Extreme mass ratio inspiral

Artist impression of the spacetime generated by an extreme mass ratio inspiral.

In astrophysics, an extreme mass ratio inspiral (EMRI) is the orbit of a relatively lighter object around a much heavier (by a factor 10,000 or more) object, that gradually decays due the emission of gravitational waves. Such systems are likely to be found in the centers of galaxies, where stellar mass compact objects, such as stellar black holes and neutron stars, may be found orbiting a supermassive black hole.[1] In the case of a black hole in orbit around another black hole this is an extreme mass ratio binary black hole. The term EMRI may be used as a shorthand to denote the emitted gravitational waveform as well as the orbit itself.

The main reason for scientific interest in EMRIs is that they are one of the most promising sources for gravitational wave astronomy using future space-based detectors such as the evolved Laser Interferometer Space Antenna (eLISA).[2] If such signals are successfully detected, they will allow accurate measurements of the mass and angular momentum of the central object, which in turn gives crucial input for models for the formation and evolution of supermassive black holes.[3] Moreover, the gravitational wave signal provides a detailed map of the spacetime geometry surrounding the central object, allowing unprecedented tests of the predictions of general relativity in the strong gravity regime.[4]

Overview

Scientific potential

Characteristic strain of EMRI signals as a function of frequency. They lie in the sensitive band for space-borne detectors like LISA or eLISA, but outside the band for ground-based detectors like advanced LIGO (aLIGO) or pulsar timing arrays such as the European Pulsar Timing Array (EPTA).[5]

If successfully detected, the gravitational wave signal from an EMRI will carry a wealth of astrophysical data. EMRIs evolve slowly and complete many (~10,000) cycles before eventually plunging.[6] Therefore, the gravitational wave signal encodes a precise map of the spacetime geometry of the supermassive black hole.[7] Consequently, the signal can be used as an accurate test of the predictions of general relativity in the regime of strong gravity; a regime in which general relativity is completely untested. In particular, it is possible to test the hypothesis that the central object is indeed a supermassive black hole to high accuracy by measuring the quadrupole moment of the gravitational field to an accuracy of a fraction of a percent.[1]

In addition, each observation of an EMRI system will allow an accurate determination of the parameters of the system, including:[8]

Formation

It is currently thought that the centers of most (large) galaxies consist of a supermassive black hole of 106 to 109 solar masses (M☉) surrounded by a cluster of 107 to 108 stars maybe 10 light-years across, called the nucleus.[3] The orbits of the objects around the central supermassive black hole are continually perturbed by two-body interactions with other objects in the nucleus, changing the shape of the orbit. Occasionally, an object may pass close enough to the central supermassive black hole for its orbit to produce large amounts of gravitational waves, significantly affecting the orbit. Under specific conditions such an orbit may become an EMRI.[3]

In order to become an EMRI, the back-reaction from the emission of gravitational waves must be the dominant correction to the orbit (compared to, for example, two-body interactions). This requires that the orbiting objects passes very close the central supermassive black hole. A consequence of this is that the inspiralling object cannot be a large heavy star, because it will be ripped apart by the tidal forces.[3]

However, if the object passes too close to the central supermassive black hole, it will make a direct plunge across the event horizon. This will produce a brief violent burst of gravitational radiation which would be hard to detect with currently planned observatories.[nb 1] Consequently, the creation of EMRI requires a fine balance between objects passing too close and too far from the central supermassive black hole. Currently, the best estimates are that a typical supermassive black hole of 106 M☉, will capture an EMRI once every 106 to 108 years. This makes witnessing such an event in our Milky Way unlikely. However, a space based gravitational wave observatory like LISA will be able to detect EMRI events up to cosmological distances, leading to an expected detection rate somewhere between a few and a few thousand per year.[1]

