Analysis of X-Ray Eclipses in SS 433

Antokhina, É. A.; Cherepashchuk, A. M.; Seyfina, E. V.

doi:10.1007/978-94-011-1924-5_64

Cited by 21 publications

(34 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Furthermore, the magnitude of the negative quadratic terms is likely to give only a lower limit, since the mass transfer events causingṖ < 0 might be expected to have a shorter duration than the time interval between observational measurements. In conclusion, we find that the variations in the derived values ofṖ are consistent with the suggestion of Kurochkin (1979; cited by Antokhina et al 1982) thatṖ alternates between positive and negative values.…”

Section: The Variations Inṗsupporting

confidence: 92%

“…The wind mass-loss is expected to produce an increase over time of the orbital period in the rangeṖ ∼ 0.07-0.2 s yr −1 (Khaliullin 1974). However, the analyses of CQ Cep's light curves by Gaposchkin (1944) and Semeniuk (1968) result in the contrary conclusion, as do Antokhina et al (1982;Ṗ = −0.019 ± 0.006 s yr −1 ) and Cherepashchuk (1982;Ṗ = −0.038 s yr −1 ). The latter authors conclude that the dominant process in CQ Cep is one in which mass is being transferred from the WR star to the companion (assuming that the WR star is the more massive of the two stars in the system).…”

Section: Introductionmentioning

confidence: 96%

“…Walker et al (1983) arrived at a similar conclusion. An alternative scenario put forth by Kurochkin in 1979 as cited by Antokhina et al (1982) and Kreiner & Tremko (1983) is that the rate of period change alternates between positive and negative values, which could be explained if mass-transfer due to RLO occurred only sporadically.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Does the Wolf-Rayet binary CQ Cephei undergo sporadic mass transfer events?

Koenigsberger

Schmutz

Skinner

2017

A&A

View full text Add to dashboard Cite

Context. Stellar wind mass-loss in binary systems carries away angular momentum causing a monotonic increase in the orbital period, P > 0. Despite possessing a significant stellar wind, the eclipsing Wolf-Rayet (WR) binary system CQ Cep does not show the expected monotonic period increase, in fact, it is sometimes reported to display the opposite behavior. Aims. The objective of this paper is to perform a new analysis of the rate of period changeṖ and determine the conditions under which Roche-lobe overflow (RLO) mass-transfer combined with wind mass loss can explain the discrepant behavior. Methods. The historic records of times of light curve minima were reviewed and compared with the theoretical values ofṖ for cases in which both wind mass-loss and RLO occur simultaneously. Results. The observational data indicate thatṖ alternates between positive and negative values on a timescale of years. The negative values (Ṗ ∼ −0.6 to −8.5 s yr −1 ) are significantly larger in absolute value than the positive ones (Ṗ ∼ +0.2 to +1.2 s yr −1 ). We find that a plausible scenario for CQ Cep is one in which the O star undergoes intense but sporadic RLO events that lead to accretion onto the WR star, at which timesṖ < 0. At other times,Ṗ > 0 when the WR wind, and possibly material swept up from the O star, carries angular momentum away from the system. A scenario in which the WR star is the mass donor cannot be excluded, but requires that either the WR wind mass-loss rate undergoes large sporadic enhancements or that an additional process that removes angular momentum from the system be present.

show abstract

Section: The Variations Inṗsupporting

confidence: 92%

Section: Introductionmentioning

confidence: 96%

See 1 more Smart Citation

Does the Wolf-Rayet binary CQ Cephei undergo sporadic mass transfer events?

Koenigsberger

Schmutz

Skinner

2017

A&A

View full text Add to dashboard Cite

show abstract

“…Observed orbital Doppler shifts of the absorption lines of the optical component and stationary He ii emission allowed Hillwig & Gies to determine the mass ratio of the compact ( m x ) and the optical ( m v ) components in SS433 q = m x / m v ≃ 0.35, implying the binary masses m x = 4.3 ± 0.8 M ⊙ and m v = 12.3 ± 3.3 M ⊙ . Similar values of q , m x and m v were obtained from the analysis of the optical light curves of SS433 (Antokhina & Cherepashchuk 1987).…”

Section: Introductionmentioning

confidence: 61%

Peculiar nature of hard X-ray eclipse in SS433 fromINTEGRALobservations

Черепащук¹,

Sunyaev

Постнов³

et al. 2009

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The analysis of hard X-ray INTEGRAL observations (2003X-ray INTEGRAL observations ( -2008 of superaccreting Galactic microquasar SS433 at precessional phases of the source with the maximum disc opening angle is carried out. It is found that the shape and width of the primary X-ray eclipse are strongly variable, suggesting additional absorption in dense stellar wind and gas outflows from the optical A7I component and the wind-wind collision region. The independence of the observed hard X-ray spectrum on the accretion disc precessional phase suggests that hard X-ray emission (20-100 keV) is formed in an extended, hot, quasi-isothermal corona, probably heated by interaction of relativistic jet with inhomogeneous wind outflow from the precessing supercritical accretion disc. A joint modelling of X-ray eclipsing and precessional hard X-ray variability of SS433 revealed by INTEGRAL by a geometrical model suggests the binary mass ratio q = m x /m v 0.25-0.5. The absolute minimum of joint orbital and precessional χ 2 residuals is reached at q 0.3. The found binary mass ratio range allows us to explain the substantial precessional variability of the minimum brightness at the middle of the primary optical eclipse. For the mass function of the optical star f v = 0.268 M as derived from Hillwig & Gies data, the obtained value of q 0.3 yields the masses of the components m x 5.3 M , m v 17.7 M , confirming the black hole nature of the compact object in SS433.

show abstract

“…The value of the mass loss rate M for WR star from the observed period changes in WR+O eclipsing binaries (Khaliullin, 1974, Kornilov and Cherepashchuk, 1979, Khaliullin et al,1984, Antokhina et al 1982, Underhill et al, 1990) M= (0.6 -1)10~5Μ Θ / year is 2-3 times less than that derived for the same WR stars from IR and available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900122120 Downloaded from https://www.cambridge.org/core.…”

Section: Period Changes In Wr+o Eclipsing Binariesmentioning

confidence: 83%