Accretion simulations of Eta Carinae and implications to massive binaries

AbstractUsing high resolution 3D hydrodynamical simulations we quantify the amount of mass accreted onto the secondary star of the binary system η Carinae during periastron passage on its highly eccentric orbit. The accreted mass is responsible for the spectroscopic event occurring every orbit close to periastron passage, during which many lines vary and the x-ray emission associated with the destruction wind collision structure declines. The system is mainly known for its giant eruptions that occurred in the nineteenth century. The high mass model of the system, M1=170M⊙ and M2=80M⊙, gives Macc≍ 3×10−6M⊙ compatible with the amount required for explaining the reduction in secondary ionization photons during the spectroscopic event, and also matches its observed duration. As accretion occurs now, it surely occurred during the giant eruptions. This implies that mass transfer can have a huge influence on the evolution of massive stars.

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Mass transfer on a nuclear timescale in models of supergiant and ultra-luminous X-ray binaries

Astronomy and Astrophysics ◽

10.1051/0004-6361/201935453 ◽

2019 ◽

Vol 628 ◽

pp. A19 ◽

Cited By ~ 6

Author(s):

M. Quast ◽

N. Langer ◽

T. M. Tauris

Keyword(s):

Mass Transfer ◽

Black Hole ◽

Neutron Star ◽

Roche Lobe ◽

High Mass ◽

X Rays ◽

X Ray ◽

Mass Ratios ◽

X Ray Binaries ◽

Eddington Limit

Context. The origin and number of the Galactic supergiant X-ray binaries is currently not well understood. They consist of an evolved massive star and a neutron star or black-hole companion. X-rays are thought to be generated from the accretion of wind material donated by the supergiant, while mass transfer due to Roche-lobe overflow is mostly disregarded because the high mass ratios of these systems are thought to render this process unstable. Aims. We investigate how the proximity of supergiant donor stars to the Eddington limit, and their advanced evolutionary stage, may influence the evolution of massive and ultra-luminous X-ray binaries with supergiant donor stars (SGXBs and ULXs). Methods. We constructed models of massive stars with different internal hydrogen and helium gradients (H/He gradients) and different hydrogen-rich envelope masses, and exposed them to slow mass-loss to probe the response of the stellar radius. In addition, we computed the corresponding Roche-lobe overflow mass-transfer evolution with our detailed binary stellar evolution code, approximating the compact objects as point masses. Results. We find that a H/He gradient in the layers beneath the surface, as it is likely present in the well-studied donor stars of observed SGBXs, can enable mass transfer in SGXBs on a nuclear timescale with a black-hole or a neutron star accretor, even for mass ratios in excess of 20. In our binary evolution models, the donor stars rapidly decrease their thermal equilibrium radius and can therefore cope with the inevitably strong orbital contraction imposed by the high mass ratio. We find that the orbital period derivatives of our models agree well with empirical values. We argue that the SGXB phase may be preceded by a common-envelope evolution. The envelope inflation near the Eddington limit means that this mechanism more likely occurs at high metallicity. Conclusion. Our results open a new perspective for understanding that SGBXs are numerous in our Galaxy and are almost completely absent in the Small Magellanic Cloud. Our results may also offer a way to find more ULX systems, to detect mass transfer on nuclear timescales in ULX systems even with neutron star accretors, and shed new light on the origin of the strong B-field in these neutron stars.

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High mass X-ray binaries as progenitors of gravitational wave sources

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318008037 ◽

2018 ◽

Vol 14 (S346) ◽

pp. 417-425 ◽

Cited By ~ 2

Author(s):

Jakub Klencki ◽

Gijs Nelemans

Keyword(s):

Mass Transfer ◽

Massive Star ◽

Formation Rate ◽

Point Of View ◽

High Mass ◽

Close Binary ◽

X Ray ◽

Orbital Periods ◽

X Ray Binaries ◽

Hubble Time

AbstractX-ray binaries with black hole (BH) accretors and massive star donors at short orbital periods of a few days can evolve into close binary BH (BBH) systems that merge within the Hubble time. From an observational point of view, upon the Roche-lobe overflow such systems will most likely appear as ultra-luminous X-ray sources (ULXs). To study this connection, we compute the mass transfer phase in systems with BH accretors and massive star donors (M > 15 Mʘ) at various orbital separations and metallicities. In the case of core-hydrogen and core-helium burning donors (cases A and C of mass transfer) we find the typical duration of super-Eddington mass transfer of up to 106 and 105 yr, with rates of 10−6 and 10−5Mʘ yr-1, respectively. Given that roughly 0.5 ULXs are found per unit of star formation rate, we estimate the rate of BBH mergers from stable mass transfer evolution to be at most 10 Gpc−3 yr−1.