Extreme mass ratio inspirals created in this way tend to have very large eccentricities (e > 0.9999). The initial, high eccentricity orbits may also be a source of gravitational waves, emitting a short burst as the compact object passes through periapsis. These gravitational wave signals are known as extreme mass ratio bursts.[10] As the orbit shrinks due the emission of gravitational waves, it becomes more circular. When it has shrunk enough for the gravitational waves to become strong and frequent enough to be continuously detectable by LISA, the eccentricity will typically be around 0.7. Since the distribution of objects in the nucleus is expected to be approximately spherically symmetric, there is expected to be no correlation between the initial plane of the inspiral and the spin of the central supermassive black holes.[1]

In 2011, an important impediment to the formation of EMRIs was discovered.[11] The "Schwarzschild Barrier" is an upper limit to the eccentricity of orbits near a supermassive black hole. Gravitational scattering is driven by torques from the slightly asymmetric distribution of mass in the nucleus ("resonant relaxation"), resulting in a random walk in each star's eccentricity.[12] When its eccentricity becomes sufficiently large, the orbit begins to undergo relativistic precession, and the effectiveness of the torques is quenched. There is a critical eccentricity, at each value of the semi-major axis, at which stars are "reflected" back to lower eccentricities. Barrier penetration can occur, but the rate of production of EMRIs is much lower than would be expected in the absence of the barrier.[11] Estimates of the EMRI rate made prior to 2011[1] ignored this effect.[3]

Two years later, however, it was realised that the role of the spin of the central supermassive black hole in this matter may be crucial. For a long time it has been believed that any EMRI originating farther away than a certain critical radius of about a hundredth of a parsec would be either scattered away from the capture orbit or directly plunge into the supermassive black hole on an extremely radial orbit. These events would lead to one or a few bursts, but not to a coherent set of thousands of them. Indeed, when taking into account the spin, [13] proved that these capture orbits do not plunge, but accumulate thousands of cycles in the detector band. Since they are driven by two-body relaxation, which is chaotic in nature, they are ignorant of the Schwarzchild barrier and are not blocked. Moreover, since they originate in the bulk of the stellar distribution, the rates are larger. Additionally, due to their larger eccentricity, they are louder, which enhances the detection volume. It is therefore expected that EMRIs originate at these distances, and that they dominate the rates, contrary to EMRIs originating from within a hundredth of a parsec, which are blocked.

Alternatives

Several alternative processes for the production of extreme mass ratio inspirals are known. One possibility would be for the central supermassive black hole to capture a passing object that is not bound to it. However, the window where the object passes close enough to the central black hole to be captured, but far enough to avoid plunging directly into it is extremely small, making it unlikely that such event contribute significantly to the expected event rate.[1]

Another possibility is present if the compact object occurs in a bound binary system with another object. If such a system passes close enough to the central supermassive black hole it is separated by the tidal forces, ejecting one of the objects from the nucleus at a high velocity while the other is captured by the central black hole with a relatively high probability of becoming an EMRI. If more than 1% of the compact objects in the nucleus is found in binaries this process may compete with the "standard" picture described above. EMRIs produced by this process typically have a low eccentricity, becoming very nearly circular by the time they are detectable by LISA.[1]

A third option is that a giant star passes close enough to the central massive black hole for the outer layers to be stripped away by tidal forces, after which the remaining core may become an EMRI. However, it is uncertain if the coupling between the core and outer layers of giant stars is strong enough for stripping to have a significant enough effect on the orbit of the core.[1]

Finally, supermassive black holes are often accompanied by an accretion disc of matter spiraling towards the black hole. If this disc contains enough matter, instabilities can collapse to form new stars. If massive enough, these can collapse to form compact objects, which are automatically on a trajectory to become an EMRI. Extreme mass ratio inspirals created in this way are characterized by the fact their orbital plane is strongly correlated with the plane of the accretion disc and the spin of the supermassive black hole.[1]

