arXiv subjects

Danny Steeghs

Publications and source records attributed to Danny Steeghs.

62 records · Page 4Linked to original sources

arXiv2004

High- and low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole transient H1743-322

We present a variability study of the black hole candidate and X-ray transient H1743-322 during its 2003/2004 outburst. We analyzed five Rossi X-ray Timing Explorer observations that were performed as part of a multi-wavelength campaign, as well as six observations from the early rise of the outburst. The source was observed in several black hole states and showed various types of X-ray variability, including high frequency quasi-periodic oscillations (QPOs) at 240 Hz and 160 Hz (i.e. with a 3:2 frequency ratio), several types of low frequency QPOs, and strong variations on a time scale of a few hundred seconds. The discovery of high frequency QPOs in H1743-322 supports predictions that these QPOs should be more easily observed in high inclination systems. In one of our observations we observed a transition in count rate and color, during which we were able to follow the smooth evolution of the low-frequency QPOs from type-B to type-A. We classify the X-ray observations and QPOs, and briefly discuss the QPOs in terms of recently proposed models.

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arXiv2001

First results from multi-wavelength observations during the 2001 outburst of WZ Sge

WZ Sge has shown superoutbursts in 1913, 1946 and 1978. On 2001 July 23 a new outburst was announced, about 10 years `too early'. Target of opportunity satellite observations with Chandra, FUSE, HST and RXTE were performed throughout the outburst. From the ground WZ Sge was monitored by numerous professional and amateur astronomers, in the optical, IR and radio. We give an account of the first exciting results from these multi-wavelength observations.

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arXiv2001

The Quiescent Spectrum of the AM CVn star CP Eri

We used the 6.5m MMT to obtain a spectrum of the AM CVn star CP Eri in quiescence. The spectrum is dominated by He I emission lines, which are clearly double peaked with a peak-to-peak separation of ~1900 km/s. The spectrum is similar to that of the longer period AM CVn systems GP Com and CE 315, linking the short and the long period AM CVn systems. In contrast with GP Com and CE 315, the spectrum of CP Eri does not show a central 'spike' in the line profiles, but it does show lines of SiII in emission. The presence of these lines indicates that the material being transferred is of higher metallicity than in GP Com and CE 315, which, combined with the low proper motion of the system, probably excludes a halo origin of the progenitor of CP Eri. We constrain the primary mass to M_1>0.27 M_sun and the orbital inclination to 33 degr < i < 80 degr. The presence of the He I lines in emission opens up the possibility for phase resolved spectroscopic studies which allows a determination of the system parameters and a detailed study of helium accretion disks under highly varying circumstances.

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arXiv2001

The mass donor of Scorpius X-1 revealed

We present the first detection of the mass donor star in the prototype X-ray binary Scorpius X-1. Phase resolved spectroscopy revealed narrow emission lines components from the irradiated secondary star. Radial velocity fits to the Bowen blend emission are used to establish an absolute orbital ephemeris and derive an accurate value for the systemic velocity; gamma= -113.8 +/- 0.6 km/s. Emission from the irradiated front side of the secondary leads to solid limits to the radial velocity of the mass donor of 87 < K_2 < 148 km/s. In conjunction with an upper limit to the velocity of the primary K_1 < 53 km/s, we derive a firm limit on the mass ratio of Sco X-1 of q < 0.61. % A likely set of system parameters satisfying the various constraints as well as the recent inclination estimate by Fomalont et al. (2001) is K_1=40 km/s, K_2=133 km/s, q=0.30 corresponding to component masses of M_1=1.4M_sun, M_2=0.42 M_sun for an orbital inclination of 38 degrees.

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arXiv1999

Multi-epoch Doppler tomography and polarimetry of QQ Vul

(abridged abstract) We present multi-epoch high-resolution spectroscopy and photoelectric polarimetry of the long-period polar (AM Herculis star) QQ Vul. The blue emission lines show several distinct components, the sharpest of which can unequivocally be assigned to the illuminated hemisphere of the secondary star and used to trace its orbital motion. This narrow emission line can be used in combination with NaI-absorption lines from the photosphere of the companion to build a stable long-term ephemeris for the star: inferior conjunction of the companion occurs at HJD = 2448446.4710(5) + E 0.15452011(11).

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arXiv1999

On the observability of spiral structures in CV accretion discs

We use the grid of hydrodynamic accretion disc calculations of Stehle (1999) to construct orbital phase dependent emission line profiles of thin discs carrying spiral density waves. The observational signatures of spiral waves are explored to establish the feasibility of detecting spiral waves in cataclysmic variable discs using prominent emission lines in the visible range of the spectrum. For high Mach number accretion discs (M = 15-30), we find that the spiral shock arms are so tightly wound that they leave few obvious fingerprints in the emission lines. Only a minor variation of the double peak separation in the line profile at a level of 8% is produced. For accretion discs in outburst (M = 5-20) however, the lines are dominated by the emission from an m=2 spiral pattern in the disc. We show that reliable Doppler tomograms of spiral shock patterns can be reconstructed provided that a signal to noise of at least 15, a wavelength resolution of 80 km/s and a time resolution of 50 spectra per binary orbit is achieved. We confirm that the observed spiral pattern in the disc of IP Pegasi can be reproduced by tidal density waves in the accretion disc and demands the presence of a large, hot disc, at least in the early outburst stages.

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arXiv1998

Tomography of Polars

We are reviewing the power of Doppler tomography for detailed investigations of polars (magnetic cataclysmic binaries without accretion disk). Using high-resolution spectroscopy in combination with tomography as analytic tool, the structure and extent of the accretion flows and accretion curtains in the binaries can be uncovered and the irradiated and non-irradiated parts of the mass-donating secondary stars can be made visible. In addition we show, how basic system parameters like the binary inclination and the mass ratio can be addressed by tomography.

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arXiv1997

A Doppler Map and Mass-ratio Constraint for the Black-Hole X-ray Nova Ophiuchi 1977

We have reanalyzed Keck observations of Nova Oph 1977 to extend the work done by Filippenko et al. (1997), who recently determined a mass function f(M_x) = 4.86 +/- 0.13 M_o for the compact object. We constrain the rotational broadening, v sin i < 79 km/s, at the 90% confidence level, which gives a mass ratio q < 0.053. The K-type companion star of Nova Oph 1977 contributes 28-37% of the light at red wavelengths. The abnormal LiI 6708 absorption line from the companion star is not detected (EW < 0.12 A), in contrast to four other X-ray binaries. An Halpha Doppler image of the system shows emission from the companion star in addition to the accretion disk.

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