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High resolution spectroscopy of X-ray emission from high mass X-ray binaries

Advances in Space Research ◽

10.1016/j.asr.2006.04.029 ◽

2006 ◽

Vol 38 (12) ◽

pp. 2737-2741

Author(s):

F. Nagase ◽

S. Watanabe

Keyword(s):

High Resolution ◽

High Resolution Spectroscopy ◽

High Mass ◽

X Ray ◽

X Ray Binaries

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Optical Low States of the Supersoft X-Ray Source RXJ0513.9–6951

International Astronomical Union Colloquium ◽

10.1017/s0252921100043992 ◽

1997 ◽

Vol 163 ◽

pp. 787-787

Author(s):

K. Reinsch ◽

A. van Teeseling ◽

K. Beuermann ◽

T.M.C. Abbott

Keyword(s):

Mass Transfer ◽

White Dwarf ◽

Mass Transfer Rate ◽

Central Star ◽

High Mass ◽

X Ray ◽

Total Luminosity ◽

Nuclear Burning ◽

Sudden Decrease ◽

Optical Flux

The transient luminous soft X-ray source RXJ0513.9–6951 (Schaeidt et al., 1993, A&A 270, L9) is a high-mass-transfer binary system (Cowley et al., 1993, ApJ 418, L63; Pakull et al., 1993, A&A 278, L39) with a probable orbital period of 0.76 days (Crampton et al., 1996, ApJ 456, 320). Here, we summarize the results of a quasi-simultaneous optical and X-ray monitoring (see Fig. 1). The sudden decrease of the optical flux, the accompanying reddening, and the turn-on in the soft X-ray band can be quantitatively described by variations in the irradiation of the accretion disk by the hot central star (Reinsch et al., 1996, A&A 309, L11). In this simple model, we consider a white dwarf with nuclear burning of accreted matter (van den Heuvel et al., 1992, A&A 262, 97), surrounded by a flat standard disk. In the optical high state, accretion at near-Eddington rate occurs and the white dwarf photospheric radius must be considerably expanded causing an enhanced illumination of the disk and the secondary. In the optical low state, the photosphere shrinks in response to a temporarily slightly reduced mass-transfer rate. At the same time, the effective temperature increases, and the soft X-ray flux becomes detectable with ROSAT. This model does not depend on the particular cause for the drop in the accretion rate and can describe the optical/ X-ray variability with the total luminosity changing by less than 20 %.

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Infrared spectroscopic variability of Cygnus X-3

Symposium - International Astronomical Union ◽

10.1017/s007418090020572x ◽

1999 ◽

Vol 193 ◽

pp. 358-359

Author(s):

Margaret M. Hanson ◽

Rob P. Fender ◽

G.G. Pooley

Keyword(s):

Mass Transfer ◽

High Resolution ◽

Ir Spectroscopy ◽

Spherically Symmetric ◽

X Rays ◽

Spectral Variability ◽

X Ray ◽

Orbital Phase ◽

Band Spectra ◽

Binary Orbit

We present four epochs of high-resolution IR spectroscopy of the peculiar X-ray binary Cygnus X-3. The observations cover quiescent, small flaring and outburst states of the system as defined by radio and X-ray monitoring. The underlying IR spectrum of the source, as observed during radio and X-ray quiescence and small flaring states is one of broad, weak He II and N V emission. Spectral variability in this state is dominated by modulation at the 4.8 hr orbital period of the system. H-band spectra confirm the significant hydrogen depletion of the mass donor. In outburst, the infrared spectrum is dramatically different, with the appearance of very strong twin-peaked He I emission displaying both day-to-day variability and V (iolet) / R(ed) variations with orbital phase. We argue that the most likely explanation appears to be an enhanced stellar wind from the companion. Thus the X-ray and radio outbursts in this system are likely to originate in mass-transfer, and not disc instabilities. We suggest that the wind in Cyg X-3 is significantly flattened in the plane of the binary orbit. This may explain the observed twin-peaked He I features as well as reconcile the large infrared luminosity with the large optical depth to X-rays if Cyg X-3 is embedded in a spherically symmetric wind.

