A&A 370, 1026-1029 (2001)
DOI: 10.1051/0004-6361:20010335
Research Note
C. Lloyd - D. J. Stickland
Space Science & Technology Department, Rutherford Appleton
Laboratory, Chilton, Didcot,
Oxon. OX11 0QX, UK
Received 22 December 2000 / Accepted 2 March 2001
Abstract
An analysis of the
Hipparcos photometry of HD 115071 shows that it is an
ellipsoidal variable with a period of 2.73126 days, twice that suggested
previously. Modelling the light curve combined with the available radial
velocities suggests that the more massive, hotter component is smaller and
less luminous than the cooler component, which is probably filling its
Roche lobe. The likely age of the system indicates that it is a MS
+ MS blue straggler, created by Case A mass exchange.
Key words: stars: binaries: spectroscopic - stars: blue stragglers -
stars: early-type - stars: evolution -
stars: variable: general
HD 115071 lies some 15
west of Stock 16, towards
Cen OB1, against a background of more distant stars.
HD 115071 is regarded as part of the wider population of Cen OB1 although
its spatial separation and distance modulus
place it rather closer to the Stock 16/RCW 75 complex than Cen OB1
(
and 11.78, respectively, Turner
1985; Kaltcheva & Georgiev
1994). On the HR diagram of stars within 30
of Stock 16,
HD 115071 lies at the top of the zero-age main sequence (ZAMS), together
with some of the other members of the wider Cen OB1 population, and the
brightest members of the cluster proper (Turner 1985).
Despite its brightness, and that it has been known as a radial-velocity variable for many years, HD 115071 has been particularly neglected, and still does not have a published orbit. One velocity has been published by Conti et al. (1977) and the single IUE spectrum, which reveals the system to be double lined, has been discussed repeatedly (Howarth et al. 1997; Penny 1996; Stickland & Lloyd 2001).
Although it is clearly impossible to derive an orbit from two epochs, the velocities, particularly those from IUE, do provide very useful constraints on the system. The radial velocities of the components have been determined from the single IUE spectrum using a cross-correlation technique, which has been applied in a series of papers on early-type binaries observed with IUE, most recently by Stickland & Lloyd (2001). A detailed description of the method, the sections of spectrum used, and the reliability of the results is given by Stickland (1998). In essence the binary spectrum is cross correlated against a standard star of the appropriate spectral type and the velocities are determined from the peaks of the cross-correlation function (CCF). The velocities are placed on a near-absolute footing by cross correlating the interstellar spectrum of the target star against the standard. The CCF of HD 115071 with the O9 V standard (HD 57682) is shown in Fig. 1 and two quite well-resolved components and a possible weak third component can be seen. The best correlation with the brighter component occurs with the O9 V standard, and this is consistent with the spectral type given by Walborn (1973). However, for the slightly fainter component the correlation improves with standards of slightly earlier spectral type, such as HD 91824 (O7 V((n)) ). Direct examination of the IUE spectrum suggests that both components are unevolved, late O-type stars with no obvious nitrogen enhancement. The interstellar velocity of HD 115071 is unknown but nearby stars, HD 114886 and HD 115455, have interstellar velocities from the Ca II K line of -17 km s-1 and -19 km s-1 respectively (Crampton 1976), and the latter has been assumed to place the IUE velocities on an absolute scale. Other stars in the area observed in the CH and CH+ molecular lines show similar velocities (Grendel 1997).
The systemic velocity of HD 115071 is also unknown and a value has been
assumed based on the local stellar and interstellar velocities. The
velocities of other stars in the area are very similar to the
interstellar velocity. For example, the mean velocity of 15 stars in Cen
OB1 from Humphreys (1978) is
km s-1. A
systemic velocity for HD 115071
-30 km s-1 would yield a
mass ratio,
,
which seems unlikely given the difference in
spectral type of the components. It is more likely to lie in the range
-20 to -10 km s-1 giving the mass ratio in the range
0.77 < q
< 0.90, making the hotter star (with the slightly weaker CCF) the more
massive of the pair.
![]() |
Figure 1: Cross-correlation function of the IUE spectrum |
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The CCF method also provides a measure of the
of the components
and these, together with the radial velocities, are given in
Table 1. The values of
found here are
about 10% and 25% larger than those of Penny (1996) and Howarth
et al. (1997) respectively. All three sets show the brighter
component as consistently broader than the fainter component. Conti &
Ebbets (1977) also give a value of the projected rotational
velocity, presumably from the same plate that provided the velocity in
the Conti et al. (1977) paper, of
km s-1.
Their value is approximately twice that of the broader star because it
includes the velocity separation of the components in the unresolved
profile. See below and Fig. 3.
