Binary star systems are not rare.
Neither are systems where one star is a remnant like a white dwarf or neutron star, and its companion is on the main sequence.
In those systems, the dense remnant can draw material away from the main sequence star.
This can create violent Type 1a supernovae in the case of a white dwarf, and the emission of extremely powerful x-rays in the case of a neutron star.
In new research, astronomers observed the cataclysmic variable binary star V Sagittae (V Sge).
It’s extremely bright for its type, indicating that the accretor star is drawing an enormous amount of material from the donor, which gathers on the surface of the accretor before igniting and flaring brightly.
The research is “V Sge: Supersoft Source or Exotic Hot Binary? I. An X-Shooter campaign in the high state. The lead author is Pasi Hakala from the Finnish Centre for Astronomy with ESO.
V Sge has a main sequence star with about 3.3 solar masses, which is the donor star in the pair.
The other star is the accretor, and while astronomers thought it was a white dwarf for a long time, more recent observations suggest that it’s a Wolf-Rayet star, which are closely related to white dwarfs. V Sge is unusual and has puzzled astronomers for decades.
“V Sagittae is no ordinary star system – it’s the brightest of its kind and has baffled experts since it was first discovered in 1902,” said Professor Phil Charles from Southampton University, who was involved with the study.
“Our study shows that this extreme brightness is down to the white dwarf sucking the life out of its companion star, using the accreted matter to turn it into a blazing inferno. It’s a process so intense that it’s going thermonuclear on the white dwarf’s surface, shining like a beacon in the night sky.”
“The speed at which this doomed stellar system is lurching wildly, likely due to the extreme brightness, is a frantic sign of its imminent, violent end.” – Pasi Hakala, Finnish Centre for Astronomy with ESO
Its optical emissions are highly variable and extremely complex. Astrophysicists have struggled to interpret its characteristics, and they’ve been observing the star for a long time. However, the new observations in this work revealed a circumbinary ring that helps explain what’s going on.
The circumbinary ring wasn’t captured visually. The researchers gather spectra of V Sge with the X-Shooter, a powerful spectrograph on the ESO’s Very Large Telescope in Chile. The emission lines they observed, including the velocities they revealed, can’t be explained by the stars themselves.
“More importantly, (a) this feature does not vary with orbital phase, and (b) is centered at the systemic velocity, meaning that these emission features do not follow the motion of either stellar component,” the authors write. “We believe the only plausible explanation for this behaviour is that they originate from a circumbinary ring or disc of matter that has escaped the binary.”
To test their idea, the researchers took the spectra and modelled it. “Our simulations show that, as matter escapes from the WD’s Roche lobe, it forms a ring or rings around the binary, with a radius of roughly 2–4 binary separations,” the authors write. The Roche lobe is a region around a star or binary pair where gas and dust are gravitationally bound to the stars.
In order for the gas to form the ring, the accretor star must be drawing an extremely large amount of material from the donor star. Most of it flows to the accretor’s accretion disk, but not all. “This unexpected ring, formed from the debris of the messy feast, gives us a clue that could change what we know about how stars live and die,” said lead author Hakala in a press release.
“The white dwarf cannot consume all the mass being transferred from its hot star twin, so it creates this bright cosmic ring,” Hakala explained.
There’ve been several competing explanations for V Sge’s unusual features. Some researchers thought it was a pair of very hot stars, and that the brightness wasn’t a ring, but the result of hot winds from both stars colliding. But that can’t explain the system’s short-term or long-term variability, according to the authors. The authors think that the circumbinary disk best explains V Sge, and that the variability is due to “the chaotic behaviour of the inner accretion disc under intense irradiation,” they write.
They think the inner accretion disk around the accreting star has two tilt modes that it flips back and forth from chaotically. “The same tilt can then persist for an extended interval (from days to years) before the next “flipping” event takes place,” the authors explain.
“The speed at which this doomed stellar system is lurching wildly, likely due to the extreme brightness, is a frantic sign of its imminent, violent end,” Hakala explained.
Many of these types of binaries can be stable for billions of years, as long as the mass transfer between them is low and stable. In that case, the accretor star repeatedly gathers a layer of gas from the donor star on its surface. Eventually, when the mass builds up, it explodes as a nova, and the cycle can start again.
Study co-author Dr Rodríguez-Gil from Spain’s Instituto de Astrofisica de Canarias explained: “The matter accumulating on the white dwarf is likely to produce a nova outburst in the coming years, during which V Sagittae would become visible with the naked eye.” But the nova is just the beginning of the end.
In some of these binary arrangements, the stars eventually collide with one another. That can happen if the donor star evolves into a giant, making the system unstable and leading to a collision. A collision can also occur if the donor star becomes a white dwarf. In that case, the pair of stars could enter a common envelope and spiral into one another, eventually exploding.
“But when the two stars finally smash into each other and explode, this would be a supernova explosion so bright it’ll be visible from Earth even in the daytime,” Rodriguez-Gil concluded.
Written by Evan Gough/Universe Today.
