共查询到20条相似文献，搜索用时 15 毫秒
1.
黑洞X射线暂现源的迷你爆发是一类峰值光度较低、持续时间较短的爆发.由于观测数据较少,其物理机制仍不清楚.利用RXTE (Rossi X-ray Timing Explorer)卫星从2001年1月28日到3月14日的数据,研究了黑洞X射线暂现源XTE J1550–564 2001年迷你爆发的X射线能谱特性.发现在本次迷你爆发中, XTE J1550–564的X射线能谱可以用幂律谱很好地拟合.整个爆发的硬度强度图不是标准的q型,而是一直保持在最右侧.此外,还分析了此次爆发谱指数Γ与未吸收的2–10 keV能段的X射线流量F_(2–10 keV)的相关性,发现Γ-F_(2–10 keV)呈反相关关系,且谱指数Γ∈[1.35, 1.72].上述结果表明2001年这次爆发一直处于低/硬态,它的X射线辐射主要来自于辐射低效的吸积模式,如ADAF(Advection-Dominated Accretion Flow). 相似文献
2.
U. Mukherjee S. Bapna H. Raichur B. Paul S. N. A. Jaaffrey 《Journal of Astrophysics and Astronomy》2006,27(1):25-35
We have investigated the Quasi Periodic Oscillation (QPO) properties of the transient accreting X-ray pulsar XTE J1858 + 034
during the second outburst of this source in April–May 2004. We have used observations made with the Proportional Counter
Array (PCA) of the Rossi X-ray Timing Explorer (RXTE) during May 14–18, 2004, in the declining phase of the outburst. We detected
the presence of low frequency QPOs in the frequency range of 140–185 mHz in all the RXTE-PCA observations. We report evolution
of the QPO parameters with the time, X-ray flux, and X-ray photon energy. Though a correlation between the QPO centroid frequency
and the instantaneous X-ray flux is not very clear from the data, we point out that the QPO frequency and the one day averaged
X-ray flux decreased with time during these observations. We have obtained a clear energy dependence of the RMS variation
in the QPOs, increasing from about 3% at 3 keV to 6% at 25 keV. The X-ray pulse profile is a single peaked sinusoidal, with
pulse fraction increasing from 20% at 3 keV to 45% at 30keV. We found that, similar to the previous outburst, the energy spectrum
is well fitted with a model consisting of a cut-off power law along with an iron emission line. 相似文献
3.
Jeroen Homan Rudy Wijnands Albert Kong Jon M. Miller Sabrina Rossi Tomaso Belloni Walter H. G. Lewin 《Monthly notices of the Royal Astronomical Society》2006,366(1):235-237
We report the result of an XMM–Newton observation of the black hole X-ray transient XTE J1650–500 in quiescence. The source was not detected, and we set upper limits on the 0.5–10 keV luminosity of 0.9–1.0 × 1031 erg s−1 (for a newly derived distance of 2.6 kpc). These limits are in line with the quiescent luminosities of black hole X-ray binaries with similar orbital periods (∼7–8 h). 相似文献
4.
The observations of the black hole binary Cygnus X-l were made in the energy band of 20–100keV with a balloon-borne Xenon-filled
multiwire proportional counter telescope on 5th April 1992. Timing analysis of the data revealed the presence of Quasi-Periodic
Oscillations (QPO) in the hard X-ray emission from the source. The QPO feature in the power density spectrum is broad with
a peak at a frequency of 0.06 Hz. This result is compared with similar reports of QPOs in Cyg X-l in soft and hard X-rays.
Short time scale random intensity variations in the X-ray light curve are described with a shot noise model. 相似文献
5.
C. Brocksopp J. C. A. Miller-Jones R. P. Fender B. W. Stappers 《Monthly notices of the Royal Astronomical Society》2007,378(3):1111-1117
XTE J1748−288 is a black hole X-ray transient which went into outburst in 1998 June. The X-ray light curves showed canonical morphologies, with minor variations on the 'fast rise exponential decay' profile. The radio source, however, reached an unusually high flux density of over 600 mJy. This high radio flux was accompanied by an exceptional (>20 per cent) fractional linear polarization, the variability of which was anticorrelated with the flux density. We use this variability to discuss possible depolarization mechanisms and to predict the underlying behaviour of the (unresolved) core/jet components. 相似文献
6.
We present the latest results from a multi-epoch timing and spectral study of the Transient Anomalous X-ray Pulsar XTE J1810–197.
