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Theoretical Studies of X-Ray Binaries in Clusters PowerPoint PPT Presentation


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Vicky Kalogera MODEST-6. Theoretical Studies of X-Ray Binaries in Clusters. ExtraGalactic only…. YOUNG. OLD. In this review:. Do IMBH in clusters form observable ULXs ? Do Super Star Clusters form High-Mass XRBs ? What is the role of SSCs in determining the

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Theoretical Studies of X-Ray Binaries in Clusters

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Vicky kalogera modest 6

Vicky Kalogera

MODEST-6

Theoretical Studies of X-Ray Binaries in Clusters

ExtraGalactic only…


In this review

YOUNG

OLD

In this review:

Do IMBH in clusters form observable ULXs ?

Do Super Star Clusters form High-Mass XRBs ?

What is the role of SSCs in determining the

X-ray luminosity functions of Starbursts ?

Do LMXBs in Ellipticals form in Globular Clusters

exclusively ?

Does the galactic field contribute at all ?

Why are red GCs better LMXB hosts than blueGCs?


Theoretical studies of x ray binaries in clusters

Do accreting IMBH in clusters form observable ULXs ?

Hopman, Portegies Zwart, Alexander 2004:YES

IMBH binary: through tidal capture (TC) of MS companions

ULX phase duration: > 10Myr

Blecha, Ivanova, Kalogera, et al. 2005: NOT LIKELY

IMBH binary: through exchanges with stellar binaries

ULX phase duration: < 0.1Myr


Theoretical studies of x ray binaries in clusters

Do accreting IMBH in clusters form observable ULXs ?

Hopman, Portegies Zwart, Alexander 2004:YES through TC

Most optimistic assumptions for TC survival of MS stars:

“hot squeezars” and ETC x Porb ~ LEdd

Analytical estimate of TC rate for 1,000Mo IMBH

for ANY orbital period

Mass Transfer and LX calculation for isolated

IMBH binaries with 5-15Mo MS donors

No dynamical interactions and evolution included

ULX phase duration per IMBH binary: >10Myr

Fraction of Clusters with IMBH-MS ULX: 30-50%


Theoretical studies of x ray binaries in clusters

Do accreting IMBH in clusters form observable ULXs ?

Blecha, Ivanova, Kalogera, et al. 2005: NOT LIKELY

Cluster coresimulations with full binary evolutionand

dynamical interactions: TC, exchanges, disruptions, collisions

(N. Ivanova’s talk from Monday’s morning session)

100-500Mo IMBH, 100Myr old clusters, Trc < 30Myr

Time fraction with IMBH binary: > 50%

Time fraction with Mass-Transfer: ~1-3%

MS donors dominate by time;

Post-MS donors dominate by number

Fraction of Mass-Transfer time as a ULX: ~2%

Average ULX phase duration per cluster: <0.1Myr


Theoretical studies of x ray binaries in clusters

IMBH Companions

Blecha, Ivanova, Kalogera, et al. 2005

Mass distribution

Orbital separation distribution


Theoretical studies of x ray binaries in clusters

Do Super Star Clusters form High-Mass XRBs ?

Distribution of point X-ray sources

Kaaret et al. 2004

  • Lx≥ (0.5-3)x1036 erg/s

< 1 XRB per cluster!


Theoretical studies of x ray binaries in clusters

N1569

50%

N5253

M82

Do Super Star Clusters form High-Mass XRBs ?

  • XRBs closely associated

    with star clusters

  • Median distance ~30-100 pc

Kaaret et al. 2004

Is this all due to

Supernova Kicks ?

  • Lx≥ 5x1035 erg/s

< 1 XRB per cluster!


Theoretical studies of x ray binaries in clusters

Do Super Star Clusters form High-Mass XRBs ?

Sepinsky, Kalogera, & Belczynski 2005

Models: Population Syntheses of XRBs and

Kinematic Orbit Evolution in Cluster Potential

  • cluster mass: ~5x104 Mo

  • LX > 5x1035 erg/s

  • average of 1,000 cluster

    simulations

  • Significant age dependence

  • < 1 XRB per cluster

1 10 100 1000

Distance from Cluster Center [pc]


Theoretical studies of x ray binaries in clusters

Do Super Star Clusters form High-Mass XRBs ?

YES!

XRB models without cluster dynamics appear

in agreement with observations

  • Mean XRB number per SSC < 1

    and spatial distribution:

    M < 105 Mo and 10-50Myr

    or more massive and ~50Myr

  • Supernova kicks: eject XRBs @ D > 10pc

    especially for M < 105 Mo


Theoretical studies of x ray binaries in clusters

LMXB origin in Ellipticals: Clusters and/or Field ?

