... To find , we must match the ram pressure of the accreting plasma with that caused by the relativistic wind or by the magnetosphere љ of the rotator (see Section 4.3 ). ...
... We will implicitly express the mass and radius of the star in solar units ( , ), time in million years ( yr), luminosities in units of erg s , wind velocities in units of cm s and accretion rates in units of M yr , unless other units are clearly indicated ...
... It is convenient to start with a situation in which the NS enters a binary system with a normal star losing matter in the form of a stellar wind. ...
... wind with constant velocity v against free-free absorption of the 430-MHz ... wind for a B1 star with bolometric luminosity 3 erg s is of the order of - yr ... wind rates cannot be a general property of all B-stars in MC, because this would ...
... initially rotates at a high enough speed to provide a powerful relativistic wind ... the pressures of plasma and relativistic wind must be matched at the surface of ...
... cases of non-conservative evolution (for example, stages with strong stellar wind or those where a loss of binary angular momentum occurs due to gravitational radiation or magnetic stellar wind) are treated using well-known prescriptions (see, e.g ...
... arxiv:0909.3843 Открытие пульсарной туманности около кандидата в магнитары AXP 1E1547.0-5408 (The discovery of a pulsar wind nebula around the magnetar candidate AXP 1E1547.0-5408) . ...
... Authors: B. A. Harmon et al. astro-ph/0404159 Зондирование релятивистских ветров в пульсаре PSRJ07370-3039 A и B (Probing Relativistic Winds: The case of PSRJ07370-3039 A & B) . ...