Aims. We aim to spatially resolve the regions producing the stationary emission lines of SS 433 to shed light on its circumbinary structure and outflows. With an estimated binary orbit size of ≲0.1 mas, this requires optical interferometry. Methods. We use the optical interferometer VLTI+GRAVITY to spatially resolve SS 433 in the near-infrared K band at high spectral resolution (R ≈ 4000) on three nights in July 2017. This is the second such observation, after the first one in July 2016. Results. The stationary Brγ line in the 2017 observation is clearly dominated by an extended ∼1 mas ∼ 5 AU circumbinary structure perpendicular to the jets with a strong rotation component. The rotation direction is retrograde relative to the jet precession, in accordance with the slaved disk precession model. The structure has a very high specific angular momentum and is too extended to be a stable circumbinary disk in Keplerian rotation; interpreting it as such leads to a very high enclosed mass M ≳ 400 M⊙. We instead interpret it as the centrifugal ejection of the circumbinary disk, with the implication that there must be an efficient transfer of specific angular momentum from the binary to the disk. We suggest that the equatorial outflows sometimes seen in radio images result from similar episodes of circumbinary disk centrifugal ejection. In addition to the equatorial structure, we find a very extended ∼6 mas ∼ 30 AU spherical wind component to the Brγ line: the entire binary is engulfed in an optically thin spherical line emission envelope.

show abstract

Section: Model Resultsmentioning

confidence: 99%

Section: Model Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 94%

See 1 more Smart Citation

Super-Keplerian equatorial outflows in SS 433

Waisberg

Dexter

Petrucci

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…It is not excluded that the so-called stable 'isotropic reemission' mass transfer mode can be realized in high-mass Xray binaries with massive BHs, thus helping to avoid the merging of the binary system components in the common envelope (van den Heuvel et al 2017). This stable mass transfer mode can explain the surprising stability of kinematic characteristics observed in the galactic microquasar SS433 (Cherepashchuk et al 2018). Of course, much more empirical constraints on and hydro simulations of the common evolution formation and properties are required.…”

Section: Introductionmentioning

confidence: 89%

Black hole spins in coalescing binary black holes

Постнов

Куранов

2018

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The possible formation mechanisms of massive close binary black holes (BHs) that can merge in the Hubble time to produce powerful gravitational wave bursts detected during advanced LIGO O1 and O2 science runs include the evolution from field low-metallicity massive binaries, the dynamical formation in dense stellar clusters and primordial BHs. Different formation channels produce different source distributions of total masses M tot and effective spins χ eff of coalescing binary BHs. Using a modified bse code, we carry out extensive population synthesis calculations of the expected effective spin and total mass distributions from the standard field massive binary formation channel for different metallicities of BH progenitors (from zero-metal Population III stars up to solar metal abundance), different initial rotations of the binary components, stellar wind mass loss prescription, different BH formation models and a range of common envelope efficiencies. The stellar rotation is treated in two-zone (coreenvelope) approximation using the effective core-envelope coupling time and with an account of the tidal synchronization of stellar envelope rotation during the binary system evolution. The results of our simulations, convolved with the metallicity-dependent star-formation history, show that the total masses and effective spins of the merging binary black holes detected during LIGO O1-O2 runs but the heaviest one (GW170729) can be simultaneously reproduced by the adopted BH formation models. Noticeable effective spin of GW170729 requires additional fallback from the rotating stellar envelope.

show abstract

“…It is a close binary system with a stellar-mass black hole (see Fabrika 2004 for a review). The accretion rate in this system is estimated to reach 300Ṁ edd (for the radiative efficiency of η = 1/12 and black hole mass MBH ≈ 10M ⊙ , Cherepashchuk et al 2018), whereṀ edd is the Eddingon ac-cretion rate. Optical spectra of SS 433 contain broad emission lines of hydrogen and He II with FWHM suggesting velocities of 1000 km/s originating from an accretion disc wind.…”

Section: Introductionmentioning

confidence: 99%

Ultraluminous X-ray sources with flat-topped noise and QPO

Атапин

Fabrika

Caballero‐García

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We analyzed the X-ray power density spectra of five ultraluminous X-ray sources (ULXs) NGC 5408 X-1, NGC 6946 X-1, M 82 X-1, NGC 1313 X-1 and IC 342 X-1 that are the only ULXs which display both flat-topped noise (FTN) and quasi-periodic oscillations (QPO). We studied the QPO frequencies, fractional root-mean-square (rms) variability, X-ray luminosity and spectral hardness. We found that the level of FTN is anti-correlated with the QPO frequency. As the frequency of the QPO and brightness of the sources increase, their fractional variability decreases. We propose a simple interpretation using the spherizarion radius, viscosity time and α-parameter as basic properties of these systems. The main physical driver of the observed variability is the mass accretion rate which varies 3 between different observations of the same source. As the accretion rate decreases the spherization radius reduces and the FTN plus the QPO move toward higher frequencies resulting in a decrease of the fractional rms variability. We also propose that in all ULXs when the accretion rate is low enough (but still super-Eddington) the QPO and FTN disappear. Assuming that the maximum X-ray luminosity depends only on the black hole (BH) mass and not on the accretion rate (not considering the effects of either the inclination of the super-Eddington disc nor geometrical beaming of radiation) we estimate that all the ULXs have about similar BH masses, with the exception of M 82 X-1, which might be 10 times more massive.

show abstract

On masses of the components in SS433

Cited by 26 publications

References 25 publications

Super-Keplerian equatorial outflows in SS 433

Super-Keplerian equatorial outflows in SS 433

Black hole spins in coalescing binary black holes

Ultraluminous X-ray sources with flat-topped noise and QPO

Contact Info

Product

Resources

About