On a Theoretical Interpretation of the Period Gap in Binary Millisecond Pulsars

Details On a Theoretical Interpretation of the Period Gap in Binary Millisecond Pulsars On a Theoretical Interpretation of the Period Gap in Binary Millisecond Pulsars

2000-07-05

arxiv.org/abs/astro-ph/0007055v1

Astronomy and Astrophysics

Astrophysics

20 pages, one encapsulated figure, LaTeX, accepted by ApJ

Scientific paper

10.1086/309392

We reexamine evolutionary channels for the formation of binary millisecond pulsars in order to understand their observed orbital period distribution. The available paths provide a natural division into systems characterized by long orbital periods (> 60 d) and short orbital periods (< 30 d). Systems with initial periods 1 - 2 d ultimately produce low mass He white dwarfs with short orbital periods (< 1 d). For longer initial periods (> few days), early massive Case B evolution produces CO white dwarfs with orbital periods < 20 d. Common envelope evolution result in short period systems (P < 1 d) from unstable low mass Case B evolution producing He white dwarfs, and from unstable Case C evolution leading to CO white dwarfs. On the other hand, the long orbital period group arises from stable low mass Case B evolution with initial periods > few days producing low mass He white dwarfs and periods > 30 d, and from stable Case C evolution producing CO white dwarfs. The lack of observed systems between 23 and 56 days probably reflects the fact that for comparable initial orbital periods (< few days) low mass Case B and early massive Case B evolution lead to very discrepant final periods. We show in particular that the lower limit (~ 23 d) cannot result from common-envelope evolution.

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