Xiang-Dong Li

ON THE FORMATION OF Be STARS THROUGH BINARY INTERACTION

Be stars are rapidly rotating B type stars. The origin of their rapid rotation is not certain, but binary interaction remains to be a possibility. In this work we investigate the formation of Be stars resulting from mass transfer in binaries in the Galaxy. We calculate the binary evolution with both stars evolving simultaneously and consider different possible mass accretion histories for the accretor. From the calculated results we obtain the critical mass ratios

A POPULATION OF ULTRALUMINOUS X-RAY SOURCES WITH AN ACCRETING NEUTRON STAR

q_{rm cr}

ON THE SPIN PERIOD DISTRIBUTION IN Be/X-Ray BINARIES

that determine the stability of mass transfer. We also numerically calculate the parameter

A STRANGE STAR SCENARIO FOR THE FORMATION OF ECCENTRIC MILLISECOND PULSAR/HELIUM WHITE DWARF BINARIES

lambda

FORMATION OF MILLISECOND PULSARS WITH LOW-MASS HELIUM WHITE DWARF COMPANIONS IN VERY COMPACT BINARIES

in common envelope evolution, and then incorporate both

Formation of Binary Millisecond Pulsars by Accretion-induced Collapse of White Dwarfs under Wind-driven Evolution

q_{rm cr}

EVOLUTION OF TRANSIENT LOW-MASS X-RAY BINARIES TO REDBACK MILLISECOND PULSARS

and

SUPER STRONG MAGNETIC FIELDS OF NEUTRON STARS IN BE X-RAY BINARIES ESTIMATED WITH NEW TORQUE AND MAGNETOSPHERE MODELS

lambda

On the White Dwarf Mass Problem of Cataclysmic Variables

into the population synthesis calculations. We present the predicted numbers and characteristics of Be stars in binary systems with different types of companions, including helium stars, white dwarfs, neutron stars, and black holes. We find that in Be/neutron star binaries the Be stars can have a lower limit of mass

The orbital period evolution of the supersoft X-ray source CAL 87

sim 8 M_{odot}