arXiv subjects

Erik Kuulkers

Publications and source records attributed to Erik Kuulkers.

At least 55 records · Page 3Linked to original sources

arXiv2001

The Optical Counterpart of the Accreting Millisecond Pulsar SAX J1808.4-3658 in Outburst: Constraints on the Binary Inclination

We present multiband optical/infrared photometry of V4580 Sgr, the optical counterpart of the accretion-powered millisecond pulsar SAX J1808.4-3658, taken during the 1998 X-ray outburst of the system. The optical flux is consistent with emission from an X-ray-heated accretion disk. Self-consistent modeling of the X-ray and optical emission during the outburst yields best-fit extinction Av=0.68 and inclination cos(i)=0.65, assuming a distance of 2.5 kpc. The allowed inclination range requires that the pulsar's stellar companion has extremely low mass, 0.05-0.10 Msun. Some of the infrared observations are not consistent with disk emission and are too bright to be from either the disk or the companion, even in the presence of X-ray heating.

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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

A Black Hole in the Superluminal source SAX J1819.3-2525 (V4641 Sgr)

(shortened) Spectroscopic observations of the fast X-ray transient and superluminal jet source SAX J1819.3-2525 (V4641 Sgr) reveal a best fitting period of P_spect=2.81678 +/- 0.00056 days and a semiamplitude of K_2=211.0 +/- 3.1 km/sec. The optical mass function is f(M)=2.74 +/- 0.12 solar masses. We find a photometric period of P_photo=2.81730 +/- 0.00001 days using a light curve measured from photographic plates. The folded light curve resembles an ellipsoidal light curve with two maxima of roughly equal height and two minima of unequal depth per orbital cycle. The secondary star is a late B-type star which has evolved off the main sequence. Using a moderate resolution spectrum (R=7000) we measure T_eff=10500 +/- 200K, log(g)=3.5 +/- 0.1, and V_rot*sin(i)=123 +/- 4 km/sec (1 sigma errors). Assuming synchronous rotation, our measured value of the projected rotational velocity implies a mass ratio of Q=M_1/M_2=1.50 +/- 0.08 (1sigma). The lack of X-ray eclipses implies an upper limit to the inclination of i<70.7 deg. On the other hand, the large amplitude of the folded light curve (about 0.5 mag) implies a large inclination (i>60 deg). Using the above mass function, mass ratio, and inclination range, the mass of the compact object is in the range 8.73 < M_1 < 11.70 solar masses and the mass of the secondary star is in the range 5.49 < M_2 < 8.14 solar masses (90% confidence). The mass of the compact object is well above the maximum mass of a stable neutron star and we conclude that V4641 Sgr contains a black hole.

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arXiv2001

A `superoutburst' in XTE J1118+480

I propose that the properties of the two outbursts observed in the X-ray transient XTE J1118+480 in 2000 are akin to superoutbursts of SU UMa stars. In these systems a `normal' outburst immediately precedes a 5-10 times longer (`super')outburst. The optical light curve of the outbursts of XTE J1118+480 is remarkably similar to that seen in some SU UMa stars, such as UV Per and T Leo, where the precursor outburst is distinct from the superoutburst, but the time scales are a factor of ~15 different. The first outburst of XTE J1118+480 was relatively short (~1 month) while the second outburst was ~5 times longer. During the second outburst superhumps were seen, a feature characteristic for superoutbursts. The gap of about a month between the two outbursts is longer in X-rays with respect to the optical, a feature not previously recognized for X-ray transients. Also in SU UMa stars the precursor outburst becomes more distinct at shorter wavelengths. Finally, I show that the time of appearance of the superhumps in XTE J1118+480 is consistent with the expected superhump growth time, if the superhump mechanism was triggered during the first outburst. I conclude that the similarity in outburst behaviour in the two types of systems provides further support that a common mechanism is at work to start the long (`super')outbursts.

