Evolution of massive binary black holes

1. Evolution of massive binary black holes Qingjuan Yu Princeton University July 21, 2002

2. Outline • Introduction • Evolution of massive binary black holes (BBHs) • Possible observational characteristics of surviving BBHs • Summary

3. Galactic center (Tremaine et al. 2002) NGC 4258 Quasar PKS 2349 (HST) M87 (HST) Introduction: Most galaxies house massive black holes (BHs) at their centers • suggested by QSO energetics and demography (e.g. Soltan 1982, Rees 1984) • observations: massive dark objects in nearby galactic centers (e.g. Kormendy & Richstone 1995, Magorrian et al. 1998)

4. Introduction: Questions • Is it possible that the massive BHs in some galactic centers are binary black holes (BBHs) (e.g. by galaxy mergers, Begelman, Blandford & Rees 1980) • How do BBHs evolve? (separation as a function of time) • Do BBHs merge or how long can they survive? (e.g. comparison with a Hubble time) • Orbital properties of surviving BBHs? Possible observational characteristics of surviving BBHs? (appropriate methods to probe BBHs?)

5. Introduction: Why interesting? • BBHs provide a laboratory to study BH physics. LISA: BBH mergers  gravitational waves test for gravitation theory or stimulus for new physics. BBH merger rates? • Understanding galaxy formation • the M• –and M• –L correlations  a close link between the formation and evolution of galaxies and their central BHs. (e.g. Tremaine et al. 2002) • a probe of the hierarchical model

6. Laser Interferometer Space Antenna (LISA)

7. Evolution of massive BBHs

8. Dynamical friction stage Dynamical friction 1010yr increasing 10kpc 10-5pc decreasing a Evolution of massive BBHs

9. 2. Non-hard binary stage 3. Hard binary stage Dynamical friction 1010yr three-body interactions with low-J stars; -1 (E: BBH energy) increasing (Heggie 1975) 10kpc 10-5pc decreasing a (Quinlan 1996) Evolution of massive BBHs bound dynamical friction (two-body interactions) and three-body interactions with stars passing in their vicinity

10. 4. Gravitational radiation stage Gravitational radiation Dynamical friction 1010yr increasing (Peters 1964) 10kpc 10-5pc decreasing a Evolution of massive BBHs

11. Gravitational radiation Gravitational radiation Dynamical friction 1010yr 1010yr increasing 10kpc 10-5pc decreasing a Dynamical friction increasing 10kpc 10-5pc decreasing a Evolution of massive BBHs • Main uncertainty is in the non-hard binary stage and the hard binary stage.. Are low-J stars depleted before the gravitational radiation stage? • Analogy: stellar tidal disruption rates around massive BHs. (e.g. Magorrian & Tremaine 1999). With the depletion of initial low- J stars, consider the refilling by two-body relaxation and tidal forces in the host galaxy. bottleneck

12. surviving BBHs merged BBHs increasing velocity dispersion increasing flattening surviving BBHs increasing triaxiality merged BBHs BBH evolution in realistic galaxy models (Yu 2002): • Sample: nearby early-type galaxies observed by HST (Faber et al. 1997) • Depends on BH masses, and velocity dispersions and shapes of host galaxies • small BHs (m2/m1<10-3) do not decay into galactic centers; • BBHs are more likely to have merged in low-dispersion galaxies and survive in high-dispersion galaxies; • BBHs are more likely to have merged in highly flattened or triaxial galaxies and survive in spherical and nearly spherical galaxies • Estimated orbital properties of surviving BBHs: • separation: 10-3 –10 pc

13. double nuclei (upper limit ~ HST resolution) bending or wiggling of jets (e.g. Blandford, Begelman, Rees 1980) double-peaked emission lines from broad line regions associated with BBHs in active galactic nuclei (AGNs) (Gaskell 1996) periodic behavior in the radio, optical, X-ray or -ray light curves (e.g. Valtaoja et al. 2000, Rieger & Mannheim 2000) broad asymmetric Iron K emission line shape from a two-accretion-disc system associated with a BBH (Yu & Lu 2001) Possible observational characteristics of surviving BBHs

14. Strongest lines of evidence for the existence of massive BHs Broad and asymmetric (Doppler and gravitational broadening) Short-term variability (~104s) Emitted from inner disc region Profiles are affected by the inclination between the observer and the disc. Two-accretion-disc system associated with a BBH with different spin axis directions Fe K lines: a tool to probe BBHs in AGNs? Fe K line profile (Yu & Lu 2001)

15. Summary • The orbital evolution of BBHs depends on the velocity dispersion and shape of the host galaxy, and on the masses of BHs. • BBHs are most likely to survive in spherical or nearly spherical and high-velocity dispersion galaxies. The upper limit of the separations of surviving BBHs is close to the HST resolution for the typical galaxies in the study. The absence of double nuclei in the centers of nearby galaxies does not mean that they have no BBHs. • If all galaxies are highly triaxial, there will be no surviving BBHs. • Possible observational characteristics of surviving BBHs (e.g. Iron K line profile from two accretion discs with different inclinations).