Intermediate mass ratio inspirals

Besides stellar black holes and supermassive black holes, it is speculated that a third class of intermediate mass black holes with masses between 102 and 104 M☉ also exists.[3] One way that these may possibly form is through a runway series of collisions of stars in a young cluster of stars. If such a cluster forms within a thousand light years from the galactic nucleus, it will sink towards the center due to dynamical friction. Once close enough the stars are stripped away through tidal forces and the intermediate mass black hole may continue on an inspiral towards the central supermassive black hole. Such a system with a mass ratio around 1000 is known as an intermediate mass ratio inspiral (IMRI). There are many uncertainties in the expected frequency for such events, but some calculations suggest there may be up to several tens of these events detectable by LISA per year. If these events do occur, they will result in an extremely strong gravitational wave signal, that can easily be detected.[1]

Another possible way for an intermediate mass ratio inspiral is for an intermediate mass black hole in a globular cluster to capture a stellar mass compact object through one of the processes described above. Since the central object is much smaller, these systems will produce gravitational waves with a much higher frequency, opening the possibility of detecting them with the next generation of Earth-based observatories, such as Advanced LIGO and Advanced VIRGO. Although the event rates for these systems are extremely uncertain, some calculations suggest that Advanced LIGO may see several of them per year.[14]

Modelling

Diagram show the relationship between various approaches to modelling extreme mass ratio inspirals.

Although the strongest gravitational wave from EMRIs may easily be distinguished from the instrumental noise of the gravitational wave detector, most signals will be deeply buried in the instrumental noise. However, since an EMRI will go through many cycles of gravitational waves (~105) before making the plunge into the central supermassive black hole, it should still be possible to extract the signal using matched filtering. In this process, the observed signal is compared with a template of the expected signal, amplifying components that are similar to the theoretical template. To be effective this requires accurate theoretical predictions for the wave forms of the gravitational waves produced by an extreme mass ratio inspiral. This, in turn, requires accurate modelling of the trajectory of the EMRI.[1]

The equations of motion in general relativity are notoriously hard to solve analytically. Consequently, one needs to use some sort of approximation scheme. Extreme mass ratio inspirals are well suited for this, as the mass of the compact object is much smaller than that of the central supermassive black hole. This allows it to be ignored or treated perturbatively.[15]

Post-Newtonian expansion

One common approach is to expand the equations of motion for an object in terms of its velocity divided by the speed of light, v/c. This approximation is very effective if the velocity is very small, but becomes rather inaccurate if v/c becomes larger than about 0.3. For binary systems of comparable mass, this limit is not reached until the last few cycles of the orbit. EMRIs, however, spend their last thousand to a million cycles in this regime, making the post-Newtonian expansion an inappropriate tool.[1]

Numerical relativity

Main article: numerical relativity

Another approach is to completely solve the equations of motion numerically. The non-linear nature of the theory makes this very challenging, but significant success has been achieved in numerically modelling the final phase of the inspiral of binaries of comparable mass. The large number of cycles of an EMRI make the purely numerical approach prohibitively expensive in terms of computing time.[1]

Gravitational self force

The large value of the mass ratio in an EMRI opens another avenue for approximation: expansion in one over the mass ratio. To zeroth order, the path of the lighter object will be a geodesic in the Kerr spacetime of the supermassive black hole. Corrections due to the finite size of the mass of the lighter object can then be included, order-by-order in the mass ratio, as an effective force on the object. This effective force is known as the gravitational self force.[1]

In the last decade or so, a lot of progress has been made in calculating the gravitational self force for EMRIs. Numerical codes are available to calculate the gravitational self force on any bound orbit around a non-rotating (Schwarzschild) black hole.[16] And significant progress has been made for calculating the gravitational self force around a rotating black hole.[17]

Notes

  1. ↑ LISA will only have a small chance of detecting such signals if it originates from our Milky Way.[1]

