A&A 404, 991-996 (2003)
DOI: 10.1051/0004-6361:20030534
L. Dessart -
N. Langer - J. Petrovic
Sterrenkundig Instituut, Universiteit Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands
Received 9 January 2003 / Accepted 21 March 2003
Abstract
We investigate to what extent the radiation and stellar wind momenta
in a massive close binary system can remove part of the matter flowing
from one towards the other star during a mass transfer phase.
We perform radiation-hydrodynamics simulations in the
co-rotating frame of a binary system made-up of two main sequence
stars of 27
and 26
in a 4 day orbit.
We study the interaction of the winds of both stars, and of their
photons, with the accretion stream
originating from the Roche-lobe filling component.
For our simulation, we adopt a mass transfer rate of 5
10-6
yr-1,
a mid-point in the range of values during massive binary star evolution.
Our simulations show that even for such moderate mass transfer rates, the
wind and radiative momenta do not alter the dynamics of the
accretion stream which is observed to follow essentially ballistic trajectories.
Such a conclusion is reinforced for higher mass transfer rates because
of the increased stream density and the correspondingly reduced
radiation force. We anticipate that the radiation and wind momenta
will affect the accretion stream only when its density is comparable
to the wind's, a situation wherein the mass transfer rate is
vanishingly small and irrelevant for binary star evolution. Alternatively,
such reduced accretion stream density could be obtained from spatial
dilution in wider systems, potentially leading to non-conservative mass
transfer.
Key words: stars: early-type - stars: winds, outflows - stars: binaries: general - hydrodynamics
Massive close binary stars may produce the most powerful explosions in the universe, the cosmic gamma ray bursts (GRBs), which can trace star formation to very high redshifts (Lloyd-Ronning et al. 2002). While the merger model for GRBs is clearly based on massive binaries (Fryer et al. 1999), even the collapsar model (MacFadyen & Woosley 1999) may require accretion of angular momentum in the GRB progenitor (Langer et al. 2002), as current single star models appear to have too little angular momentum (Heger et al. 2000, 2002). Further evolved observed massive binary counterparts include massive X-ray binaries - where in particular the black hole systems may again be linked to GRBs (Brown et al. 2000) -, supernovae of Type Ib and Ic (Podsiadlowski et al. 1992), Wolf-Rayet binaries (Schulte-Ladbeck 1989) and massive Algol systems (Penny et al. 2002).
To understand all these exciting objects, we need to understand the evolution of massive close binaries. However, the reliability of massive binary evolution models is hampered by a major uncertainty: What fraction of the mass transfered during a Roche-lobe overflow phase can be accreted by the secondary star?
From observations of post-mass transfer systems,
there seems to be evidence for both extremes. The two O stars in the
binary V 729 Cyg have a mass ratio of 3.5 but the same
spectral type and visual flux (Bohannan & Conti 1976).
An initial mass ratio close
to 1 is required to ensure the possibility of accretion (see below).
However, since during the mass transfer phase a primary star would lose just
about half of
its mass, a mass ratio of at most 2 could be produced were the
secondary not allowed to accrete. Another system showing strong evidence
for accretion is the massive X-ray binary Wray 977; it would require
that stars of
form neutron stars to explain this system
without accretion (Wellstein & Langer 1999).
Several Galactic short period WNE+O binaries, on the other hand, cannot
be understood had the O star accreted substantial amounts
from the WNE progenitor
(cf. Petrovic & Langer 2002). While those might have formed through
common envelope evolution - for which no accretion is expected - the key
X-ray binary 4U 1700-37 has such a short period that a major
accretion phase can be excluded. However, as common envelope evolution would
lead to a compact object much more massive than 2.4
,
a short
initial period is most likely here (Clark et al. 2002).
From the theoretical viewpoint, accretion in massive close binaries appears difficult. Indeed, the accreted material carries a large amount of angular momentum, potentially spinning the surface of the secondary star up to critical rotation, thereby halting the accretion process (Packet 1981; Wellstein 2001; Langer et al. 2002). In particular for the case of massive binaries, where accretion appears possible from the stellar structure point of view - short period systems consisting of two main sequence stars with nearly equal masses - this process faces another threat.
