Survivor of Stellar Collision is New Type of Pulsating Star

 

A team of astronomers from the UK, Germany and Spain have observed the remnant of a stellar collision and discovered that its brightness varies in a way not seen before on this rare type of star. By analyzing the patterns in these brightness variations, astronomers will learn what really happens when stars collide. 

Artist’s impression of the eclipsing, pulsating binary star J0247-25. Image Credit: Keele University

Stars like our Sun expand and cool to become red giant stars when the hydrogen that fuels the nuclear fusion in their cores starts to run out. Many stars are born in binary systems so an expanding red giant star will sometimes collide with an orbiting companion star.   As much as 90% of the red giant star’s mass can be stripped off in a stellar collision, but the details of this process are not well understood. Only a few stars that have recently emerged from a stellar collision are known, so it has been difficult to study the connection between stellar collisions and the various exotic stellar systems they produce.

When an eclipsing binary system containing one such star turned up as a by-product of a search  for extrasolar planets, Dr Pierre Maxted and his colleagues decided to use the high-speed camera ULTRACAM* to study the eclipses of the star (J0247-25in detail. These new high-speed brightness measurements show that the remnant of the stripped red giant is a new type of pulsating star.

Many stars, including our own Sun, vary in brightness because of pulsations caused by sound waves bouncing around inside the star. For both the Sun and the new variable star, each pulsation cycle takes about 5 minutes. These pulsations can be used to study the properties of a star below its visible surface. Computer models produced by the discovery team show that the sound waves probe all the way to the center of the new pulsating star. Further observations of this star are now planned to work out how long it will be before the star starts to cool and fade to produce a stellar corpse (“white dwarf’”) of abnormally low mass.

The relative sizes of the stars are correctly shown relative to their separation. The timescales for the pulsations on both stars are correct relative to the orbital period of the binary, which is about 16 hours. We do not currently known the exact pulsation modes of the stars, so the pattern of the pulsations on the stars are arbitrary. The constrast of the image has been set to show the pulsations clearly, in reality the size of the variations is much more subtle that shown here. Image Credit: Keele University

Dr Pierre Maxted from Keele University, who led the study, said  “We have been able to find out a lot about these stars, such as how much they weigh, because they are in a binary system. This will really help us to interpret the pulsation signal and so figure out how these stars survived the collision and what will become of them over the next few billion years.”

This discovery has been published in the 27 June 2013 issue of the journal Nature.

Notes:

* ULTRACAM is a high-speed, 3-channel CCD camera for astrophysical research ULTRACAM was funded by PPARC and is a collaboration between, Professor Tom Marsh (University of Warwick) Professor Vik Dhillon (Sheffield) and the Astronomy Technology Centre (Edinburgh).

The observations were made using the 3.6-m New Technology Telescope at the European Southern Observatory (ESO).

Source: Keele University

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