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arXiv2001

On the X-ray fast-time variability of Sco X-2 (GX 349+2)

We have analysed archived Ginga data on the Z source Sco X-2 (GX349+2). We present the first detailed investigation of its X-ray fast-time variability, as a function of position in the Z track. During the two-day observation over the period 5-7 March 1989, the source was in the so-called flaring branch, and the lower part of the so-called normal branch. We found broad peaked noise with a centroid frequency and width of ~4-7 Hz and ~6-12 Hz respectively. The peaked noise was strongest in the lower flaring branch, with a maximum fractional rms amplitude of ~3 %. We conclude that it is not a manifestation of atoll source high frequency noise, as had been suggested, and compare it with the power spectral features seen in other Z sources. We find that the peaked noise is markedly different to the quasi-periodic oscillations found in the normal and flaring branches of Sco X-1; however it bears some resemblance to that seen in the flaring branch of Cyg X-2 at low overall intensities.

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arXiv2000

An Atlas of Burst Oscillations and Spectral Properties in 4U 1728-34

We study correlations between the burst properties and the position in the color-color diagram of the low mass X-ray binary 4U 1728-34 using 21 bursts found in two data sets obtained with the Rossi X-ray Timing Explorer. Using spectral fits we analyze the spectral evolution during the bursts and determine the burst peak flux, temperature, rise time and fluence. Using dynamical power spectra we study the properties of the ~363 Hz burst oscillations. We find correlations between fluence, peak flux, the occurrence of radius expansion and the presence of burst oscillations, and the position of the source in the color-color diagram. The radius expansion bursts with and without burst oscillations differ both with respect to where they occur in the color-color diagram and in how the radius expansion takes place. We compare our results with those of a similar study by Muno et al. (2000) for KS 1731-26. Both KS 1731-260 and 4U 1728-34 show more or less the same behavior with respect to the dependence of the presence/absence of the burst oscillations on the position of the source in the color-color diagram, but the dependence of most of the spectral burst parameters on the position in the color-color diagram is clearly different. We find that the systematic absence in 4U 1728-34 of burst oscillations in the ``island'' state of the color-color diagram is not explained by the bursts involving mixed H-He burning, as may be the case in KS 1731--260 (Cumming & Bildsten 2000).

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arXiv2000

Canonical Timing and Spectral Behavior of LMC X-3 in the Low/Hard State

We present results from three observations with the Rossi X-ray Timing Explorer (RXTE) of LMC X-3, obtained while the source was in an extended 'low/hard' state. The data reveal a hard X-ray spectrum which is well fit by a pure power law with photon index Gamma=1.69+/-0.02, with a source luminosity at 50 kpc of 5-16x10^{36}erg/s (2--10 keV). Strong broad-band (0.01-100 Hz) time variability is also observed, with fractional rms amplitude 40+/-4%, plus a quasi-periodic oscillation (QPO) peak at 0.46+/-0.02 Hz with rms amplitude \~14%. This is the first reported observation in which the full canonical low/hard state behavior (pure hard power law spectrum combined with strong broad-band noise and QPO) for LMC X-3 is seen. We reanalyze several archival RXTE observations of LMC X-3 and derive consistent spectral and timing parameters, and determine the overall luminosity variation between high/soft and low/hard states. The timing and spectral properties of LMC X-3 during the recurrent low/hard states are quantitatively similar to that typically seen in the Galactic black hole candidates.

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arXiv2000

X-ray Spectral Diagnostics of Gamma-Ray Burst Environments

Recently, the detection of discrete features in the X-ray afterglow spectra of GRB970508 and GRB970828 was reported. The most natural interpretation of these features is that they are redshifted Fe K emission complexes. The identification of the line emission mechanism has drastic implications for the inferred mass of radiating material, end hence the nature of the burst site. X-ray spectroscopy provides a direct observational constraint on these properties of gamma-ray bursters. We briefly discuss how these constraints arise, in the context of an application to the spectrum of GRB970508.