Short period systems, because of their reduced orbital separation, undergo mass transfer during the core hydrogen burning evolution of the primary (so called Case A mass transfer). As the masses of both stars are similar, so are their thermal time scales, which means that the secondary does not swell due to mass overflow on the thermal time scale of the primary, thus avoiding a contact situation (Wellstein & Langer 1999; Wellstein et al. 2001). As both stars have a similar size, the accreting star fills a significant fraction of its critical volume, leaving no space for an accretion disk, i.e. the overflowing matter may impact directly onto the accreting star, thereby minimising the angular momentum gain of the secondary (Wellstein 2001; Langer et al. 2002).
However, the price to pay for these advantages for accretion is a threat to it: a mass ratio close to one in a massive Case A binary means that the secondary is a massive and luminous main sequence star, i.e., it has an intense radiation field and a powerful stellar wind. Evolutionary studies of massive binary star systems so far have not investigated the impact of such wind and radiation momenta on the dynamics of accretion streams, but instead adopted, with a variable level of justification, how conservative mass transfer ought to be. This covers investigations that simply assume the amount of mass loss from the system (Huang & Taam 1990; Kondo 1974; Vanbeveren 1996) and those that account for a modulation depending on luminosity, evolutionary stage etc. (Podsiadlowsky et al. 1992; Doom & de Greve 1983; de Loore & de Greve 1992; de Loore & Vanbeveren 1994). Some detailed calculations of mass transfer and accretion do exist but were limited to objects with no stellar wind and weak radiation fields (Blondin et al. 1995; Boroson et al. 2001). Here, we wish to study the mass transfer properties in massive binary systems, avoiding former educated guesses by addressing with a physical rather than phenomenological model the dynamical properties of the accretion stream in the presence of stellar winds and intense radiation fields expected in such environments.
We present radiation-hydrodynamic simulations in Sect. 2, discussing the choice of geometrical set-up, boundary conditions and the radiation force implemented. In Sect. 3, we show the results of such a model for different scenarios of wind-momentum balance between the two components. We also discuss the outcome for different accretion stream densities and cross-sections. From our simulations, we conclude in Sect. 4 that radiation and wind momenta play an insignificant role in the mass budget during the mass transfer evolution of our example system.
The radiation-hydrodynamics simulations presented in this paper were performed with ZEUS-2D (Stone & Norman 1992), a finite difference, Eulerian code whose original magnetism and radiation modules were switched-off during the calculations. Hence, we only make use of the hydrodynamical structure of the code, implementing our own radiation module independently (see below). The advection scheme used is the first order Van Leer method. We introduce some artificial viscosity to smooth out strong shocks, improving the stability of the code without affecting the main features of the simulations. The simulated fluid is assumed isothermal, so that the sound speed is everywhere equal to a unique value corresponding to a temperature of 30 000 K.
In the present work, we have slightly modified the code to work in the
equatorial plane of the system, in spherical polar rather than cylindrical
coordinates. Since we wish to study the trajectory of the accretion stream
leaving the primary photosphere via the first Lagrangian point L1,
the secondary is placed at the
origin of the coordinate system. We calculate the fluid
properties from the secondary photosphere out to a distance which corresponds
to the orbital separation. In the azimuthal direction, we cover the full
2
angle as seen from the secondary star center. However, the simulated
domain is truncated along the line of centers and near the primary. The
surface of the latter cannot be described by a simple change of
one of the coordinates, but rather follows a curve relating the coordinates (r,
). Its photosphere, which acts as a boundary, has
a sawtooth shape, making its treatment very delicate, as encountered
by Owocki et al. (1994) and Petrenz & Puls (2000)
in simulations of winds from rotating hot stars.
The steep acceleration of hot star winds as predicted by radiatively-driven
wind theory requires a thorough treatment of the small subsonic region
confined to the photosphere, specifically because it is in this region that
the mass loss rate is set (Castor et al. 1975). To keep the
computation time of our simulations to a reasonable value, we decided
to fix the density and the velocity at the surface of the primary, allowing
the use of a lower grid resolution. The mass loss rate of the primary
is then set by the user rather than being a solution of the calculation.
