740 research outputs found
Neutrinos from Accreting Neutron Stars
The magnetospheres of accreting neutron stars develop electrostatic gaps with
huge potential drops. Protons and ions, accelerated in these gaps along the
dipolar magnetic field lines to energies greater than 100 TeV, can impact onto
a surrounding accretion disc. A proton-induced cascade so develops, and
-emission is produced from charged pion decays. Using GEANT4, a computer
code that tracks particles produced in high energy collisions, we have
calculated the resulting -spectrum with extensive disc shower simulations.
We show that the -spectrum produced out of the proton beam is a power law.
We use this result to propose accretion-powered X-ray binaries (with highly
magnetized neutron stars) as a new population of point-like -sources for
km-scale detectors, such as ICECUBE. As a particular example we discuss the
case of A0535+26. We show that ICECUBE should find A0535+26 to be a periodic
-source: one for which the formation and loss of its accretion disc can be
fully detected. Finally, we briefly comment on the possibility that smaller
telescopes, like AMANDA, could also detect A0535+26 by folding observations
with the orbital period.Comment: 7 pages, 5 figures. Updates to match accepted version in Astrophys.
Discovery of a Transition to Global Spin-up in EXO 2030+375
EXO 2030+375, a 42-second transient X-ray pulsar with a Be star companion,
has been observed to undergo an outburst at nearly every periastron passage for
the last 13.5 years. From 1994 through 2002, the global trend in the pulsar
spin frequency was spin-down. Using RXTE data from 2003 September, we have
observed a transition to global spin-up in EXO 2030+375. Although the spin
frequency observations are sparse, the relative spin-up between 2002 June and
2003 September observations, along with an overall brightening of the outbursts
since mid 2002 observed with the RXTE ASM, accompanied by an increase in
density of the Be disk, indicated by infrared magnitudes, suggest that the
pattern observed with BATSE of a roughly constant spin frequency, followed by
spin-up, followed by spin-down is repeating. If so this pattern has
approximately an 11 year period, similar to the 15 +/- 3 year period derived by
Wilson et al. (2002) for the precession period of a one-armed oscillation in
the Be disk. If this pattern is indeed repeating, we predict a transition from
spin-up to spin-down in 2005.Comment: Accepted for publication in ApJ Letters, 4 pages, 5 figures, using
emulateapj.cl
The variability behavior of CoRoT M-giant Stars
For 6 years the Convection, Rotation, and Planetary Transits (CoRoT) space
mission has acquired photometric data from more than one hundred thousand point
sources towards and directly opposite from the inner and outer regions of the
Galaxy. The high temporal resolution of the CoRoT data combined with the wide
time span of the observations has enabled the study of short and long time
variations in unprecedented detail. From the initial sample of 2534 stars
classified as M-giants in the CoRoT databasis, we selected 1428 targets that
exhibit well defined variability, using visual inspection. The variability
period and amplitude of C1 stars (stars having Teff < 4200 K) were computed
using Lomb-Scargle and harmonic fit methods. The trends found in the V-I vs J-K
color-color diagram are in agreement with standard empirical calibrations for
M-giants. The sources located towards the inner regions of the Galaxy are
distributed throughout the diagram while the majority of the stars towards the
outer regions of the Galaxy are spread between the calibrations of M-giants and
the predicted position for Carbon stars. The stars classified as supergiants
follow a different sequence from the one found for giant stars. We also
performed a KS test of the period and amplitude of stars towards the inner and
outer regions of the Galaxy. We obtained a low probability that the two samples
come from the same parent distribution. The observed behavior of the
period-amplitude and period-Teff diagrams are, in general, in agreement with
those found for Kepler sources and ground based photometry, with pulsation
being the dominant cause responsible for the observed modulation. We also
conclude that short-time variations on M-Giant stars do not exist orare very
rare and the few cases we found are possibly related to biases or background
stars.Comment: 11 pages, 6 figure
Multi-periodicity of the Be star η Centauri from spectroscopic and photometric observations
Abstract. We present photometric data and 209 highresolution, high signal-to-noise ratio optical spectra of the Be star η Centauri obtained in 1993 and 1995, respectively. Time series analysis of these and other data, performed using the CLEAN, CLEANEST and Fourier Doppler Imaging techniques, show the presence of multiperiodic variations. They are interpreted in terms of low and high order non-radial pulsation modes. A strong frequency of 1.29 c/d is detected in line profile and photometric variations. It is attributed to a mode with l = 2. Other high amplitude signals present in spectroscopic data are 1.78 c/d, 3.82 c/d and 4.51 c/d. A frequency of 1.48 c/d appearing in spectroscopic data is compatible with the 1.56 c/d periodicity largely dominant in observations taken prior to 1993. The corresponding "superperiods" for four of the frequencies are commensurate at the 8% level. The star showed period and non-radial pulsation degree variations in timescales as short as ∼ 1.5 hour. The dominant mode apparently alternates between l = 2 and l = 4 every other day during the eight day time span. This could be a modulation linked to the superperiod or to the stellar rotation. The main periodicities detected in our analysis are compatible with theoretical unstable g modes in SPB variables. Short time scale variability (1 − 3 hr), typical of high-order p modes is also systematically present
Photometric and spectroscopic variability of the B5IIIe star HD 171219
