FORMATION OF PLANETS AROUND PULSARS

Pulse arrival-time delays PSR 1257+12 suggest the existence of at leas t two planets in nearly circular orbits around it. In this paper we di scuss different scenarios for the formation of planets in circular orb its around pulsars. Among other topics, we look in some detail at wind emission mechanisms that are particularly relevant to the process of evaporation of planets around pulsars and discuss their possible role in orbit circularization. We conclude that the formation of such plane ts may occur in a very late phase of low-mass X-ray binary (LMXB) or b inary millisecond pulsar (BMP) evolution. Evaporation of the companion star in these phases supplies matter to a circumbinary ''excretion'' disk in which the physical conditions, similar to those appropriate fo r the BMP 1957+20 system, may allow the formation of planets like thos e observed in PSR 1257+12.