The 35 day cycle of Her X-1 and the coronal wind model

Schandl, S.; Staubert, R.; König, Matthias

doi:10.1063/1.54149

Cited by 2 publications

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“…The precessing motion of the disk can be understood in the context of tidal interaction and/or as a consequence of non vanishing torques acting on the disk, e.g. due to a coronal wind (Schandl & Meyer 1994;Schandl et al 1997;Shakura et al 1998;Ketsaris et al 2001). Because of the high inclination of the system, the disk periodically blocks the line of sight to the neutron star during about 60% of the 35 day cycle.…”

Section: Introductionmentioning

confidence: 99%

Probing the outer edge of an accretion disk: a Her X-1 turn-on observed withRXTE

Kuster

Wilms

Staubert

et al. 2005

A&A

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We present the analysis of Rossi X-ray Timing Explorer (RXTE) observations of the turn-on phase of a 35 day cycle of the X-ray binary Her X-1. During the early phases of the turn-on, the energy spectrum is composed of X-rays scattered into the line of sight plus heavily absorbed X-rays. The energy spectra in the 3-17 keV range can be described by a partial covering model, where one of the components is influenced by photoelectric absorption and Thomson scattering in cold material plus an iron emission line at 6.5 keV. In this paper we show the evolution of spectral parameters as well as the evolution of the pulse profile during the turn-on. We describe this evolution using Monte Carlo simulations which self-consistently describe the evolution of the X-ray pulse profile and of the energy spectrum.

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Section: Introductionmentioning

confidence: 99%

Probing the outer edge of an accretion disk: a Her X-1 turn-on observed withRXTE

Kuster

Wilms

Staubert

et al. 2005

A&A

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Long-term developments in Her X-1: Correlation between the histories of the 35 day turn-on cycle and the 1.24 sec pulse period

Staubert¹,

Schandl²,

Klochkov³

et al. 2006

AIP Conference Proceedings

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Abstract.We have studied the long-term behaviour of the 1.24 sec pulse period and the 35 day precession period of Her X-1 and show that both periods vary in a highly correlated way (see also Staubert et al. 1997 and2000). When the spin-up rate decreases, the 35 day turn-on period shortens. This correlation is most evident on long time scales (∼2000 days), e.g., around four extended spindown episodes, but also on shorter time scales (a few 100 days) on which quasi-periodic variations are apparent. We argue that the likely common cause is variations of the mass accretion rate onto the neutron star. The data since 1991 allow a continuous sampling and indicate a lag between the turn-on behaviour and the spin behaviour, in the sense that changes are first seen in the spin, about one cycle later in the turn-on. Both the coronal wind model (Schandl & Meyer 1994) as well as the stream-disk model (Shakura et al. 1999) predict this kind of behaviour.

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The 35 day cycle of Her X-1 and the coronal wind model

Cited by 2 publications

References 0 publications

Probing the outer edge of an accretion disk: a Her X-1 turn-on observed withRXTE

Probing the outer edge of an accretion disk: a Her X-1 turn-on observed withRXTE

Long-term developments in Her X-1: Correlation between the histories of the 35 day turn-on cycle and the 1.24 sec pulse period

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