26,069 research outputs found
Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model
The high-frequency quasi-periodic oscillations (HF QPOs) that appear in the
X-ray fluxes of low-mass X-ray binaries remain an unexplained phenomenon. Among
other ideas, it has been suggested that a non-linear resonance between two
oscillation modes in an accretion disc orbiting either a black hole or a
neutron star plays a role in exciting the observed modulation. Several possible
resonances have been discussed. A particular model assumes resonances in which
the disc-oscillation modes have the eigenfrequencies equal to the radial and
vertical epicyclic frequencies of geodesic orbital motion. This model has been
discussed for black hole microquasar sources as well as for a group of neutron
star sources. Assuming several neutron (strange) star equations of state and
Hartle-Thorne geometry of rotating stars, we briefly compare the frequencies
expected from the model to those observed. Our comparison implies that the
inferred neutron star radius "RNS" is larger than the related radius of the
marginally stable circular orbit "rms" for nuclear matter equations of state
and spin frequencies up to 800Hz. For the same range of spin and a strange star
(MIT) equation of state, the inferrred radius RNS is roughly equal to rms. The
Paczynski modulation mechanism considered within the model requires that RNS <
rms. However, we find this condition to be fulfilled only for the strange
matter equation of state, masses below one solar mass, and spin frequencies
above 800Hz. This result most likely falsifies the postulation of the neutron
star 3:2 resonant eigenfrequencies being equal to the frequencies of geodesic
radial and vertical epicyclic modes. We suggest that the 3:2 epicyclic modes
could stay among the possible choices only if a fairly non-geodesic accretion
flow is assumed, or if a different modulation mechanism operates.Comment: 7 pages, 4 figures (in colour), accepted for publication in Astronomy
& Astrophysic
Oscillations of Thick Accretion Discs Around Black Holes
We present a numerical study of the response of a thick accretion disc to a
localized, external perturbation with the aim of exciting internal modes of
oscillation. We find that the perturbations efficiently excite global modes
recently identified as acoustic p--modes, and closely related to the epicyclic
oscillations of test particles. The two strongest modes occur at
eigenfrequencies which are in a 3:2 ratio. We have assumed a constant specific
angular momentum distribution within the disc. Our models are in principle
scale--free and can be used to simulate accretion tori around stellar or super
massive black holes.Comment: 4 pages, 4 figures, accepted for publication as a letter in the
Monthly Notices of the Royal Astronomical Societ
Of NBOs and kHz QPOs: a low-frequency modulation in resonant oscillations of relativistic accretion disks
The origin of quasi periodic modulations of flux in the kilohertz range (kHz
QPOs), observed in low-mass X-ray binaries, is usually assumed to be physically
distinct from that of the ``normal branch oscillations'' (NBOs) in the
Z-sources. We show that a low-frequency modulation of the kHz QPOs is a natural
consequence of the non-linear relativistic resonance suggested previously to
explain the properties of the high-frequency twin peaks. The theoretical
results discussed here are reminiscent of the 6 Hz variations of frequency and
amplitude of the kHz QPOs reported by Yu, van der Klis and Jonker (2001).Comment: Accepted for publication in PASJ; 4 pages, 1 figur
Leaving the ISCO: the inner edge of a black-hole accretion disk at various luminosities
The "radiation inner edge" of an accretion disk is defined as the inner
boundary of the region from which most of the luminosity emerges. Similarly,
the "reflection edge" is the smallest radius capable of producing a significant
X-ray reflection of the fluorescent iron line. For black hole accretion disks
with very sub-Eddington luminosities these and all other "inner edges" locate
at ISCO. Thus, in this case, one may rightly consider ISCO as the unique inner
edge of the black hole accretion disk. However, even for moderate luminosities,
there is no such unique inner edge as differently defined edges locate at
different places. Several of them are significantly closer to the black hole
than ISCO. The differences grow with the increasing luminosity. For nearly
Eddington luminosities, they are so huge that the notion of the inner edge
losses all practical significance.Comment: 12 pages, 15 figures, submitted to A&
QPOs in Cataclysmic Variables and in X-ray Binaries
Recent observations, reported by Warner and Woudt, of Dwarf Nova Oscillations
(DNOs) exhibiting frequency drift, period doubling, and 1:2:3 harmonic
structure, can be understood as disc oscillations that are excited by
perturbations at the spin frequency of the white dwarf or of its equatorial
layers. Similar quasi-periodic disc oscillations in black hole low-mass X-ray
binary (LMXB) transients in a 2:3 frequency ratio show no evidence of frequency
drift and correspond to two separate modes of disc oscillation excited by an
internal resonance. Just as no effects of general relativity play a role in
white dwarf DNOs, no stellar surface or magnetic field effects need be invoked
to explain the black hole QPOs.Comment: Revised version. Astronomy & Astrophysics (Letters), in pres
A non-linear resonance model for the black hole and neutron star QPOs: theory supported by observations
Kilohertz Quasi-Periodic Oscillations (QPOs) have been detected in many
accreting X-ray binaries. It has been suggested that the highest QPO
frequencies observed in the modulation of the X-ray flux reflect a non-linear
resonance between two modes of accreting disk oscillation. This hypothesis
implies certain very general predictions, several of which have been borne out
by observations. Some of these follow from properties of non-linear
oscillators, while the others are specific to oscillations of fluid in strong
gravity. A 3:2 resonant ratio of frequencies can be clearly recognized in the
black-hole as well as in the neutron-star QPO data.Comment: 8 pages, 8 figures, to appear in Proceedings of the Albert Einstein
Century International Conferenc
QPOs in microquasars and Sgr A*: measuring the black hole spin
In all four microquasars which show double peak kHz QPOs, the ratio of the
two frequencies is 3:2. This strongly supports the suggestion that twin peak
kHz QPOs are due to a resonance between some modes of accretion disk
oscillations. Here, we stress that fits to observations of the hypothetical
resonances between vertical and radial epicyclic frequencies (particularly of
the parametric resonance) give an accurate estimate of the spin for the three
microquasars with known mass. Measurement of double peak QPOs frequencies in
the Galaxy centre seems also to be consistent with the 3:2 ratio established by
previous observations in microquasars, however the Sgr A* data are rather
difficult for the same exact analysis. If confirmed, the 3:2 ratio of double
peak QPOs in Sgr A* would be of a fundamental importance for the black hole
accretion theory and the precise measurement could help to solve the question
of QPOs nature.Comment: 5 pages, 5 figures, 3 table
The slimming effect of advection on black-hole accretion flows
At super-Eddington rates accretion flows onto black holes have been described
as slim (aspect ratio ) or thick (H/R >1) discs, also known as
tori or (Polish) doughnuts. The relation between the two descriptions has never
been established, but it was commonly believed that at sufficiently high
accretion rates slim discs inflate, becoming thick. We wish to establish under
what conditions slim accretion flows become thick. We use analytical equations,
numerical 1+1 schemes, and numerical radiative MHD codes to describe and
compare various accretion flow models at very high accretion rates.We find that
the dominant effect of advection at high accretion rates precludes slim discs
becoming thick. At super-Eddington rates accretion flows around black holes can
always be considered slim rather than thick.Comment: 8 pages, 5 figures. Astronomy & Astrophysics, in pres
- âŠ