Relativistic dynamics and extreme mass ratio inspirals
Amaro-Seoane, Pau1,2,3,4
AbstractIt is now well-established that a dark, compact object, very likely a massive black hole (MBH) of around four million solar masses is lurking at the centre of the Milky Way. While a consensus is emerging about the origin and growth of supermassive black holes (with masses larger than a billion solar masses), MBHs with smaller masses, such as the one in our galactic centre, remain understudied and enigmatic. The key to understanding these holes-how some of them grow by orders of magnitude in mass-lies in understanding the dynamics of the stars in the galactic neighbourhood. Stars interact with the central MBH primarily through their gradual inspiral due to the emission of gravitational radiation. Also stars produce gases which will subsequently be accreted by the MBH through collisions and disruptions brought about by the strong central tidal field. Such processes can contribute significantly to the mass of the MBH and progress in understanding them requires theoretical work in preparation for future gravitational radiation millihertz missions and X-ray observatories. In particular, a unique probe of these regions is the gravitational radiation that is emitted by some compact stars very close to the black holes and which could be surveyed by a millihertz gravitational-wave interferometer scrutinizing the range of masses fundamental to understanding the origin and growth of supermassive black holes. By extracting the information carried by the gravitational radiation, we can determine the mass and spin of the central MBH with unprecedented precision and we can determine how the holes "eat" stars that happen to be near them.
KeywordBlack holes Gravitational waves Stellar dynamics
WOS Research AreaPhysics
WOS SubjectPhysics, Particles & Fields
WOS IDWOS:000434341300001
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Document Type期刊论文
Corresponding AuthorAmaro-Seoane, Pau
Affiliation1.CSIC, IEEC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain
2.Chinese Acad Sci, Acad Math & Syst Sci, Inst Appl Math, Beijing 100190, Peoples R China
3.Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
4.TU Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany
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Amaro-Seoane, Pau. Relativistic dynamics and extreme mass ratio inspirals[J]. LIVING REVIEWS IN RELATIVITY,2018,21:150.
APA Amaro-Seoane, Pau.(2018).Relativistic dynamics and extreme mass ratio inspirals.LIVING REVIEWS IN RELATIVITY,21,150.
MLA Amaro-Seoane, Pau."Relativistic dynamics and extreme mass ratio inspirals".LIVING REVIEWS IN RELATIVITY 21(2018):150.
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