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arXiv2000

The first radius-expansion X-ray burst from GX 3+1

During several observations in 1999 August with RXTE of the low-mass X-ray binary GX 3+1, we found a single short and strong X-ray burst. This is the first burst from GX 3+1 which clearly shows evidence for radius expansion of the neutron-star photosphere during the thermo-nuclear runaway. We show that the cooling phase of the neutron star photosphere starts already just before the end of the contraction phase. Considering the fact that the radius expansion is due to the burst luminosity being at the Eddington luminosity, assuming standard burst parameters and accounting for gravitational redshift effects we derive a distance to the source of ~4.5 kpc, although relaxing these assumptions may lead to uncertainties up to ~30%. By comparing the persistent flux with that observed at the peak of the burst we infer that near the time of the X-ray burst the persistent luminosity of GX 3+1 is ~0.17*L_edd, confirming predictions from theoretical modeling of X-ray spectra of bright sources like GX 3+1.

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arXiv2000

The power spectral properties of the Z-source GX 340+0

We present an analysis of ~390 ksec of data of the Z source GX 340+0 taken during 24 observations with the Rossi X-ray Timing Explorer satellite. We report the discovery of a new broad component in the power spectra. The frequency of this component varied between 9 and 14 Hz, and remained close to half that of the horizontal branch quasi-periodic oscillations (HBO). Its rms amplitude was consistent with being constant around ~5%, while its FWHM increased with frequency from 7 to 18 Hz. If this sub-HBO component is the fundamental frequency, then the HBO and its second harmonic are the second and fourth harmonic component, while the third harmonic was not detected. This is similar to what was recently found for the black hole candidate XTE J1550-564. The profiles of both the horizontal- and the normal branch quasi-periodic oscillation peaks were asymmetric when they were strongest. We describe this in terms of a shoulder component at the high frequency side of the quasi-periodic oscillation peak, whose rms amplitudes were approximately constant at ~4% and \~3%, respectively. The peak separation between the twin kHz quasi-periodic oscillations was consistent with being constant at 339+-8 Hz but a trend similar to that seen in, e.g. Sco X-1 could not be excluded. We discuss our results within the framework of the various models which have been proposed for the kHz QPOs and low frequency peaks.

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arXiv1999

No QPO time lags from Sco X-1 as seen with EXOSAT: a comparison with Cyg X-2

We have measured the phase-delay and rms amplitude spectra of CygX-2 and ScoX-1. Using EXOSAT data from the normal branch of CygX-2 we confirm earlier (Ginga) results, showing that at an energy near 6keV there is both a minimum in the QPO rms amplitude spectrum and a 150 degree phase jump in the quasi-periodic oscillations (QPO) phase-delay spectrum. Surprisingly, using EXOSAT and Ginga data, we find no evidence for a phase jump of this kind in the phase-delay spectrum of ScoX-1 on either the normal or flaring branch. Upper limits (90% confidence) of 42 degrees can be set on any phase jump in the energy range 2-10keV on the normal branch, and 88 degrees on the flaring branch. The QPO rms amplitude spectrum of ScoX-1 increases steeply with energy on both the normal and flaring branches. These results suggest that the X-ray spectrum pivots about an energy of <~2keV or >~10keV or that normal branch QPO of ScoX-1 does not have a pivoting spectrum. We discuss the implications of these results in terms of the radiation-hydrodynamic model for normal branch QPO.

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arXiv1999

Optical Lightcurves of the Black Hole Binaries GRS 1124-68 and A0620-00 in Outburst: the Importance of Irradiation

We test whether the model proposed by Esin et al. to explain X-ray observations of the black hole soft X-ray transient GRS 1124-68 in outburst can also explain the optical lightcurves of a similar object A0620-00. We show that to reproduce the observed X-ray to optical flux ratio in A0620-00, we need to assume X-ray irradiation of the outer disk that is significantly in excess of what is expected for a standard planar disk. With enhanced irradiation, the Esin et al. model can reproduce the optical evolution of A0620-00 in outburst very well. Though we find that optical observations of GRS 1124-68 also imply enhanced X-ray heating of the outer disk, the irradiation appears to be a factor of roughly 3 weaker in this system than in A0620-00. This is surprising, since GRS 1124-68 has a larger disk. We speculate that enhanced irradiation may be due to disk warping, and that the degree of warping differs between the two binaries.

