Accretion disc
The eccentric accretion disc of the black hole A0620 00
... the accretion disc is eccentric and precess- ...cal disc, we can present a complete and coherent argument that this is the ...The disc has grown to tidal resonance, where the enhanced ...
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Investigating the structure of the accretion disc in WZ Sge from multiwaveband time-resolved spectroscopic observations - II
... symmetric accretion disc, and a phase offset larger than zero in systems having asymmetries in their ...the accretion disc and a considerable fraction of the total emission-line ...show ...
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Stability of Accretion Discs around Magnetized Stars
... axisymmetric accretion disc with an internal dynamo around magnetised ...our disc model which has been developed in Paper I & ...the disc is geometrically thin and optically ...our ...
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Kepler K2observations of the intermediate polar FO Aquarii
... by accretion of matter (Wijnands & van der Klis 1998) and where the accretion disc can also be truncated by the strong magnetic moment of the neutron ...understanding accretion in young ...
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Cataclysmic variables below the period gap: mass determinations of 14 eclipsing systems
... As well as the parameters described above, the model also provides an estimate of the flux contribution from the white dwarf, bright spot, accretion disc and donor. The white dwarf temperature and distance ...
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SDSS J0926+3624: the shortest period eclipsing binary star
... We phase-folded the March 30 data using the ephemeris given in Section 4.1, and plot the results in Fig. 8. Again, we plot a quiescent model light curve for comparison. In this plot the structure in the light curve after ...
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The photometric period in ES Ceti
... In order to address this issue we have conducted a long-term timing study of the AM CVn star ES Ceti (Warner & Woudt 2002). This system shows a 620s opti- cal modulation which is complex in structure and varies on a ...
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Kinematical studies of the low mass X ray binary GR Mus (XB 1254 690)
... In Fig. 5, we display the Bowen blend and He ii λ4686 in the form of a trailed spectrogram. All of the individual spectra were first normalized to the continuum using a third- order polynomial fit, and then phase-folded ...
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Accretion disc time lag distributions : applying CREAM to simulated AGN light curves
... an accretion disc orbiting a supermassive black hole (SMBH), clouds of both broad and narrow-line-emitting gas (the Broad Line Region and Narrow Line Region) that surround the AGN with uncertain geometry ...
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SDSS J105754 25+275947 5 : a period bounce eclipsing cataclysmic variable with the lowest mass donor yet measured
... pc, accretion disc temperature of 5800 K and an L5 secondary ...the accretion disc (Horne et ...an accretion veil (Copperwheat et ...
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Using Gaussian processes to model light curves in the presence of flickering : the eclipsing cataclysmic variable ASASSN 14ag
... the accretion disc radius, which are observed in a significant num- ber of ...with disc radius changes have to be fitted individually, requiring another method to combat ...
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Mass and spin co evolution during the alignment of a black hole in a warped accretion disc
... The spin and mass of BHs residing in galaxy nuclei do not remain constant, close to their birth values, but change sizeably through cosmic time, in response to major accretion events. In current cos- mological ...
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Correlated X ray/ultraviolet/optical variability in NGC 6814
... the accretion disc and thus produces a portion of the thermal emission – the thermal reprocessing ...the accretion disc exists that produces the UV/optical ...the accretion disc ...
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Physical properties of IP Pegasi: an eclipsing dwarf nova with an unusually cool white dwarf
... the accretion history of this ...and accretion disc in more ...the accretion disc we examine changes in disc flux and radius over the course of our ...
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Cataclysmic variables below the period gap : mass determinations of 14 eclipsing systems
... As well as the parameters described above, the model also provides an estimate of the flux contribution from the white dwarf, bright spot, accretion disc and donor. The white dwarf temperature and distance ...
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Long-term Nonlinear Behaviour of the Magnetorotational Instability in a Localised Model of an Accretion Disc
... of accretion. In an accretion disc the dissipative length-scale is much less than we considered here and so we conclude that in a disc there will be a significant enhancement to the rate of ...
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On the orbital periods of the AM CVn stars HP Librae and V803 Centauri
... cause of this complication, several of the short-period AM CVn stars do not have a secure orbital period measurement. AM CVn itself, which has a number of photometric periods dominated by one at 1051 seconds, has been ...
9
ULTRACAM photometry of the eclipsing cataclysmic variables GY Cnc, IR Com and HT Cas
... the disc in order to explain the constant quiescent brightness observed in (most) dwarf novae, which is contrary to the increase of 1–3 mag predicted by most disc instability models (see Lasota 2001 for a ...
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From outburst to quiescence : spectroscopic evolution of V1838 Aql imbedded in a bow shock nebula
... The system returned to its quiescence state after 500 d, thus presenting an opportunity to analyse the system in its quiescent state. The full optical spectrum, taken over 1000 d after the outburst, shows a clear ...
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X ray observations of cataclysmic variables
... the disc enters outburst the accretion rate increases and material in the disc fills the truncated boundary layer causing the hard X-ray flux to ...not disc truncation. Holes present in the ...
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