In the case of 1D simulations of hot star winds, this would be highly
unorthodox, but in our present study, the primary has a very ellipsoidal
surface, possesses a zero gravity point and is likely to be gravity darkened.
In other words, we believe that the proper treatment of such a hot star
surface and wind is beyond the scope of this paper - in fact such an exercise
defies even the current best models of hot star winds - so that our
choice is not such a bad compromise (see Friend & Castor 1982; Owocki et al. 1996).
Hot stars drive outflows from the photosphere out to infinity
by imparting a radiative acceleration on the atmospheric material that
supersedes the local gravitational acceleration. In the phenomenon of
mass transfer, it is the thermal pressure within the outer
layers of the stellar envelope that lead to an outflow in the region
where the gravitational step is minimum, i.e. the vicinity of the
first Lagrangian point.
Thus, the dense photospheric material expands
and accelerates through the L1 region and "falls'' into the
gravitational potential well of the secondary star.
The velocity of the accretion stream through the L1
point is at most the sound speed, i.e. of the order of a few tens of km s-1 for hot
stars, and its geometrical cross section is of the order of a few degrees
(Lubow & Shu 1975; Ritter 1988). Typical photospheric densities of hot stars
are 10-10 g cm-3, which would then correspond to a mass transfer rate
of the order of few times 10-6 yr-1. Such a value will be adopted in most
of the simulations discussed in Sect. 3. However, there is evidence from
binary star evolutionary calculations that mass transfer occurs routinely with
a much larger magnitude of the order of 10-3
yr-1.
Physically, this can occur through an increase
in density or cross section of the accretion stream, alternatives we
investigate with our radiation-hydrodynamics model and discuss
in Sects. 3.2 and 3.3.
For our simulations, we assume both mass transfer and
stellar wind mass loss rates of the primary and secondary stars.
To simulate the wind from
the secondary, we choose a surface density such that the sound-speed
inflow of material at the boundary corresponds to the mass loss
rate as calculated with identical stellar and opacity parameters but with a
high spatial resolution (done separately in a 1D simulation), and using
reference parameters from Kudritzki et al. (1989). Each
of our simulations is first performed until a
stationary solution is found for both winds. Once this steady-state is
reached, we turn on the mass transfer. This takes the form of a sound-speed
inflow of mass from the primary surface at the L1 location, with specified
density and cross-section. These parameters are chosen so that they cover
the range of mass transfer rates predicted by stellar evolutionary
calculations. Note that the problem we are trying to tackle here
shares very little common ground with previous radiation-hydro
simulations of mass transfer by Roche-lobe overflow, which focused on
the case of white dwarfs, neutron stars, Algol systems, where the
magnitude of the mass transfer is always feeble, i.e. 10-7
yr-1 (Blondin et al. 1995; Boroson et al. 2001).
For the outer boundary, we clearly have an outflow if we treat exclusively the stellar winds. It was not clear whether such boundary type was appropriate for the simulations including mass transfer. However in all simulations performed, we find that any material reaching the outer edge of the grid possesses a velocity in excess of the escape value, ensuring that the choice of outflow for the outer boundary is adequate. Note that the staircase inflow boundary describing the surface of the primary is not perfectly handled (see Fig. 1) and leads to a spurious flow phenomenon in a few confined directions. This does not affect the gross fluid properties derived here.
We also have to treat the eventuality of the accretion stream impacting the secondary surface. The physics of the shock interface is very complex and cannot be modeled with the desired accuracy, especially with the low resolution of our simulations. We could have adopted different conditions that cover the extreme dynamical scenarios: material is allowed to freely penetrate the secondary surface, to do so at most with the sound speed or not at all (reflecting boundary). However, for simplicity, if material impacts the secondary star surface, the boundary type switches to reflecting.
![]() |
Figure 1: (Left column) Sequence of gray scale images showing the logarithm of the density of the fluids surrounding the two stars (steady state is reached). The details for each simulation from 1 to 3 are given in Table 2. (Right column) Same as above after mass transfer has been switched on for about 100 ksec (the images do not correspond to a steady state, which will not necessarily be reached before some fraction of the system evolutionary time scale). The secondary star surface does not permit inflow in the simulations shown here. |
Open with DEXTER |
For the calculation of the radiation force, we use two approaches.