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arXiv1999

Discovery of a ~1 Hz quasi-periodic oscillation in the low-mass X-ray binary 4U 1746-37

We have discovered a ~1 Hz quasi-periodic oscillation (QPO) in the persistent X-ray emission and during type I X-ray bursts of the globular cluster source, dipper and low-mass X-ray binary (LMXB) 4U 1746-37. The QPO properties resemble those of QPOs found recently in the LMXB dippers 4U 1323-62, and EXO 0748-676, which makes 4U 1746-37 the third source known to exhibit this type of QPOs. We present evidence for X-ray spectral changes in this source similar to those observed in LMXBs referred to as atoll sources. We detect two states, a low intensity and spectrally hard state, and a higher intensity and spectrally soft state. This may explain the different spectral characteristics reported for 4U 1746-37 earlier. The high intensity state resembles the banana branch state of atoll sources. The QPOs are only seen in the low intensity state, and are absent when the source is in the banana branch. This strongly suggests that either the accretion disk or an extended central source change shape between the low intensity state and the banana branch. Twelve bursts were detected, of which 5 took place while the source was on the banana branch and 7 when the source was in the low intensity state. The bursts occurring on the banana branch had an e-folding time ~3 times longer than those which occurred in the low intensity state. Whereas previously detected dips showed only a decrease in count rate of ~15%, we found in one observation a dip in which the count rate dropped from ~200 counts per second to ~20 counts per second. This dip lasted only ~250 seconds, during which clear spectral hardening occured. This is the first time strong evidence for spectral changes during a dip are reported for this source.

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arXiv1999

LMC X-2: The First Extragalactic Z-Source?

We present RXTE observations of LMC X-2 obtained during a five-day interval in 1997 December, during which the source was radiating at a mean intensity near the Eddington limit, and strongly variable on timescales of seconds to hours. The shapes of the X-ray color-color and hardness-intensity diagrams during the observations, the presence of VLFN and HFN in the power spectra, and the high intrinsic X-ray luminosity of LMC X-2 (which historically spans 0.4-2.0*L_{Edd} for reasonable estimates of the neutron star mass) are more characteristic of a Z-source in its flaring branch than of an atoll-source. On this basis, we provisionally reclassify LMC X-2 as a Z-source, the eighth such source known and the first to be detected beyond our Galaxy. Using periodogram and Fourier analysis of the X-ray lightcurve we detect an apparently-significant modulation with a period of 8.160+/-0.011 hrs and a semi-amplitude increasing from 14% in the 1.8-4.0 keV range to 40% at 8.7-19.7 keV. This X-ray modulation appears to confirm a candidate orbital periodicity determined from optical photometry ten years prior to our campaign, but we cannot rule out a chance alignment of intrinsic X-ray flares. Current RXTE ASM light curves and archival EXOSAT observations show no sign of such a pronounced periodicity. The X-ray spectrum of LMC X-2 can be well fit using variations of simple Comptonization models. Fits to phase(=intensity)-resolved spectra show strong correlations between the power law slope (in one parameterization) or the depth to optical scattering (in another) and phase. We discuss the implications of these results for the inclination, geometry, and emitting regions of the LMC X-2 system.

