Dynamical friction and scratches of orbiting satellite galaxies on host systems

Ogiya, Go; Burkert, Andreas

doi:10.1093/mnras/stw091

Cited by 24 publications

(20 citation statements)

References 53 publications

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“…In the first stage (pre-binary phase), dynamical friction of stars and dark matter (e.g. Chandrasekhar 1943;Antonini & Merritt 2012;Ogiya & Burkert 2016) as well as of the interstellar gas (e.g. Ostriker 1999; Escala et al 2004;Tanaka & Haiman 2009) play a role in depleting the SMBH's angular momentum and orbital energy with respect to the centre of the merged galaxy.…”

Section: Introductionmentioning

confidence: 99%

Accelerated orbital decay of supermassive black hole binaries in merging nuclear star clusters

Ogiya

Hahn

Mingarelli

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The coalescence of supermassive black holes (SMBHs) should generate the strongest sources of gravitational waves (GWs) in the Universe. However, the dynamics of their coalescence is the subject of much debate. In this study, we use a suite of N-body simulations to follow the merger of two nuclear star clusters (NSCs), each hosting a SMBH in their centre. We find that the presence of distinct star clusters around each SMBH has important consequences for the dynamical evolution of the SMBH binary: (i) The separation between the SMBHs decreases by a few orders of magnitude in the first few Myrs by the combined effects of dynamical friction and a drag force caused by tidally stripped stars. In fact, this is a significant speedup for equal mass ratio binaries, and becomes extreme for unequal mass ratios, e.g. 1:10 or 1:100, which traditional dynamical friction alone would not permit to bind. (ii) The subsequent binary hardening is driven by the gravitational slingshots between the SMBH binary and stars, and also depends on the mass ratio between the SMBHs. Thus, with this additional drag force, we find that all SMBHs in our suite coalesce within a Hubble time. Given that about 50% of Milky Way sized galaxies host NSCs, our results are encouraging for upcoming GW observations with the Laser Interferometer Space Antenna -LISA -which will detect SMBH coalescence in the 10 4 − 10 7 M mass range.

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Section: Introductionmentioning

confidence: 99%

Accelerated orbital decay of supermassive black hole binaries in merging nuclear star clusters

Ogiya

Hahn

Mingarelli

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The dipole feature at the centre of the host is caused by the tidal effect of the subhalo, which perturbs the position of the halo potential minimum. This effect diminishes with time as the satellite is stripped of mass (figure adapted from[218] 43 ). Right: evolution of the radial distance of a simulated subhalo orbiting a Milky Way-size halo (figure taken from[219] 44 ).…”

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confidence: 99%

Dark Matter Haloes and Subhaloes

2019

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The development of methods and algorithms to solve the N-body problem for classical, collisionless, non-relativistic particles has made it possible to follow the growth and evolution of cosmic dark matter structures over most of the Universe's history. In the best studied case -the cold dark matter or CDM model -the dark matter is assumed to consist of elementary particles that had negligible thermal velocities at early times. Progress over the past three decades has led to a nearly complete description of the assembly, structure and spatial distribution of dark matter haloes, and their substructure in this model, over almost the entire mass range of astronomical objects. On scales of galaxies and above, predictions from this standard CDM model have been shown to provide a remarkably good match to a wide variety of astronomical data over a large range of epochs, from the temperature structure of the cosmic background radiation to the large-scale distribution of galaxies. The frontier in this field has shifted to the relatively unexplored subgalactic scales, the domain of the central regions of massive haloes, and that of low-mass haloes and subhaloes, where potentially fundamental questions remain. Answering them may require: (i) the effect of known but uncertain baryonic processes (involving gas and stars), and/or (ii) alternative models with new dark matter physics. Here we present a review of the field, focusing on our current understanding of dark matter structure from N-body simulations and on the challenges ahead.

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“…To o v ercome this shortcoming, we are currently working on a new version of the present approach which includes the effects of dynamical friction. But the present version is enough for the main goal of the present series of papers: the detailed study on the 'typical' properties of low-mass subhaloes, the only ones with large enough ensembles in any individual halo (Zhao 2004 ;Pe ˜ narrubia & Benson 2005 ;Ogiya & Buckert 2016 ).…”

Section: T W O -B O Dy I N T E R Ac T I O N Smentioning

confidence: 99%

An accurate comprehensive approach to substructure – I. Accreted subhaloes

Salvador-Solé

Manrique

Botella

2021

Monthly Notices of the Royal Astronomical Society

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This is the first of a series of three Papers devoted to the study of halo substructure in hierarchical cosmologies by means of the CUSP formalism. In the present Paper we derive the properties of subhaloes and diffuse dark matter (dDM) accreted onto haloes and their progenitors. Specifically, we relate the dDM present at any time in the inter-halo medium of the real Universe or a cosmological simulation with the corresponding free-streaming mass or the halo resolution mass, respectively, and establish the link between subhaloes and their seeds in the initial density field. By monitoring the collapse and virialisation of haloes, we derive from first principles and with no single free parameter the abundance and radial distribution of dDM and subhaloes accreted onto them. Our predictions are in excellent agreement with the results of simulations, but for the predicted fraction of accreted dDM, which is larger than reported in previous works as they only count the dDM accreted onto the final halo, not onto its progenitors. The derivation pursued here clarifies the origin of some key features of substructure. Overall, our results demonstrate that CUSP is a powerful tool for understanding halo substructure and extending the results of simulations to haloes with arbitrary masses, redshifts and formation times in any hierarchical cosmology endowed with random Gaussian density perturbations.

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Dynamical friction and scratches of orbiting satellite galaxies on host systems

Cited by 24 publications

References 53 publications

Accelerated orbital decay of supermassive black hole binaries in merging nuclear star clusters

Accelerated orbital decay of supermassive black hole binaries in merging nuclear star clusters

Dark Matter Haloes and Subhaloes

An accurate comprehensive approach to substructure – I. Accreted subhaloes

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