We analyzed the star HD171219, one of the relatively bright Be stars observed in the seismo field of the CoRoT satellite, in order to determine its physical and pulsation characteristics. Classical Be stars are main-sequence objects of mainly B-type, whose spectra show,or have shown at some epoch, Balmer lines in emission and an infrared excess. Both characteristics are attributed to an equatorially concentrated circumstellar disk fed by non-periodic mass-loss episodes (outbursts). Be stars often show nonradial pulsation gravity modes and, as more recently discovered, stochastically excited oscillations. Applying the CLEANEST algorithm to the high-cadence and highly photometrically precise measurements of the HD171219 light curve led us to perform an unprecedented detailed analysis of its nonradial pulsations. Tens of frequencies have been detected in the object compatible with nonradial g-modes. Additional ighresolution ground-based spectroscopic observations were obtained at La Silla (HARPS) and Haute Provence (SOPHIE) observatories during the month preceding CoRoT observations. Additional information was obtained from low-resolution spectra from the BeSS database. From spectral line fitting we determined physical parameters of the star, which is seen equator-on (i = 90 ). We also found in the ground data the same frequencies as in CoRoT data. Additionally, we analyzed the circumstellar activity through the traditional method of violet to red emission H line variation. A quintuplet was identified at approximately 1:113 c d\u1000001 (12.88 Hz) with a separation of 0:017 c d\u1000001 that can be attributed to a pulsation degree ` 2. The light curve shows six small- to medium-scale outbursts during the CoRoT observations. The intensity of the main frequencies varies after each outburst, suggesting a possible correlation between the nonradial pulsations regime and the feeding of the envelope
Discovery of a QPO in the X-ray pulsar 1A 1118-615: correlated spectral and aperiodic variability
Our goal is to investigate the X-ray timing and spectral variability of the
high-mass X-ray binary 1A 1118-615 during a type-II outburst. We performed a
detailed color, spectral and timing analysis of a giant outburst from 1A
1118-615, using RXTE data. Results. We report the discovery of a variable
quasi-periodic oscillation (QPO) in the power spectral density of 1A 1118-615,
with a centroid frequency of ~0.08 Hz. The centroid frequency of the QPO
correlates with the X-ray flux, as expected according to the most accredited
models for QPO production. For energies above ~4 keV, the QPO rms variability
decreases as the energy increases. Pulse profiles display energy dependence,
with a two-peak profile at lower energies, and a single peak at higher
energies. From spectral analysis, we confirm the presence of a cyclotron
absorption feature at ~60 keV, the highest value measured for an X-ray pulsar.
We find that the spectral parameters (photon index, cutoff energy, iron
fluorescence line strength) display a marked dependence with flux. We detect
two different levels of neutral hydrogen column density, possibly due to the Be
companion activity. We report for the first time a correlation between the
timing and spectral parameters in an X-ray pulsar. All the correlations found
between spectral/timing parameters and X-ray flux are present up to a flux of
~6x10^-9 erg cm^-2 s^-1, when a saturation level is reached. We propose that
the saturation observed corresponds to the minimum extent of the neutron star
magnetosphere. We estimate the magnetic field of the neutron star from two
independent ways, using results from spectral (cyclotron line energy) and
timing (QPO frequency) analysis, obtaining consistent values, of ~7-8x10^12 G.
Results from the comprehensive spectral and timing analysis are discussed in
comparison with other X-ray pulsars.Comment: 9 pages, 11 figures. Accepted for publication in Astronomy and
Astrophysic
Fundamental parameters of Be stars located in the seismology fields of COROT
In preparation for the COROT space mission, we determined the fundamental
parameters (spectral type, temperature, gravity, vsini) of the Be stars
observable by COROT in its seismology fields (64 Be stars). We applied a
careful and detailed modeling of the stellar spectra, taking into account the
veiling caused by the envelope, as well as the gravitational darkening and
stellar flattening due to rapid rotation. Evolutionary tracks for fast rotators
were used to derive stellar masses and ages. The derived parameters will be
used to select Be stars as secondary targets (i.e. observed for 5 consecutive
months) and short-run targets of the COROT mission. Furthermore, we note that
the main part of our stellar sample is falling in the second half of the main
sequence life time, and that in most cases the luminosity class of Be stars is
inaccurate in characterizing their evolutionary status.Comment: 25 pages, 9 figures, Accepted for publication in A&
Discovery of a cluster of galaxies behind the Milky Way: X-ray and optical observations
We report the discovery of Cl 2334+48, a rich cluster of galaxies in the Zone
of Avoidance, identified in public images from the XMM-Newton archive. We
present the main properties of this cluster using the XMM-Newton X-ray data,
along with new optical spectroscopic and photometric observations. Cl 2334+48
is located at z = 0.271 +/- 0.001, as derived from the optical spectrum of the
brightest member galaxy. Such redshift agrees with a determination from the
X-ray spectrum (z = 0.263 (+0.012/-0.010)), in which an intense emission line
is matched to the rest wavelength of the Fe Kalpha complex. Its intracluster
medium has a plasma temperature of 4.92 (+0.50/-0.48) keV, sub-solar abundance
(0.38 +/- 0.12 Zsun), and a bolometric luminosity of 3.2 x 10^44 erg/s. A
density contrast delta = 2500 is obtained in a radius of 0.5 Mpc/h70, and the
corresponding enclosed mass is 1.5 x 10^14 Msun. Optical images show an
enhancement of g'-i' > 2.5 galaxies around the central galaxy, as expected if
these were cluster members. The central object is a luminous E-type galaxy,
which is displaced ~ 40 kpc/h70 from the cluster X-ray center. In addition, it
has a neighbouring arc-like feature (~ 22" or 90 kpc/h70 from it), probably due
to strong gravitational lensing. The discovery of Cl 2334+48 emphasises the
remarkable capability of the XMM-Newton to reveal new clusters of galaxies in
the Zone of Avoidance.Comment: 9 pages, 11 figures, Accepted for publication in A&A (on July 12,
2006
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