Bildsten & Deloye 2004:NS Ultra-Compact Binaries from Clusters

Matches observed XLF slope below BREAK at ~5x1038 erg/s

Formation rate: 1/2Myr per 107Mo of GCs and this

matches cumulative #Ucs for continuous UC formation

due to dynamical interactions (Ivanova & Rasio 2004)

and observed #MSPc in Galactic GCs

prediction: search for orbital periods of 5-10min!

questions: MW has H-rich donors in GCs

what about above the BREAK ?


Theoretical studies of x ray binaries in clusters

LMXB origin in Ellipticals: Clusters and/or Field ?

Bildsten & Deloye 2004:NS Ultra-Compact Binaries from Clusters

Juett 2005:Ellipticals’ Field Must Contribute

Reason: Fraction of GC-LMXBs depends on SN

Issues with incompatible

coverage for definition of

fLMXB,GC and SN ?


Theoretical studies of x ray binaries in clusters

LMXB origin in Ellipticals: Clusters and/or Field ?

Bildsten & Deloye 2004:NS Ultra-Compact Binaries from Clusters

Juett 2005:Ellipticals’ Field Must Contribute

Reason: Fraction of GC-LMXBs depends on SN

Irwin 2005:Ellipticals’ Field Must Contribute

Reason: non-zero y-intercept of

LX/LB vs. SN (ASN+B, B<>0 @8s)

Not due to:

large-scale GC disruption

or

variations in red/blue GC ratio


Theoretical studies of x ray binaries in clusters

LMXB origin in Ellipticals: Clusters and/or Field ?

Bildsten & Deloye 2004:NS Ultra-Compact Binaries from Clusters

Juett 2005:Ellipticals’ Field Must Contribute

Irwin 2005:Ellipticals’ Field Must Contribute

Ivanova & Kalogera 2005: Brightest are BH LMXBs from Field

Sources with 5x1038 < LX < fewx1039 erg/s too bright for NS accretor

BH LMXBs not expected in GCs,(Kalogera, King, & Rasio 2004)

but are expected in the Field as BH transients

If Loutburst ~ Ledd :

XLF slope above BREAK is a

footprint of BH mass spectrum

Current Lmax ~ 2x1039 erg/s

implies max BH mass of 15-20Mo

consistent with stellar evolution


Theoretical studies of x ray binaries in clusters

LMXB origin in Ellipticals: Clusters and/or Field ?

Bildsten & Deloye 2004:NS Ultra-Compact Binaries from Clusters

Juett 2005:Ellipticals’ Field Must Contribute

Irwin 2005:Ellipticals’ Field Must Contribute

Ivanova & Kalogera 2005: Brightest are BH LMXBs from Field

Consistent answer appears to be: Both Clusters & Field

BUT: Irwin considers sources below the BREAK: mixed

Juett considers all sources: mixed

B&D can explain all sources below the BREAK

as coming from Clusters

I&K agree (based on pop-syn models) and

propose Field contribution only for

sources above the BREAK …


Theoretical studies of x ray binaries in clusters

Why are Red Clusters more likely (by ~3)

to host LMXBs than Blue Clusters?

Maccarone, Kundu, & Zepf 2004:

Z-dependence of Irradiation-Induced Winds

In Blue, Metal-Poor GCs donors have stronger IIWs (less line-cooling)

---> shorter LMXB lifetimes ---> lower LMXB numbers

Number ratio comes to 2.5-3.5!

Also accounts for:

harder LMXB spectra in Blue, Metal-Poor Clusters

Prediction:

Should see monotonic # dependence on Z

And account for LMC vs. MW observations


Theoretical studies of x ray binaries in clusters

Why are Red Clusters more likely (by ~3)

to host LMXBs than Blue Clusters?

Maccarone, Kundu, & Zepf 2004:

Z-dependence of Irradiation-Induced Winds

Ivanova 2005: Z-dependence of Magnetic Braking A.M. Loss

In Blue, Metal-poor GCs MS donors w/ 0.85-1.25Mo have

no outer convective zone ---> no MB ---> harder to start MT

Even if MT starts, NS-MS LMXBs are transients (hard to detect)

NS-MS LMXBs in Red, Metal-rich GCs are easier to form and

have some bright phase

Estimate of formation rate of

Bright NS-MS LMXBs in

Metal-Rich GCs agrees with obs.


Theoretical studies of x ray binaries in clusters

Why are Red Clusters more likely (by ~3)

to host LMXBs than Blue Clusters?

Maccarone, Kundu, & Zepf 2004:

Z-dependence of Irradiation-Induced Winds

Ivanova 2005: Z-dependence of Magnetic Braking A.M. Loss

Not clear (to me!) which of the two is more realistic

Any thoughts ?

Both deal with NS-LMXBs and MS donors -

How are these connected to B&D results about

NS Ultra-compacts with WD companions ?


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