8 research outputs found
Accretion flow behaviour during the evolution of the Quasi Periodic Oscillation Frequency of XTE J1550-564 in 1998 outburst
Low and intermediate frequency quasi-periodic oscillations (QPOs) are thought
to be due to oscillations of Comptonizing regions or hot regions embedded in
Keplerian discs. Observational evidence of evolutions of QPOs would therefore
be very important as they throw lights on the dynamics of the hotter region.
Our aim is to find systems in which there is a well-defined correlation among
the frequencies of the QPOs over a range of time so as to understand the
physical picture. In this paper, we concentrate on the archival data of XTE
J1550-564 obtained during 1998 outburst, and study the systematic drifts during
the rising phase from the 1998 September 7 to the 1998 September 19, when the
QPO frequency increased monotonically from 81mHz to 13.1Hz. Immediately after
that, QPO frequency started to decrease and on the 1998 September 26, the QPO
frequency became 2.62Hz. After that, its value remained almost constant. This
frequency drift can be modelled satisfactorily with a propagatory oscillating
shock solution where the post-shock region behaves as the Comptonized region.
Comparing with the nature of a more recent 2005 outburst of another black hole
candidate GRO 1655-40, where QPOs disappeared at the end of the rising phase,
we conjecture that this so-called `outburst' may not be a full-fledged
outburst.Comment: 15 pages, 6 figure
Discovery of Jet-Induced Soft Lags of XTE J1550-564 during Its 1998 Outburst
X-ray time lags are complicated in nature. The exact reasons for complex lag
spectra are yet to be known. However, the hard lags, in general, are believed
to be originated due to the inverse Comptonization process. But, the origin of
soft lags remained mischievous. Recent studies on "Disk-Jet Connections"
revealed that the jets are also contributing to the X-ray spectral and timing
properties in a magnitude which was more than what was predicted earlier. In
this article, we first show an exact anti-correlation between X-ray time lag
and radio flux for XTE J1550-546 during its 1998 outburst. We propose that the
soft lags might be generated due to the change in the accretion disk structure
along the line of sight during higher jet activity.Comment: The article contains six pages and two figures. Open access publisher
link https://www.mdpi.com/2504-3900/17/1/
Long-term X-ray observations of seyfert 1 galaxy ark 120: on the origin of soft-excess
We present the long-term X-ray spectral and temporal analysis of a tare-type AGN' Ark 120. We consider the observations from XMM-Newton, Suzaku, Swift, and NuSTAR from 2003 to 2018. The spectral properties of this source are studied using various phenomenological and physical models present in the literature. We report (a) the variations of several physical parameters, such as the temperature and the optical depth of the electron cloud, the size of the Compton cloud, and the accretion properties for the last 15 yr. The spectral variations are explained from the changes in the accretion dynamics; (b) the X-ray time delay between 0.2-2 and 3-10 keV light-curves exhibited zero-delay in 2003, positive delay of 4.71 +/- 2.1 ks in 2013, and negative delay of 2.90 +/- 1.26 ks in 2014. The delays are explained considering Comptonization, reflection, and light-crossing time; (c) the long-term intrinsic luminosities, obtained using nthcomp, of the soft-excess and the primary continuum show a correlation with a Pearson correlation coefficient of 0.90. This indicates that the soft-excess and the primary continuum originate from the same physical process. From a physical model fitting, we infer that the soft excess for Ark 120 could be due to a small number of scatterings in the Compton cloud. Using Monte Carlo simulations, we show that indeed the spectra corresponding to fewer scatterings could provide a steeper soft-excess power law in the 0.2-3 keV range. Simulated luminosities are found to be in agreement with the observed values. We present the long-term X-ray spectral and temporal analysis of a 'bare-type AGN' Ark 120. We consider the observations from XMM-Newton, Suzaku, Swift, and NuSTAR from 2003 to 2018. The spectral properties of this source are studied using various phenomenological and physical models present in the literature. We report (a) the variations of several physical parameters, such as the temperature and the optical depth of the electron cloud, the size of the Compton cloud, and the accretion properties for the last 15 yr. The spectral variations are explained from the changes in the accretion dynamics; (b) the X-ray time delay between 0.2-2 and 3-10 keV light-curves exhibited zero-delay in 2003, positive delay of 4.71 +/- 2.1 ks in 2013, and negative delay of 2.90 +/- 1.26 ks in 2014. The delays are explained considering Comptonization, reflection, and light-crossing time; (c) the long-term intrinsic luminosities, obtained using nthcomp, of the soft-excess and the primary continuum show a correlation with a Pearson correlation coefficient of 0.90. This indicates that the soft-excess and the primary continuum originate from the same physical process. From a physical model fitting, we infer that the soft excess for Ark 120 could be due to a small number of scatterings in the Compton cloud. Using Monte Carlo simulations, we show that indeed the spectra corresponding to fewer scatterings could provide a steeper soft-excess power law in the 0.2-3 keV range. Simulated luminosities are found to be in agreement with the observed values