Either we calculate the radiation force from a point star with a constant
correction factor for the finite disk size, or we integrate the radiation
force over the two stellar disks. We have found that the two methods lead
to similar properties, for two reasons. First, we find
that the radiation force on the accretion stream itself is only moderate
(Sect. 3). Moreover, the binary system we study is so compact that the
wind-wind-interaction region overlaps with the acceleration regions of
both winds, i.e. there is no wind stagnation for which multi-ray calculation
of the radiation force led to the discovery of the radiative braking
phenomenon (Gayley et al. 1997). Hence, a single ray calculation
of the radiation acceleration is performed according to
We also include the contribution from the centrifugal and Coriolis forces in the momentum equation. At the start of the computation, we calculate the centrifugal potential for all grid points, together with its gradient in the azimuthal and radial directions. It is then incorporated into the momentum equation in the same way as the pressure gradient. The Coriolis force is calculated using the coordinates of the center of mass and the gas parcel velocities with respect to it in a standard way.
Table 1: Standard parameters of our simulations. Table 2 gives updates to those parameters that are modified for the calculations presented in Sect. 3.
In this section, we discuss the results of our calculations. We investigate in particular the properties of the accretion stream in a number of simulations with different stellar wind mass loss and mass transfer rates (cf. Table. 2).
The central question of our investigation is whether radiation and wind
momenta can significantly affect the dynamics of the accretion stream
generated by the Roche-lobe filling component.
Therefore, we have performed various simulations adopting different
primary star luminosities and mass loss rates, hence modifying
the strength of the radiation field and the density of the wind emanating from
it. This way, we investigate three scenarios: 1) the
primary wind winning over the secondary's; 2) a wind balance between the two
stars leading to the formation of a wind-wind collision zone;
and 3) a situation where the secondary wind wins over the
primary wind. For each of these three cases, we investigate what happens
to the accretion stream using a moderate mass transfer rate
(5
10-6
yr-1). The results are shown
in Fig. 1.
Table 2:
List of performed simulations and the respective values used
for the key parameters. Sim 1-3 focus on the impact of varying wind
properties (through wind and radiation momenta). Sim 4 treats the case
of a bigger stream cross section and Sim 5-7 address the situation for
an enhanced stream density. These changes are implemented by changing
,
the half angular width of the stream as seen from the
primary center, or the density at L1. Scaling
(
)
by x scales the mass transfer by x(x2).
In case 1) 1 is enhanced by a factor 100 and the luminosity
of the primary by a factor of ten compared to the more realistic default
values presented in Table 1. We observe in Fig. 1
that in this situation, the wind of the secondary star is completely overwhelmed.
We find that the motion of the accretion stream is not impeded, nor is it modified in
any significant way from a standard ballistic trajectory. For the fluid densities
concerned here, the stream momentum is orders of magnitude above that of the winds,
which explains the disregard of the accretion stream with respect to
the "ambient'' medium.
In this close binary system, this leads to a fully conservative mass transfer.
Case 2) corresponds to the situation where the wind momenta of both stars
are equal (1 =
2 and similar luminosity for both stars),
giving rise to a wind-wind collision between the two binary
components. It has been argued in the past that the collision interface, because
it lies between L1 and the secondary surface, could interfere and maybe prevent
mass transfer from occurring. In our simulation, it is clear that the accretion
stream is not at all affected by this colliding zone. The same argument as in
case 1) applies, where essentially the density contrast favors the stream over
the two winds and the colliding interface. An analogy that may help is to view
such density contrasts as much bigger than that between air and water
(at room temperature). So, case 2) robustly leads to conservative mass transfer.
In case 3), we make the wind of the primary artificially small by reducing
1 to half the secondary's value. This situation would apparently be
unfavourable to the primary's mass transfer, but again, for similar
arguments as used in case 2) and 1), the wind from the secondary is no
match for the dense accretion stream.