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 Amaro-Seoane, Pau; Gair, Jonathan R.; Freitag, Marc; Miller, M. Coleman; Mandel, Ilya; Cutler, Curt J.; Babak, Stanislav (2007). "Intermediate and Extreme Mass-Ratio Inspirals -- Astrophysics, Science Applications and Detection using LISA". Classical and Quantum Gravity. 24 (17): R113–R169. arXiv:astro-ph/0703495Freely accessible. Bibcode:2007CQGra..24R.113A. doi:10.1088/0264-9381/24/17/R01.
  2. ↑ Amaro-Seoane, Pau; Aoudia, Sofiane; Babak, Stanislav; Binétruy, Pierre; Berti, Emanuele; Bohé, Alejandro; Caprini, Chiara; Colpi, Monica; Cornish, Neil J; Danzmann, Karsten; Dufaux, Jean-François; Gair, Jonathan; Jennrich, Oliver; Jetzer, Philippe; Klein, Antoine; Lang, Ryan N; Lobo, Alberto; Littenberg, Tyson; McWilliams, Sean T; Nelemans, Gijs; Petiteau, Antoine; Porter, Edward K; Schutz, Bernard F; Sesana, Alberto; Stebbins, Robin; Sumner, Tim; Vallisneri, Michele; Vitale, Stefano; Volonteri, Marta; Ward, Henry; Babak, Stanislav; Binétruy, Pierre; Berti, Emanuele; Bohé, Alejandro; Caprini, Chiara; Colpi, Monica; Cornish, Neil J.; Danzmann, Karsten; Dufaux, Jean-François; Gair, Jonathan; Jennrich, Oliver; Jetzer, Philippe; Klein, Antoine; Lang, Ryan N.; Lobo, Alberto; Littenberg, Tyson; McWilliams, Sean T.; Nelemans, Gijs; Petiteau, Antoine; Porter, Edward K.; Schutz, Bernard F.; Sesana, Alberto; Stebbins, Robin; Sumner, Tim; Vallisneri, Michele; Vitale, Stefano; Volonteri, Marta; Ward, Henry (21 June 2012). "Low-frequency gravitational-wave science with eLISA/NGO". Classical and Quantum Gravity. 29 (12): 124016. arXiv:1202.0839Freely accessible. Bibcode:2012CQGra..29l4016A. doi:10.1088/0264-9381/29/12/124016.
  3. 1 2 3 4 5 6 Merritt, David (2013). Dynamics and Evolution of Galactic Nuclei. Princeton, NJ: Princeton University Press. ISBN 9781400846122.
  4. ↑ Gair, Jonathan; Vallisneri, Michele; Larson, Shane L.; Baker, John G. (2013). "Testing General Relativity with Low-Frequency, Space-Based Gravitational-Wave Detectors". Living Reviews in Relativity. 16: 7. arXiv:1212.5575Freely accessible. Bibcode:2013LRR....16....7G. doi:10.12942/lrr-2013-7.
  5. ↑ Moore, Christopher; Cole, Robert; Berry, Christopher (19 July 2013). "Gravitational Wave Detectors and Sources". Retrieved 14 April 2014.
  6. ↑ Glampedakis, Kostas (7 August 2005). "Extreme mass ratio inspirals: LISA's unique probe of black hole gravity". Classical and Quantum Gravity. 22 (15): S605–S659. arXiv:gr-qc/0509024Freely accessible. Bibcode:2005CQGra..22S.605G. doi:10.1088/0264-9381/22/15/004.
  7. ↑ Gair, J. R. (13 December 2008). "The black hole symphony: probing new physics using gravitational waves". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 366 (1884): 4365–4379. Bibcode:2008RSPTA.366.4365G. doi:10.1098/rsta.2008.0170.
  8. ↑ Barack, Leor; Cutler, Curt (2004). "LISA Capture Sources: Approximate Waveforms, Signal-to-Noise Ratios, and Parameter Estimation Accuracy". Physical Review D. 69 (8): 082005. arXiv:gr-qc/0310125Freely accessible. Bibcode:2004PhRvD..69h2005B. doi:10.1103/PhysRevD.69.082005.
