Deutsch
 
Hilfe Datenschutzhinweis Impressum
  DetailsucheBrowse

Datensatz

 
 
DownloadE-Mail
  Excitation of Kerr quasinormal modes in extreme--mass-ratio inspirals

Thornburg, J., Wardell, B., & van de Meent, M. (in preparation). Excitation of Kerr quasinormal modes in extreme--mass-ratio inspirals.

Item is

Basisdaten

einblenden: ausblenden:
Genre: Forschungspapier

Dateien

einblenden: Dateien
ausblenden: Dateien
:
1906.06791.pdf (Preprint), 2MB
Name:
1906.06791.pdf
Beschreibung:
File downloaded from arXiv at 2019-06-25 08:15
OA-Status:
Sichtbarkeit:
Öffentlich
MIME-Typ / Prüfsumme:
application/pdf / [MD5]
Technische Metadaten:
Copyright Datum:
-
Copyright Info:
-

Externe Referenzen

einblenden:

Urheber

einblenden:
ausblenden:
 Urheber:
Thornburg , Jonathan, Autor
Wardell, Barry1, Autor           
van de Meent, Maarten2, Autor           
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

Inhalt

einblenden:
ausblenden:
Schlagwörter: General Relativity and Quantum Cosmology, gr-qc
 Zusammenfassung: If a small compact object orbits a black hole, it is known that it can excite
the black hole's quasinormal modes (QNMs), leading to high-frequency
oscillations (``wiggles'') in the radiated field at $\mathcal{J}^+$, and in the
radiation-reaction self-force acting on the object after its orbit passes
through periapsis. Here we survey the phenomenology of these wiggles across a
range of black hole spins and equatorial orbits. In both the scalar-field and
gravitational cases we find that wiggles are a generic feature across a wide
range of parameter space, and that they are observable in field perturbations
at fixed spatial positions, in the self-force, and in radiated fields at
$\mathcal{J}^+$. For a given charge or mass of the small body, the QNM
excitations have the highest amplitudes for systems with a highly spinning
central black hole, a prograde orbit with high eccentricity, and an orbital
periapsis close to the light ring. The QNM amplitudes depend smoothly on the
orbital parameters, with only very small amplitude changes when the orbit's
(discrete) frequency spectrum is tuned to match QNM frequencies. The
association of wiggles with QNM excitations suggest that they represent a
situation where the \emph{nonlocal} nature of the self-force is particularly
apparent, with the wiggles arising as result of QNM excitation by the compact
object near periapsis, and then encountered later in the orbit.
Astrophysically, the effects of wiggles at $\mathcal{J}^+$ might allow direct
observation of Kerr QNMs in extreme-mass-ratio inspiral (EMRI) binary black
hole systems, potentially enabling new tests of general relativity.

Details

einblenden:
ausblenden:
Sprache(n):
 Datum: 2019-06-16
 Publikationsstatus: Keine Angabe
 Seiten: 26 pages, 12 color pdf figures and 6 color png bitmap figures, full-resolution versions of png bitmap figures included as ancillary files in anc/ directory
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Identifikatoren: arXiv: 1906.06791
URI: http://arxiv.org/abs/1906.06791
 Art des Abschluß: -

Veranstaltung

einblenden:

Entscheidung

einblenden:

Projektinformation

einblenden:

Quelle

einblenden: