ar X iv : a st ro - p h / 04 10 51 6 v 2 2 8 O ct 2 00 4 1 WEIGHING STELLAR – MASS BLACK HOLES WITH GAIA

ar X iv : a st ro - p h / 01 10 17 6 v 1 8 O ct 2 00 1 WHY NS AND BH MASS DISTRIBUTION IS BIMODAL ?

The observed mass distribution for the compact remnants of massive stars (neutron stars and black holes) and its relationship to possible mechanisms for the ejection of the envelopes of type II and Ib/c supernovae is analyzed. The conclusion is drawn that this distribution can be obtained only by a magneto-rotational mechanism for the supernovae with sufficiently long time of the field amplific...

ar X iv : a st ro - p h / 98 10 37 9 v 1 2 3 O ct 1 99 8 Supermassive Black Holes Then and Now ∗

Recent surveys suggest that most or all normal galaxies host a massive black hole with 1/100 to 1/1000 of the visible mass of the spheroid of the galaxy. Various lines of argument suggest that these galaxies have merged at least once in our past lightcone, and that the black holes have also merged. This leads to a merger rate of massive black holes of about 1/yrs.

ar X iv : a st ro - p h / 02 10 42 8 v 1 1 8 O ct 2 00 2 Star Clusters in Interacting Galaxies : The Case of M 51 Nate

ar X iv : a st ro - p h / 01 12 42 3 v 1 1 8 D ec 2 00 1 The black hole mass of BL Lacs from stellar velocity dispersion of the host galaxy

The black hole mass of BL Lacs from stellar velocity dispersion of the host galaxy.

ar X iv : a st ro - p h / 02 01 11 4 v 1 8 J an 2 00 2 Binary coalescence of a strange star with a black hole : Newtonian results .

We present Newtonian three–dimensional hydrodynamical simulations of the merger of quark stars with black holes. The initial conditions correspond to non-spinning stars in Keplerian orbits, the code includes gravitational radiation reaction in the quadrupole approximation for point masses. We find that the quark star is disrupted, forming transient accretion structures around the black hole, bu...