Relativistic Diskoseismology. II. Analytical Results for c‐modes

Silbergleit, A. S.; Wagoner, Robert V.; Ortega‐Rodríguez, Manuel

doi:10.1086/318659

Cited by 114 publications

(159 citation statements)

References 15 publications

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“…For example, R. V. Wagoner (2001, private communication) has pointed out that the 40 Hz QPO could in principle be identified with a corrugation or c-mode and the 67 Hz QPO with the g-mode. If these identifications are correct, one can obtain constraints on both the mass and spin of the black hole (see Wagoner 1999;Silbergleit, Wagoner, & Ortega-Rodríguez 2001).…”

Section: Discussion and Summarymentioning

confidence: 99%

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

Strohmayer

2001

The Astrophysical Journal

132

107

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We report the discovery in archival Rossi X-Ray Timing Explorer data of a ∼40 Hz quasi-periodic oscillation (QPO) in the hard X-ray flux from the Galactic microquasar GRS 1915ϩ105. The QPO is detected only in the hard X-ray band above ∼13 keV and was discovered in observations in which the previously known 67 Hz QPO is present. The 40 Hz QPO has a typical rms amplitude of ∼2% in the 13-27 keV band and a width of ∼5.5 Hz (FWHM). We show that the 67 and 40 Hz QPOs are detected in the same observations in 1997 July and November. However, the QPO is not detected in observations from 1996 April, May, and June in which the 67 Hz QPO was first discovered. The frequency of the 67 Hz QPO is significantly higher in the 1997 observations by about 5% compared with the 1996 data. The identification of the 40 Hz QPO makes GRS 1915ϩ105 the second black hole binary to show a pair of simultaneous high-frequency QPOs (the other being GRO J1655Ϫ40). The similarities between the properties of the 67 Hz QPO in GRS 1915ϩ105 and the recently discovered 450 Hz QPO in GRO J1655Ϫ40 suggest that the pairs of frequencies in these systems may be produced by the same physical mechanism, with the frequency differences between the two being likely due to different black hole masses in the two systems. We discuss the implications of our result for the mass and spin of GRS 1915ϩ105 as well as for models of X-ray variability in black holes and neutron stars.

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Section: Discussion and Summarymentioning

confidence: 99%

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

Strohmayer

2001

The Astrophysical Journal

132

107

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“…The resulting ordinary di †erential equations for the vertical and radial eigenfunctions are (see Nowak & (V y ) ( V r ) Wagoner 1992, Perez et al 1997, andSilbergleit et al 2001 for details)…”

Section: Equations For the Disk Perturbationsmentioning

confidence: 99%

“…Along with the angular mode number m, we employ j and n for the vertical and radial mode numbers (number of nodes in the corresponding eigenfunction), respectively, as in Perez et al (1997) and Silbergleit et al (2001).…”

Section: Formentioning

confidence: 99%

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Relativistic Diskoseismology. III. Low‐Frequency Fundamentalp‐Modes

Ortega‐Rodríguez

Silbergleit

Wagoner

2002

ApJ

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We extend our investigation of the normal modes of small adiabatic oscillations of relativistic barotropic thin accretion disks to the inertial-pressure (p) modes. We focus here on the lowest frequency fundamental p-modes, those with no axial or vertical nodes in their distribution. Through a variety of analyses, we obtain closed-form expressions for the eigenfrequencies and eigenfunctions. These depend on the luminosity and viscosity parameter of the disk as well as the mass and angular momentum of the black hole via detailed formulae for the speed of sound. The e †ect of a torque on the inner edge of the disk is also included. We compare the p-mode properties to those of the g-and c-modes.

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“…These ideas have been widely discussed and adapted into numerous individual disc-oscillation models. The subject of disc oscillations and their propagation has been extensively studied analytically for thin disc (i.e., nearly geodesic, radiatively efficient) configurations (Okazaki et al 1987;Kato et al 1998;Wagoner 1999Wagoner , 2008Wagoner et al 2001;Silbergleit et al 2001;Ortega-Rodríguez et al 2002). The derived results have been compared to those for "thick" (radiatively inefficient, slim-disc or toroidal) configurations foe which both analytical (Blaes 1985;Šrámková 2005;Abramowicz et al 2006;Blaes et al 2006Blaes et al , 2007Straub & Šrámková 2009) and numerical (Rezzolla et al 2003a,b;Rezzolla 2004;Montero et al 2004;Zanotti et al 2005;Šrámková et al 2007) studies have been performed.…”

Section: Hf Qpo Interpretationmentioning

confidence: 99%

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

Urbanec

Török

Šrámková

et al. 2010

A&A

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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 R NS is larger than the related radius of the marginally stable circular orbit r ms for nuclear matter equations of state and spin frequencies up to 800 Hz. For the same range of spin and a strange star (MIT) equation of state, the inferrred radius is R NS ∼ r ms . The "Paczyński modulation" mechanism considered within the model requires that R NS < r ms . However, we find this condition to be fulfilled only for the strange matter equation of state, masses below 1 M , and spin frequencies above 800 Hz. 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.

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Relativistic Diskoseismology. II. Analytical Results for c‐modes

Cited by 114 publications

References 15 publications

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

Discovery of a Second High-Frequency Quasi-periodic Oscillation from the Microquasar GRS 1915+105

Relativistic Diskoseismology. III. Low‐Frequency Fundamentalp‐Modes

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

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