Data describe the evolution of a population of millisecond pulsars (MSPs) born from Accretion Induced Collapse. Data entries are comma-separated. The formation and subsequent evolution of 9194 MSPs have been modelled with code based on the BSE Code [see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000)]. For each MSP, the first row describes the magnetic field B (in Gauss) and the inclination angle (i, in radians) between magnetic & rotational axes. These quantities (B,i) do not evolve. Thus, every row containing only two entries indicates the beginning of the data covering a separate MSP.
For subsequent rows, there are seven entries in each row. The first entry in each row is the (discretised) time in units of Gyr since the star formation event when the MSP is formed. 0.1 is the minimum time possible time for which an MSP can be born. Subsequent discrete time steps are 0.1 Gyr. The last row for every MSP is for a time of 15.9 Gyr. Subsequent entries show (as a function of time) period (in s) period derivative dP/dt (s/s) NS mass (in units of solar masses) secondary mass (in units of solar masses) secondary type (for an explanation of secondary type label see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000). orbital separation

Data describe the evolution of a population of millisecond pulsars (MSPs) born from Accretion Induced Collapse. Data entries are comma-separated. The formation and subsequent evolution of 9194 MSPs have been modelled with code based on the BSE Code [see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000)]. For each MSP, the first row describes the magnetic field B (in Gauss) and the inclination angle (i, in radians) between magnetic & rotational axes. These quantities (B,i) do not evolve. Thus, every row containing only two entries indicates the beginning of the data covering a separate MSP.
For subsequent rows, there are seven entries in each row. The first entry in each row is the (discretised) time in units of Gyr since the star formation event when the MSP is formed. 0.1 is the minimum time possible time for which an MSP can be born. Subsequent discrete time steps are 0.1 Gyr. The last row for every MSP is for a time of 15.9 Gyr. Subsequent entries show (as a function of time) period (in s) period derivative dP/dt (s/s) NS mass (in units of solar masses) secondary mass (in units of solar masses) secondary type (for an explanation of secondary type label see Hurley, J. R., Pols, O. R. & Tout, C. A. Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity. Mon. Not. Roy. Astron. Soc. 315, 543–569 (2000). orbital separation