Formation and Evolution of Contact Binaries

• Main Author: Peter P. Eggleton
• Format: Article
• Language: English
• Published: Korean Space Science Society (KSSS) 2012-06-01
• Series: Journal of Astronomy and Space Sciences
• Subjects: binaries; stars: evolution
• Online Access: http://ocean.kisti.re.kr/downfile/volume/kosss/OJOOBS/2012/v29n2/OJOOBS_2012_v29n2_145.pdf

describe a series of processes, including hierarchical fragmentation, gravitational scattering, Kozai cycles within triple systems, tidal friction and magnetic braking, that I believe are responsible for producing the modest but significant fraction of stars that are observed as contact binaries. I also discuss further processes, namely heat transport, mass transport, nuclear evolution, thermal relaxation oscillations, and further magnetic braking with tidal friction, that influence the evolution during contact. The endpoint, for contact, is that the two components merge into a single star, as recently was observed in the remarkable system V1309 Sco. The single star probably throws off some mass and rotates rapidly at first, and then slows by magnetic braking to become a rather inconspicuous but normal dwarf or subgiant. If however the contact binary was part of a triple system originally–as I suggested above was rather likely–then the result could be a widish binary with apparently non-coeval components. There are several such known.