This leads us to conclude that the radiation and wind momenta are totally
irrelevant for the general dynamics of the accretion stream, even in the
situation where the mass transfer rate is moderate
(5
10-6
yr-1). Hence, in such close binary systems, our
simulations strongly advocate conservative mass transfer.
As discussed in Sect. 2, the mass transfer rate can vary enormously during the evolution of a massive binary system. We investigate in this section the various ways such a mass transfer rate could be enhanced, namely by means of an increased density or geometrical cross section. We devote less attention to the case of lower rates than adopted in the previous section because they are doomed to play a weaker role, the accretion through direct impact of the companion wind potentially becoming an efficient alternative.
As discussed in the introduction to this section, a change in stream
cross-section can amplify the amount of transfered mass by at most a factor
of a few. We have run a number of simulations increasing the value of this
cross section up to 20
(Sim 4). While this seems a lot, one needs to remember
that given the low density in the outer envelope of the star, at the onset of
mass transfer, the corresponding rate of mass loss through L1 will likely be small.
We anticipate that the stellar envelope will continue growing beyond the Roche
surface, until the dense layers located deeper in the envelope near the L1 region
lead to a strong increase in mass transfer and the stabalisation of the envelope.
During this transition, the stream could indeed be much broader than the values
suggested in Ritter (1988).
Our simulations demonstrate that this case is a hybrid. A large fraction
of the accretion stream impacts the secondary surface, while the rest
creates a colliding interface with the secondary's outflow. This fraction of
interacting material is however small and therefore leads only to a minor
departure from conservative mass transfer.
We have performed simulations for L1 densities a factor ten and a hundred
higher than in Sect. 3.1 (Sim 5, 6 and 7). The momentum contrasts between
the stream and the winds are even larger than in Sect. 3.1, and we find that
the simulations, as expected, re-enforce the conclusion already made before.
Namely, for the high mass transfer rates (10-3
yr-1)
at which most of the mass from the primary is lost during Case A mass
transfer, the winds and radiation from either component have no effect on
the accretion stream.
We have investigated the importance of radiation and wind momenta on the dynamical behaviour of accretion streams produced by overflow of the Roche-lobe filling component in a binary system. We performed radiation-hydrodynamic simulations of a typical young, close (4 day period) and massive binary system, calculating explicitly the radiation force and wind properties for each component. We discussed situations for the different mass transfer rates encountered in evolutionary calculations for massive binary systems (Wellstein 2001), as well as the occurrence of different wind momentum balance.
The central result of our calculation is that the dynamics of mass transfer in massive close binary stars is not affected in any noticeable way by the radiation and wind momenta from each luminous component. These latter mechanisms cannot therefore be at the origin of the non-conservative mass transfer required to explain the observed mass ratios of many Wolf-Rayet binaries.
The reader may find surprising that the radiation force does not
modify the dynamical behaviour of an accretion stream. Although the
radiation force
efficiency is complex because it depends on the local velocity gradient
and therefore on the dynamics itself, its dependence on the inverse of the
density is really what makes it so ineffective here. The source of confusion
on the importance of the radiation force in massive close binary systems
could possibly arise from the failure to realise that important mass transfer
rates for the evolution of those systems are of the order of 10-3 yr-1,
corresponding to density regimes orders of magnitude beyond those of
hot star winds where the radiation acceleration is admittedly crucial.
One must also bear in mind that this mass transfer occurs through a restricted
region of space whilst stellar winds occur in principle from all
stellar surface locations. Thus, for a mass transfer and wind mass loss
of identical magnitude correspond a stream density a factor
1/sin2(
/2) greater than the wind's, simply from geometrical
arguments.
Finally, we anticipate that in wider binary systems, the dilution of the accretion stream through spatial expansion could lead to a progressive "switch-on'' of the importance of radiation and wind momenta, when and if the stream density becomes comparable to the standard wind density of the accreting star (as derived in single-star radiation-hydrodynamics simulations). This would offer an explanation for non-conservative mass transfer in wide massive binary systems.
Acknowledgements
All hydrodynamical simulations were performed on the basis of the ZEUS-2D code developed at the National Centre for Supercomputing Applications (NCSA) at the University of Urbana, Illinois. The authors wish to thank Stan Owocki for helpful discussions.