Vicky Kalogera Jeremy Sepinsky with Krzysztof Belczynski X-Ray Binaries and and Super-Star Clusters Super-Star Clusters

Super-Star Clusters (SSCs) Compact, young analog to globular clusters Occur frequently in starburst environments Masses range from ~10 4 to ~10 7 M o Ages range from a few to tens of Myr

: candidate SSCs x : Chandra point X-ray sources XRB and SSC observations: Kaaret et al NIC2/NIC3 IR image of M82

Kaaret et al L x ≥ (0.5-3)x10 36 erg/s Distribution of X-Ray point sources < 1 XRB per cluster!

Kaaret et al L x ≥ 5x10 35 erg/s Distribution of X-Ray point sources XRBs closely associated with star clusters Median distance ~ pc < 1 XRB per cluster! M82 N5253 N % Supernova Kicks and/or Cluster Dynamics ?

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Asymmetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations (1) XRB Population Syntheses

StarTrack code (Belczynski et al and 2004) Tracks evolution of binaries and single stars (Hurley et al.) Detailed calculations of mass transfer rate Integrated tidal evolution Assymetric core collapse and mass range for NS / BH Angular momentum and mass losses Calibrated against open-cluster and XRB observations and mass transfer calculations and mass transfer calculations (1) XRB Population Syntheses

(2) Orbital Evolution in SSCs Isolated XRBs evolved in a static Plummer potential > self-consistent initial positions and velocities Position, X-Ray Luminosity, and Evolutionary Status are simultaneously tracked through 200 Myr Dynamical interactions and an evolving cluster potential are NOT included!

(2) Orbital Evolution in SSCs Isolated XRBs evolved in a static Plummer potential > self-consistent initial positions and velocities Position, X-Ray Luminosity, and Evolutionary Status Position, X-Ray Luminosity, and Evolutionary Status are simultaneously tracked through 200 Myr are simultaneously tracked through 200 Myr Dynamical interactions and an evolving cluster potential are NOT included!

(2) Orbital Evolution in SSCs Isolated XRBs evolved in a static Plummer potential > self-consistent initial positions and velocities Position, X-Ray Luminosity, and Evolutionary Status are simultaneously tracked through 200 Myr Dynamical interactions and an evolving cluster potential are NOT included!

Present Calculations  Low-mass clusters require a large number of MC realizations to address statistical effects: 2,000for ~5x10 4 M o 1,000 with f(m)  m ,000with f(m)  m for~5x10 5 M o 10for ~5x10 6 M o  Binaries evolved for 200 Myr  Half-mass radius set to 10pc  Binary fraction set to 100% (N XRB : upper limits)

Theoretical XRB Distributions cluster mass: ~5x10 4 M o L X > 5x10 35 erg/s average of 1,000 clusters Significant age dependence < 1 XRB per cluster

More Massive Clusters cluster mass: ~5x10 5 M o L X > 5x10 35 erg/s average of 100 clusters Similar age dependence Mean XRB number /cluster ~ cluster mass

Conclusions XRB models without cluster dynamics appear in agreement with observations Mean XRB number per SSC < 1 and spatial distribution: M < 10 5 M o and 10-50Myr or more massive and ~50Myr Supernova kicks: eject D > 10pc especially for M < 10 5 M o Results do not appear sensitive to binary evolution assumptions, but extended parameter study is needed. Explore role of dynamics