We have acquired seven observations of this pulsar with the Newton X-ray Multi-mirror Mission (XMM-Newton) over the course
of two and a half years, to follow the spectral evolution as the source fades from outburst. The spectrum is arguably best
characterized by a two-temperature blackbody whose luminosities are decreasing exponentially with τ
1=870 d and τ
2=280 d, respectively. The temperatures of these components are currently cooling at a rate of 22% per year from a nearly constant
value recorded at earlier epochs of kT
1=0.25 keV and kT
2=0.67 keV, respectively. The new data show that the temperature T
1 and luminosity of that component have nearly returned to their historic quiescent levels and that its pulsed fraction, which
has steadily decreased with time, is now consistent with the previous lack of detected pulsations in quiescence. We also summarize
the detections of radio emission from XTE J1810–197, the first confirmed for any AXP. We consider possible models for the
emission geometry and mechanisms of XTE J1810–197.
XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This
research is supported by XMM-Newton grant NNG05GJ61G and NASA ADP grant ADP04-0059-0024. 相似文献
7.
Cindy R. Tam Victoria M. Kaspi Bryan M. Gaensler Eric V. Gotthelf 《Astrophysics and Space Science》2007,308(1-4):519-523
The population of clearly identified anomalous X-ray pulsars has recently grown to seven, however, one candidate anomalous
X-ray pulsar (AXP) still eludes re-confirmation. Here, we present a set of seven Chandra ACIS-S observations of the transient
pulsar AX J1845.0-0258, obtained during 2003. Our observations reveal a faint X-ray point source within the ASCA error circle
of AX J1845.0-0258’s discovery, which we designate CXOU J184454.6-025653 and tentatively identify as the quiescent AXP. Its
spectrum is well described by an absorbed single-component blackbody (kT∼2.0 keV) or power law (Γ∼1.0) that is steady in flux on timescales of at least months, but fainter than AX J1845.0-0258 was during its 1993 period
of X-ray enhancement by at least a factor of 13. Compared to the outburst spectrum of AX J1845.0-0258, CXOU J184454.6-025653
is considerably harder: if truly the counterpart, then its spectral behavior is contrary to that seen in the established transient
AXP XTE J1810-197, which softened from kT∼0.67 keV to ∼0.18 keV in quiescence. This unexpected result prompts us to examine the possibility that we have observed an
unrelated source, and we discuss the implications for AXPs, and magnetars in general.
相似文献
8.
L. Sidoli P. Romano L. Ducci A. Paizis G. Cusumano V. Mangano H. A. Krimm S. Vercellone D. N. Burrows J. A. Kennea N. Gehrels 《Monthly notices of the Royal Astronomical Society》2009,397(3):1528-1538
We report on new X-ray outbursts observed with Swift from three Supergiant Fast X-ray Transients (SFXTs): XTE J1739−302, IGR J17544−2619 and IGR J08408−4503. XTE J1739−302 underwent a new outburst on 2008 August 13, IGR J17544−2619 on 2008 September 4 and IGR J08408−4503 on 2008 September 21. While the XTE J1739−302 and IGR J08408−4503 bright emission triggered the Swift /Burst Alert Telescope, IGR J17544−2619 did not, thus we could perform a spectral investigation only of the spectrum below 10 keV. The broad-band spectra from XTE J1739−302 and IGR J08408−4503 were compatible with the X-ray spectral shape displayed during the previous flares. A variable absorbing column density during the flare was observed in XTE J1739−302 for the first time. The broad-band spectrum of IGR J08408−4503 requires the presence of two distinct photon populations, a cold one (∼0.3 keV) most likely from a thermal halo around the neutron star and a hotter one (1.4–1.8 keV) from the accreting column. The outburst from XTE J1739−302 could be monitored with a very good sampling, thus revealing a shape which can be explained with a second wind component in this SFXT, in analogy to what we have suggested in the periodic SFXT IGR J11215−5952. The outburst recurrence time-scale in IGR J17544−2619 during our monitoring campaign with Swift suggests a long orbital period of ∼150 d (in a highly eccentric orbit), compatible with what previously observed with INTEGRAL . 相似文献
9.
We present the INTEGRAL and RXTE X-ray observations of XTE J1550-564, a Galactic microquasar and a black hole candidate, during its outburst in the spring of 2003. The source during the outburst was in a canonical hard state, and its spectrum remained constant in both the rise and decay phases. 相似文献
10.
F. Capitanio T. Belloni M. Del Santo P. Ubertini 《Monthly notices of the Royal Astronomical Society》2009,398(3):1194-1200
We report on a campaign of X-ray and soft γ-ray observations of the black hole candidate (BHC) H1743−322 (also named IGR J17464-3213), performed with the RXTE , INTEGRAL and Swift satellites. The source was observed during a short outburst between 2008 October 03 and November 16. The evolution of the hardness–intensity diagram throughout the outburst is peculiar, in that it does not follow the canonical pattern through all the spectral states (the so-called q-track pattern) seen during the outburst of black hole transients. On the contrary, the source only makes a transition from the hard state to the hard–intermediate state. After this transition, the source decreases in luminosity and its spectrum hardens again. This behaviour is confirmed by both spectral and timing analyses. This kind of outburst has been rarely observed before in a transient BHC. 相似文献
11.