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Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

Galaxies ◽

10.3390/galaxies7040088 ◽

2019 ◽

Vol 7 (4) ◽

pp. 88 ◽

Cited By ~ 7

Author(s):

Paul A. Crowther

Keyword(s):

Massive Stars ◽

Hii Regions ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

High Mass ◽

Stellar Content ◽

X Ray ◽

Star Forming ◽

Rosetta Stone ◽

The Individual

A review of the properties of the Tarantula Nebula (30 Doradus) in the Large Magellanic Cloud is presented, primarily from the perspective of its massive star content. The proximity of the Tarantula and its accessibility to X-ray through radio observations permit it to serve as a Rosetta Stone amongst extragalactic supergiant HII regions since one can consider both its integrated characteristics and the individual properties of individual massive stars. Recent surveys of its high mass stellar content, notably the VLT FLAMES Tarantula Survey (VFTS), are reviewed, together with VLT/MUSE observations of the central ionizing region NGC 2070 and HST/STIS spectroscopy of the young dense cluster R136, provide a near complete Hertzsprung-Russell diagram of the region, and cumulative ionizing output. Several high mass binaries are highlighted, some of which have been identified from a recent X-ray survey. Brief comparisons with the stellar content of giant HII regions in the Milky Way (NGC 3372) and Small Magellanic Cloud (NGC 346) are also made, together with Green Pea galaxies and star forming knots in high-z galaxies. Finally, the prospect of studying massive stars in metal poor galaxies is evaluated.

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Wind Roche lobe overflow in high-mass X-ray binaries

Astronomy and Astrophysics ◽

10.1051/0004-6361/201834543 ◽

2019 ◽

Vol 622 ◽

pp. L3 ◽

Cited By ~ 18

Author(s):

I. El Mellah ◽

J. O. Sundqvist ◽

R. Keppens

Keyword(s):

Mass Transfer ◽

Compact Object ◽

Stellar Mass ◽

Roche Lobe ◽

High Mass ◽

Transfer Rates ◽

X Ray ◽

Accretion Rates ◽

Mass Outflow ◽

X Ray Binaries

Ultraluminous X-ray sources (ULXs) have such high X-ray luminosities that they were long thought to be accreting intermediate-mass black holes. Yet, some ULXs have been shown to display periodic modulations and coherent pulsations suggestive of a neutron star in orbit around a stellar companion and accreting at super-Eddington rates. In this Letter, we propose that the mass transfer in ULXs could be qualitatively the same as in supergiant X-ray binaries (SgXBs), with a wind from the donor star highly beamed towards the compact object. Since the star does not fill its Roche lobe, this mass transfer mechanism known as “wind Roche lobe overflow” can remain stable even for large donor-star-to-accretor mass ratios. Based on realistic acceleration profiles derived from spectral observations and modeling of the stellar wind, we compute the bulk motion of the wind to evaluate the fraction of the stellar mass outflow entering the region of gravitational predominance of the compact object. The density enhancement towards the accretor leads to mass-transfer rates systematically much larger than the mass-accretion rates derived by the Bondi-Hoyle-Lyttleton formula. We identify orbital and stellar conditions for a SgXBs to transfer mass at rates necessary to reach the ULX luminosity level. These results indicate that Roche-lobe overflow is not the only way to funnel large quantities of material into the Roche lobe of the accretor. With the stellar mass-loss rates and parameters of M101 ULX-1 and NGC 7793 P13, wind Roche-lobe overflow can reproduce mass-transfer rates that qualify an object as an ULX.

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Episodic Mass Transfer: A Trigger for Nova Outbursts?

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312014755 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 88-95

Author(s):

Robert Williams

Keyword(s):

Mass Transfer ◽

High Resolution ◽

White Dwarf ◽

Spectral Evolution ◽

Secondary Star ◽

Multiple Components ◽

Line Widths ◽

Alternative Scenarios ◽

Nova Outbursts ◽

Secular Increase

AbstractHigh resolution spectra of post-outburst novae show multiple components of ejected gas that are kinematically distinct. We interpret the observations in terms of episodes of enhanced mass transfer originating from the secondary star that result in the formation of discrete components of circumbinary gas and accretion onto the white dwarf (WD) that trigger nova outbursts. In this picture the concordance between absorption line velocities and emission line widths in most novae occurs as a result of the collision of the expanding nova ejecta with a larger mass of surrounding circumbinary gas. One implication of this model is that much of the accreted gas remains on the WD, leading to a secular increase in WD mass over each outburst event. Alternative scenarios to explain nova spectral evolution are possible that do not invoke circumbinary gas and a possible test of different models is proposed.

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