In simple models of binary-star interaction, it is usually assumed that both the total mass and the orbital angular momentum are conserved. This simple model actually works quite well for many binaries. But it is clear that angular momentum can be lost, by magnetic stellar winds, and that mass can also be lost by this process.
I have developed a model of mass and angular momentum loss by dynamo activity -- as in the Solar dynamo, which both drives the Solar wind and causes the Sun to rotate slowly. I am attempting to apply it, along with a model of tidal friction, to all of the following kinds of system: (i) BY Dra binaries, (ii) RS CVn binaries, (iii) cool Algols, (iv) cataclysmic variables, (v) low-mass X-ray binaries, and (vi) contact binaries. Preliminary results will be presented, which suggest that in several of these kinds of system mass loss may be just as important as angular momentum loss.
Tuesday, December 2nd
Seminar is to be held at 4:00 PM in the conference room
on the second floor of Dearborn Observatory
Refreshments will be served at 3:30
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