14,544 research outputs found
The evolution of the high energy tail in the quiescent spectrum of the soft X-ray transient Aql X-1
A moderate level of variability has been detected in the quiescent luminosity
of several neutron star soft X-ray transients. Spectral variability was first
revealed by Chandra observations of Aql X-1 in the four months that followed
the 2000 X-ray outburst. By adopting the canonical model for quiescent spectrum
of soft X-ray transients, i.e. an absorbed neutron star atmosphere model plus a
power law tail, Rutledge et al. (2002a) concluded that the observed spectral
variations can be ascribed to temperature variations of the neutron star
atmosphere. These results can hardly be reconciled with the neutron star
cooling that is expected to take place in between outbursts (after deep crustal
heating in the accretion phase). Here we reanalyse the Chandra spectra of Aql
X-1, together with a long BeppoSAX observation in the same period, and propose
a different interpretation of the spectral variability: that this is due to
correlated variations of the power law component and the column density (>5, a
part of which might be intrinsic to the source), while the temperature and flux
of the neutron star atmospheric component remained unchanged. This lends
support to the idea that the power law component arises from emission at the
shock between a radio pulsar wind and inflowing matter from the companion star.Comment: 6 pages, 2 figures. Accepted for publication on Ap
Structure of l-Benzyl-2,2,3,3-tetramethyl-l-phenylphosphetanium Bromide, a Cyelobutane Derivative
Doppler tomography of the transient X-ray binary Centaurus X-4 in quiescence
We present ESO-NTT low resolution spectroscopy of the neutron star X-ray
transient Cen X-4 in quiescence over a complete orbital cycle. Our data reveal
the presence of a K3-7 V companion which contributes 63% to the 5600-6900A flux
and orbits the neutron star with a velocity semi-amplitude of K_2=145.8 +/- 1.0
km s^{-1}. This, combined with a previous determination of the inclination
angle and mass ratio, yields a neutron star and companion mass of M_1=1.5 +/-
1.0 M_Sun and M_2=0.31 +/- 0.27 M_Sun, respectively. The mass donor is thus
undermassive for the inferred spectral type indicating it is probably evolved,
in agreement with previous studies. Doppler tomography of the H_alpha line
shows prominent emission located on the companion and a slightly asymmetric
accretion disc distribution similar to that seen in systems with precessing
eccentric discs. Strong H_alpha emission from the companion can be explained by
X-ray irradiation from the primary. No evidence is found for a hot spot in
H_alpha, whereas one is revealed via Doppler tomography of the HeI lines. This
can be interpreted as the hot spot and outer regions of the disc being at a
higher temperature than in other systems.Comment: 9 pages, 5 figures, accepted for publication in A&
Further Constraints on Thermal Quiescent X-ray Emission from SAX J1808.4-3658
We observed SAX J1808.4-3658 (1808), the first accreting millisecond pulsar,
in deep quiescence with XMM-Newton and (near-simultaneously) Gemini-South. The
X-ray spectrum of 1808 is similar to that observed in quiescence in 2001 and
2006, describable by an absorbed power-law with photon index 1.74+-0.11 and
unabsorbed X-ray luminosity L_X=7.9+-0.7*10^{31} ergs/s, for N_H=1.3*10^{21}
cm^{-2}. Fitting all the quiescent XMM-Newton X-ray spectra with a power-law,
we constrain any thermally emitting neutron star with a hydrogen atmosphere to
have a temperature less than 30 eV and L_{NS}(0.01-10 keV)<6.2*10^{30} ergs/s.
A thermal plasma model also gives an acceptable fit to the continuum. Adding a
neutron star component to the plasma model produces less stringent constraints
on the neutron star; a temperature of 36^{+4}_{-8} eV and L_{NS}(0.01-10
keV)=1.3^{+0.6}_{-0.8}*10^{31} ergs/s. In the framework of the current theory
of neutron star heating and cooling, the constraints on the thermal luminosity
of 1808 and 1H 1905+000 require strongly enhanced cooling in the cores of these
neutron stars.
We compile data from the literature on the mass transfer rates and quiescent
thermal flux of the largest possible sample of transient neutron star LMXBs. We
identify a thermal component in the quiescent spectrum of the accreting
millisecond pulsar IGR J00291+5934, which is consistent with the standard
cooling model. The contrast between the cooling rates of IGR J00291+5934 and
1808 suggests that 1808 may have a significantly larger mass. This can be
interpreted as arising from differences in the binary evolution history or
initial neutron star mass in these otherwise similar systems.Comment: ApJ in press, 7 pages, 2 color figure
The quiescent X-ray emission of three transient X-ray pulsars
We report on BeppoSAX and Chandra observations of three Hard X-Ray Transients
in quiescence containing fast spinning (P<5 s) neutron stars: A 0538-66, 4U
0115+63 and V 0332+53. These observations allowed us to study these transients
at the faintest flux levels thus far. Spectra are remarkably different from the
ones obtained at luminosities a factor >10 higher, testifying that the
quiescent emission mechanism is different. Pulsations were not detected in any
of the sources, indicating that accretion of matter down to the neutron star
surface has ceased. We conclude that the quiescent emission of the three X-ray
transients likely originates from accretion onto the magnetospheric boundary in
the propeller regime and/or from deep crustal heating resulting from
pycnonuclear reactions during the outbursts.Comment: Accepted for publication on ApJ (5 pages and 2 figures
A search for evidence of irradiation in Centaurus X-4 during quiescence
We present a study of the neutron star X-Ray Transient Cen X-4. Our aim is to
look for any evidence of irradiation of the companion with a detailed analysis
of its radial velocity curve, relative contribution of the donor star and
Doppler tomography of the main emission lines. To improve our study all our
data are compared with a set of simulations that consider different physical
parameters of the system, like the disc aperture angle and the mass ratio. We
conclude that neither the radial velocity curve nor the orbital variation of
the relative donor's contribution to the total flux are affected by
irradiation. On the other hand, we do see emission from the donor star at
H and HeI 5876 which we tentatively attribute to irradiation effects.
In particular, the H emission from the companion is clearly
asymmetric and we suggest is produced by irradiation from the hot-spot.
Finally, from the velocity of the HeI 5876 spot we constrain the disc opening
angle to alpha=7-14 deg.Comment: 4 pages, 5 figures, accepted for publication in A&A as a R
Swift monitoring of the new accreting millisecond X-ray pulsar IGRJ17511-3057 in outburst
A new accreting millisecond X-ray pulsar, IGR J17511-3057, was discovered in
outburst on 2009 September 12 during the INTEGRAL Galactic bulge monitoring
programme. To study the evolution of the source X-ray flux and spectral
properties during the outburst, we requested a Swift monitoring of
IGRJ17511-3057. In this paper we report on the results of the first two weeks
of monitoring the source. The persistent emission of IGR J17511-3057 during the
outburst is modeled well with an absorbed blackbody (kT~0.9 keV) and a
power-law component (photon index~1-2), similar to what has been observed from
other previously known millisecond pulsars. Swift also detected three type-I
Xray bursts from this source. By assuming that the peak luminosity of these
bursts is equal to the Eddington value for a pure helium type-I X-ray burst, we
derived an upper limit to the source distance of ~10 kpc. The theoretical,
expected recurrence time of the bursts according to the helium burst hypothesis
is 0.2-0.9 days, in agreement with the observations.Comment: Accepted for publication in A&A Letters. V2: corrected some typos and
added one referenc
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