JD | Primary | Secondary | |
Velocity (km s-1) | 2444487.4713 | +101 | -155 |
![]() |
133 | 148 |
In the Hipparcos Catalogue (Perryman et al. 1997)
HD 115071 is given as a sinusoidal variable, with P = 1.36 days and a
comment that it could be twice this value. For the types of stars
involved it is more likely that the light curve is due to ellipsoidal
variations with twice this period. A least squares fit to the data gives
slightly smaller residuals than the sinusoidal fit and provides the
ephemeris of primary minimum
![]() |
Figure 2: The Hipparcos light curve of HD 115071 with the photometric solution over plotted |
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The velocities are shown in Fig. 3, together with the
orbital solutions, assuming
km s-1. The velocity
from Conti et al. shows only a single, broad line and although it falls
close to single-line phase on the diagram, the velocity separation of the
components is
150 km s-1. Combined with the
s of
the components the velocity separation would produce a single unresolved line with a width of
280 km s-1, as seen by Conti & Ebbets.
Both the spectroscopic and photometric evidence point to the hotter component being more massive, yet smaller and fainter than the cooler component. Despite the main-sequence classification, the relative sizes of the stars mean that it is impossible for both stars to lie on the main sequence. There are probably only two possible ways to resolve this problem. Either the cooler component is the evolved member of a mass-exchange binary or it is still contracting onto the main sequence.
The age of HD 115071 is not directly known so, until reliable stellar parameters become available that can be compared with stellar evolution models, a less direct approach will have to be adopted. It seems unlikely that HD 115071 is strictly a member of Stock 16. It lies some distance from the cluster and, being a massive binary in its own right, is unlikely to have been ejected by gravitational interactions with other cluster members. The most likely interpretation is that HD 115071 is a product of the previous generation of star formation in this region, which makes it at least as old as the brightest and most massive star in Stock 16, HD 115455, and is unlikely to have one component still contracting onto the main sequence. The position of HD 115071 at the top of the ZAMS in the HR diagram of local stars is exactly what would be expected if it were a blue straggler, belonging to a slightly older population.
While most blue stragglers have spectral types of A or F (Ahumada & Lapasset 1995), early-type blue stragglers do occur but are comparatively rare, and approximately half of them have spectral anomalies (Mermilliod 1982). According to Monte Carlo simulations by Pols & Marinus (1994), blue stragglers produced by mass exchange in close binaries come in five types; MS star plus helium star, white dwarf or neutron star, MS plus MS stars, or merged MS star. The main sequence pairs are produced by Case A mass transfer (Pols 1994) and this seems the most likely origin of HD 115071, although there do not appear to be any spectral anomalies.
![]() |
Figure 3: The velocities of HD 115071 from Conti et al. (square) and IUE (circles), with the adopted orbital solution over plotted. The phases are photometric |
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The present mass of the system is unlikely to exceed 45 ,
so if
one third of the mass was lost from the system during transfer, the
initial total mass could have been
70
,
with
and q < 0.4. Such a massive star would very quickly evolve
into a Wolf-Rayet star, even without any mass transfer, but this has
clearly not happened. Therefore, the initial mass of the primary, the
total mass of the system, and probably the mass lost from the system must
have been less extreme.
As the system contains two apparently relatively
normal stars, it suggests that mass transfer took place before the initial
primary had evolved significantly, which points to Case A mass transfer.
The slow growth in radius during the main-sequence evolution of the
initial primary and, presumably, smooth mass transfer could have led to
little mass being lost from the system.
Without detailed modelling and a reliable age it is impossible to be
precise about the evolutionary stage of the system, although if the
cooler star does fill its Roche lobe, mass transfer may still be
occurring, or may have only recently ceased. Also, within the
uncertainties, the system is probably rotationally locked. For
synchronous rotation the components would have s of 113 and 142
km s-1 respectively, which are comparable with the values given in
Table 1, discussed in
Sect. 2.
HD 115071 lies at a similar distance to Stock 16, which is given by Turner
(1985) as
kpc, with a reddening of
EB-V
= 0.46. Combined with the visual magnitude, and assuming AV=3.0,
this gives an absolute magnitude of
MV=-4.8 for the system. For
two equal components this gives
MV=-4.1 individually, which is
entirely consistent with the expected luminosity of two late O-type
stars.
HD 115071 is an ellipsoidal variable, probably containing stars of spectral types O7-8 V and O9 IV. The primary is the hotter, more massive, but smaller and less luminous component. The system has undergone mass exchange, probably conservative Case A, and the present secondary is probably filling its Roche lobe.