D. C. Hannikainen R. W. Hunstead K. Wu V. McIntyre J. E. J. Lovell D. Campbell-Wilson M. L. McCollough J. Reynolds A. K. Tzioumis 《Monthly notices of the Royal Astronomical Society》2009,397(1):569-576
We revisit the discovery outburst of the X-ray transient XTE J1550−564 during which relativistic jets were observed in 1998 September, and review the radio images obtained with the Australian Long Baseline Array, and light curves obtained with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. Based on H i spectra, we constrain the source distance to between 3.3 and 4.9 kpc. The radio images, taken some 2 d apart, show the evolution of an ejection event. The apparent separation velocity of the two outermost ejecta is at least 1.3 c and may be as large as 1.9 c ; when relativistic effects are taken into account, the inferred true velocity is ≥ 0.8 c . The flux densities appear to peak simultaneously during the outburst, with a rather flat (although still optically thin) spectral index of −0.2. 相似文献
12.
R. Cornelisse R. Wijnands J. Homan 《Monthly notices of the Royal Astronomical Society》2007,380(4):1637-1641
We observed the neutron star X-ray transient 2S 1803−245 in quiescence with the X-ray satellite XMM–Newton , but did not detect it. An analysis of the X-ray bursts observed during the 1998 outburst of 2S 1803−245 gives an upper limit to the distance of ≤7.3 kpc, leading to an upper limit on the quiescent 0.5–10 keV X-ray luminosity of ≤2.8 × 1032 erg s−1 (3σ). Since the expected orbital period of 2S 1803−245 is several hours, this limit is not much higher than those observed for the quiescent black hole transients with similar orbital periods. 相似文献
13.
In 1998–1999, the X-ray transients XTE J2012+381 and XTE J1550-564 were observed with the TTM X-ray telescope onboard the Mir-Kvant astrophysical module. Spectral properties of these sources on the descent of the light curve after the secondary maxima of their outbursts are studied. Upper limits on the off-state flux are given. Comparison with other X-ray novae observed with the TTM telescope leads us to conclude that XTE J2012+381 and XTE J 1550-564 are soft X-ray novae. XTE J2012+381 probably belongs to the subclass of long-period X-ray transients. 相似文献
14.
Initial low/hard state, multiple jet ejections and X-ray/radio correlations during the outburst of XTE J1859+226 总被引：1，自引：0，他引：1
C.Brocksopp R. P.Fender M.McCollough G. G.Pooley M. P.Rupen R. M.Hjellming C. J.de la Force R. E.Spencer T. W. B.Muxlow S. T.Garrington S.Trushkin 《Monthly notices of the Royal Astronomical Society》2002,331(3):765-775
We have studied the 1999 soft X-ray transient outburst of XTE J1859+226 at radio and X-ray wavelengths. The event was characterized by strong variability in the disc, corona and jet – in particular, a number of radio flares (ejections) took place and seemed well-correlated with hard X-ray events. Apparently unusual for the canonical 'soft' X-ray transient, there was an initial period of low/hard state behaviour during the rise from quiescence but prior to the peak of the main outburst – we show that not only could this initial low/hard state be a ubiquitous feature of soft X-ray transient outbursts, but also it could be extremely important in our study of outburst mechanisms. 相似文献
15.
R. K. Manchanda 《Journal of Astrophysics and Astronomy》2000,21(1-2):39-52
We report the spectral measurement of GRS 1915+105 in the hard X-ray energy band of 20–140keV. The observations were made
on March 30th, 1997 during a quiescent phase of the source. We discuss the mechanism of emission of hard X-ray photons and
the evolution of the spectrum by comparing the data with earlier measurements and an axiomatic model for the X-ray source. 相似文献
16.
RXTE observations of the low/hard state X-ray outburst of the new X-ray transient SWIFT J1753.5−0127
We present the results of the analysis of Rossi X-ray Timing Explorer ( RXTE ) observations of the new X-ray transient, SWIFT J1753.5−0127, during its outburst in 2005 July. The source was caught at the peak of the burst with a flux of 7.19e-09 erg s−1 cm−2 in the 3–25 keV energy range and observed until it decreased by about a factor of 10. The photon index of the power-law component, which is dominant during the entire outburst, decreases from ∼1.76 to 1.6. However, towards the end of the observations the photon index is found to increase, indicating a softening of the spectra. The presence of an ultrasoft thermal component, during the bright phases of the burst, is clear from the fits to the data. The temperature associated with this thermal component is 0.4 keV. We believe that this thermal component could be due to the presence of an accretion disc. Assuming a distance of 8.5 kpc, L X / L Edd ≃ 0.05 at the peak of the burst, for a black hole of mass 10 M⊙ . The source is found to be locked in the low/hard state during the entire outburst and likely falls in the category of the X-ray transients that are observed in the low/hard state throughout the outburst. We discuss the physical scenario of the low/hard state outburst for this source. 相似文献
17.