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arXiv1999

X-ray timing behaviour of Cygnus X-2 at low intensities

It is known that the overall (mean) intensity of the low-mass X-ray binary Cyg X-2 varies on time scales from a day to months, independently from the variations on time scales of hours to a day by which the source moves between the horizontal, normal and flaring branches. We present RXTE PCA observations of Cyg X-2, taken when its overall intensity was near its lowest values, in October 1996 and September 1997. For the first time we perform a study of the fast timing behaviour at such low intensities. During the October 1996 observations the source was in the left part of the horizontal branch, and during the September 1997 observations most likely in the lower parts of the normal branch and flaring branch. We find that the properties of the very low frequency noise during the September 1997 observations are consistent with a monotonic decrease in its strength and power-law index as a function of overall intensity. In contrast, the strength of the ~6 Hz normal branch quasi-periodic oscillations do not vary monotonically with overall intensity. They are strongest at medium overall intensity and weaker both when the overall intensity is low and when the overall intensity is high.

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arXiv1999

On the Magnetospheric Beat-Frequency and Lense-Thirring Interpretations of the Horizontal Branch Oscillation in the Z Sources

We study the horizontal branch oscillations (HBO) and the two simultaneous kilohertz QPOs comparing their properties in five Z sources with the predictions of the magnetospheric beat-frequency and Lense-Thirring precession models. We find that the variation of the HBO frequency with accretion rate predicted by the magnetospheric beat-frequency model for a purely dipolar stellar magnetic field and a radiation-pressure-dominated inner accretion disk agrees well with the observed variation. This model implies that the neutron stars in the Z sources are near magnetic spin equilibrium, that their magnetic field strengths are ~10^9-10^10 G, and that the critical fastness parameter for these sources is >0.8. If the frequency of the upper kilohertz QPO is an orbital frequency in the accretion disk, the magnetospheric beat-frequency model requires that a small fraction of the gas in the disk does not couple strongly to the stellar magnetic field at 3-4 stellar radii but instead drifts slowly inward in nearly circular orbits until it is within a few kilometers of the neutron star surface. The Lense-Thirring precession model is consistent with the observed magnitudes of the HBO frequencies only if the moments of inertia of the neutron stars in the Z sources are 4-5 times larger than the largest values predicted by realistic neutron-star equations of state. The trend of the correlation between the HBO and upper kHz QPO frequencies is not consistent with this model. We argue that the change in the slope of the correlation between the frequency of the horizontal branch oscillation and the frequency of the upper kilohertz QPO, when the latter is greater than 850 Hz, is directly related to the varying frequency separation of the kilohertz QPOs.

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arXiv1999

Multiple ejections during the 1975 outburst of A0620-00

The well-known black-hole X-ray transient A0620-00 was a bright radio source during the first part of its outburst in 1975. We have revisited the available data and find for the first time evidence that the source exhibited multiple jet ejections. Rapid radio spectral changes indicate the addition of at least three new components which are initially optically thick. From single baseline interferometry taken about three weeks after the start of the X-ray outburst we find that the source is extended on arcsec scales and infer a relativistic expansion velocity. Some of the other (soft) X-ray transients, such as GS 1124-68 and GS 2000+25, show very similar X-ray outburst light curve shapes to that of A0620-00, while their radio outburst light curve shapes are different. We suggest that this is due to the radio emission being strongly beamed in outburst, whereas the X-ray emission remains isotropic. Since this effect is stronger at higher jet velocities, this strengthens our conclusion that the jets in A0620-00 and other soft X-ray transients move with relativistic speeds.

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arXiv1999

WZ Sagittae as a DQ Herculis star

We argue that quiescent WZ Sge is a rapidly spinning magnetic rotator in which most of the matter transfered from the secondary is ejected from the system. Assuming that the observed 27.87 s oscillation period is due to the spinning white dwarf we propose that the other observed principal period of 28.96 s is a beat due to reprocessing of the rotating white dwarf beam on plasma blobs in Keplerian rotation at the outer disc rim. The weaker, transient, 29.69 s period is identified as a beat with the Keplerian period of the magnetosphere. WZ Sge evolves through a cycle of spin-up and spin-down phases. During the spin-down phase it is a DQ Her star, during the spin-up phase it should be a ER UMa star.

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