  9. ↑ Grace Mason-Jarrett, "Mapping spacetime around supermassive black holes" Things We Don´t Know, 1 July 2014
  10. ↑ Berry, C. P. L.; Gair, J. R. (12 December 2012). "Observing the Galaxy's massive black hole with gravitational wave bursts". Monthly Notices of the Royal Astronomical Society. 429 (1): 589–612. arXiv:1210.2778Freely accessible. Bibcode:2013MNRAS.429..589B. doi:10.1093/mnras/sts360.
  11. 1 2 Merritt, David; Alexander, Tal; Mikkola, Seppo; Will, Clifford (August 2011). "Stellar dynamics of extreme-mass-ratio inspirals". Physical Review D. 84 (4): 044024. arXiv:1102.3180Freely accessible. Bibcode:2011PhRvD..84d4024M. doi:10.1103/PhysRevD.84.044024.
  12. ↑ Hopman, Clovis; Alexander, Tal (10 July 2006). "Resonant Relaxation near a Massive Black Hole: The Stellar Distribution and Gravitational Wave Sources". The Astrophysical Journal. 645 (2): 1152–1163. arXiv:astro-ph/0601161Freely accessible. Bibcode:2006ApJ...645.1152H. doi:10.1086/504400.
  13. ↑ Amaro-Seoane, Pau; Sopuerta, Carlos F.; Freitag, Marc D. (2013). "The role of the supermassive black hole spin in the estimation of the EMRI event rate". Monthly Notices of the Royal Astronomical Society,. 429 (4): 3155–3165. arXiv:1205.4713Freely accessible. Bibcode:2013MNRAS.429.3155A. doi:10.1093/mnras/sts572.
  14. ↑ Mandel, Ilya; Brown, Duncan A.; Gair, Jonathan R.; Miller, M. Coleman (2008). "Rates and Characteristics of Intermediate Mass Ratio Inspirals Detectable by Advanced LIGO". Astrophysical Journal. 681 (2): 1431–1447. arXiv:0705.0285Freely accessible. Bibcode:2008ApJ...681.1431M. doi:10.1086/588246.
  15. ↑ Barack, Leor (7 November 2009). "Gravitational self-force in extreme mass-ratio inspirals". Classical and Quantum Gravity. 26 (21): 213001. arXiv:0908.1664Freely accessible. Bibcode:2009CQGra..26u3001B. doi:10.1088/0264-9381/26/21/213001.
  16. ↑ Barack, Leor; Sago, Norichika (2007). "Gravitational self force on a particle in circular orbit around a Schwarzschild black hole". Physical Review D. 75 (6): 064021. arXiv:gr-qc/0701069Freely accessible. Bibcode:2007PhRvD..75f4021B. doi:10.1103/PhysRevD.75.064021. Barack, Leor; Sago, Norichika (2010). "Gravitational self-force on a particle in eccentric orbit around a Schwarzschild black hole". Physical Review D. 81 (8): 084021. arXiv:1002.2386Freely accessible. Bibcode:2010PhRvD..81h4021B. doi:10.1103/PhysRevD.81.084021.
  17. ↑ Warburton, Niels; Barack, Leor (2011). "Self force on a scalar charge in Kerr spacetime: eccentric equatorial orbits". Physical Review D. 83 (12): 124038. arXiv:1103.0287Freely accessible. Bibcode:2011PhRvD..83l4038W. doi:10.1103/PhysRevD.83.124038.Warburton, Niels; Barack, Leor (2010). "Self force on a scalar charge in Kerr spacetime: circular equatorial orbits". Physical Review D. 81 (8): 084039. arXiv:1003.1860Freely accessible. Bibcode:2010PhRvD..81h4039W. doi:10.1103/PhysRevD.81.084039.

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External links

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