H. Liang R.D. Ekers R.W. Hunstead E.E. Falco P. Shaver 《Monthly notices of the Royal Astronomical Society》2001,328(2):L23-L27
We present observations of the X-ray transient XTE J1118+480 during its low/hard X-ray state outburst in 2000, at radio and submillimetre wavelengths with the VLA, Ryle Telescope, MERLIN and JCMT. The high-resolution MERLIN observations reveal all the radio emission (at 5 GHz) to come from a compact core with physical dimensions smaller than 65 d (kpc) au. The combined radio data reveal a persistent and inverted radio spectrum, with spectral index ∼ +0.5. The source is also detected at 350 GHz, on an extrapolation of the radio spectrum. Flat or inverted radio spectra are now known to be typical of the low/hard X-ray state, and are believed to arise in synchrotron emission from a partially self-absorbed jet. Comparison of the radio and submillimetre data with reported near-infrared observations suggest that the synchrotron emission from the jet extends to the near-infrared, or possibly even optical regimes. In this case the ratio of jet power to total X-ray luminosity is likely to be P J L X ≫0.01, depending on the radiative efficiency and relativistic Doppler factor of the jet. Based on these arguments we conclude that during the period of our observations XTE J1118+480 was producing a powerful outflow which extracted a large fraction of the total accretion power. 相似文献
18.
Gloria Sala Jochen Greiner Eugenio Bottacini Frank Haberl 《Astrophysics and Space Science》2007,309(1-4):315-319
The new black hole candidate XTE J1817-330, discovered on 26 January 2006 with RXTE, was observed with XMM-Newton and INTEGRAL
in February and March 2006, respectively. The X-ray spectrum is dominated by the thermal emission of the accretion disk in
the soft band, with a low absorption column density (N
H=1.77(±0.01)×1021 cm−2) and a maximum disk temperature kT
max=0.68(±0.01) keV, plus a power law component, with the photon index decreasing from 2.66±0.02 to 1.98±0.07 between the two
observations. Several interstellar absorption lines are detected in the X-ray spectrum, corresponding to O I, O II, O III,
O VII and Fe XXIV. We constrain the distance to the system to be in the range 1–5 kpc.
相似文献
19.
C. Brocksopp K. E. McGowan H. Krimm O. Godet P. Roming K. O. Mason N. Gehrels M. Still K. Page A. Moretti C. R. Shrader S. Campana J. Kennea 《Monthly notices of the Royal Astronomical Society》2006,365(4):1203-1214
We present Swift observations of the black hole X-ray transient, GRO J1655−40, during the recent outburst. With its multiwavelength capabilities and flexible scheduling, Swift is extremely well suited for monitoring the spectral evolution of such an event. GRO J1655−40 was observed on 20 occasions and data were obtained by all instruments for the majority of epochs. X-ray spectroscopy revealed spectral shapes consistent with the 'canonical' low/hard, high/soft and very high states at various epochs. The soft X-ray source (0.3–10 keV) rose from quiescence and entered the low/hard state, when an iron emission line was detected. The soft X-ray source then softened and decayed, before beginning a slow rebrightening and then spending ∼3 weeks in the very high state. The hard X-rays (14–150 keV) behaved similarly but their peaks preceded those of the soft X-rays by up to a few days; in addition, the average hard X-ray flux remained approximately constant during the slow soft X-ray rebrightening, increasing suddenly as the source entered the very high state. These observations indicate (and confirm previous suggestions) that the low/hard state is key to improving our understanding of the outburst trigger and mechanism. The optical/ultraviolet light curve behaved very differently from that of the X-rays; this might suggest that the soft X-ray light curve is actually a composite of the two known spectral components, one gradually increasing with the optical/ultraviolet emission (accretion disc) and the other following the behaviour of the hard X-rays (jet and/or corona). 相似文献
20.
The source XTE J1901+014 discovered by the RXTE observatory during an intense outburst of hard radiation and classified as a fast X-ray transient is studied. The source’s spectral characteristics in the quiescent state have been investigated for the first time both in the soft X-ray energy range (3–20 keV) based on ROSAT and RXTE data and in the hard energy range (>20 keV) based on INTEGRAL data. A timing analysis of the source’s properties has revealed weak nonperiodic bursts of activity on time scales of several tens of seconds and two intense (～0.5–1 Crab) outbursts more than several hundred seconds in duration. Certain assumptions about the nature of the object under study are made. 相似文献