5,728 research outputs found
XMM-Newton observations of three short period polars: V347 Pav, GG Leo and EU UMa
We present phase-resolved XMM_Newton data of three short period polars: V347
Pav, GG Leo and EU UMa. All three systems show one dominant accretion region
which is seen for approximately half of the orbital cycle. GG Leo shows a
strong dip feature in its X-ray and UV light curves which is due to absorption
of X-rays from the accretion site by the accretion stream. The emission in the
case of EU UMa is dominated by soft X-rays: its soft/hard X-ray ratio is
amongst the highest seen in these objects. In contrast, GG Leo and V347 Pav
shows a ratio consistent with that predicted by the standard shock model. We
infer the mass of the white dwarf and explore the affect of restricting the
energy range on the derived parameters.Comment: accepted MNRA
White dwarf masses in magnetic cataclysmic variables: Multi-temperature fits to Ginga data
One method of obtaining the mass of the white dwarf in magnetic cataclysmic variables (mCVs) is through their hard X-ray spectra. However, previous mass estimates using this method give lower limits because the temperature of the plasma in the post-shock region (where the hard X-rays are emitted) is lower than the temperature of the shock itself. In AM Her systems, the additional cooling of the post-shock plasma by cyclotron emission will further lower the derived mass. Here we present estimates of the masses of the white dwarf in 13 mCVs derived using Ginga data and a model in which X-rays are emitted from a multi-temperature emission region with the appropriate temperature and density profile. We include in the model reflection from the surface of the white dwarf and a partially ionized absorber. We are able to achieve good fits to the data. We compare the derived masses with previous estimates and the masses for larger samples of isolated white dwarfs and those in CVs
Molecular Hydrogen emission from disks in the eta Chamaeleontis cluster
Disks in the 6 Myr old cluster eta Chamaeleontis were searched for emission
from hot H2. Around the M3 star ECHAJ0843.3-7905 we detect circumstellar gas
orbiting at ~2 AU. If the gas is UV-excited, the ro-vibrational line traces a
hot gas layer supported by a disk of mass ~0.03Msolar, similar to the minimum
mass solar nebula. Such a gas reservoir at 6 Myr would promote the formation
and inwards migration of gas giant planets.Comment: Accepted for publication in MNRAS. 9 page
X-ray spectroscopy and photometry of the long-period polar AI Tri with XMM-Newton
Context. The energy balance of cataclysmic variables with strong magnetic
fields is a central subject in understanding accretion processes on magnetic
white dwarfs. With XMM-Newton, we perform a spectroscopic and photometric study
of soft X-ray selected polars during their high states of accretion. Aims. On
the basis of X-ray and optical observations of the magnetic cataclysmic
variable AI Tri, we derive the properties of the spectral components, their
flux contributions, and the physical structure of the accretion region in soft
polars. Methods. We use multi-temperature approaches in our xspec modeling of
the spectra to describe the physical conditions and the structures of the
post-shock accretion flow and the accretion spot on the white-dwarf surface. In
addition, we investigate the accretion geometry of the system by a timing
analysis of the photometric data. Results. Flaring soft X-ray emission from the
heated surface of the white dwarf dominates the X-ray flux during roughly 70%
of the binary cycle. This component deviates from a single black body and can
be described by a superimposition of mildly absorbed black bodies with a
Gaussian temperature distribution. In addition, weaker hard X-ray emission is
visible nearly all the time. The spectrum from the cooling post-shock accretion
flow is most closely fitted by a combination of thermal plasma mekal models
with temperature profiles adapted from prior stationary two-fluid hydrodynamic
calculations. The soft X-ray light curves show a dip during the bright phase,
which can be interpreted as self-absorption in the accretion stream.
Phase-resolved spectral modeling supports the picture of one-pole accretion and
self-eclipse. One of the optical light curves corresponds to an irregular mode
of accretion. During a short XMM-Newton observation at the same epoch, the
X-ray emission of the system is clearly dominated by the soft component.Comment: A&A, in press; 11 pages, 9 figures, 3 table
Investigating the Rotational Phase of Stellar Flares on M dwarfs Using K2 Short Cadence Data
We present an analysis of K2 short cadence data of 34 M dwarfs which have
spectral types in the range M0 - L1. Of these stars, 31 showed flares with a
duration between 10-90 min. Using distances obtained from Gaia DR2
parallaxes, we determined the energy of the flares to be in the range
erg. In agreement with previous studies
we find rapidly rotating stars tend to show more flares, with evidence for a
decline in activity in stars with rotation periods longer than 10 days.
The rotational modulation seen in M dwarf stars is widely considered to result
from a starspot which rotates in and out of view. Flux minimum is therefore the
rotation phase where we view the main starspot close to the stellar disk
center. Surprisingly, having determined the rotational phase of each flare in
our study we find none show any preference for rotational phase. We outline
three scenarios which could account for this unexpected finding. The
relationship between rotation phase and flare rate will be explored further
using data from wide surveys such as NGTS and TESS.Comment: Accepted main Journal MNRA
A search for stellar X-ray sourcesin the Sagittarius and Carina dwarf galaxies - I: X-ray observations
ROSAT observations found no convincing evidence for X-ray sources located in local dwarf spheroidal galaxies (dSph). Now with more sensitive instruments on board Chandra and XMM-Newton we can reach fainter luminosity levels. We report on an observation of the Sagittarius (Sgr) dSph made using Chandra and an observation of the Carina (Car) dSph made using XMM-Newton. Our observations are sensitive to sources with X-ray luminosities in the 0.1-10 keV band of \~1x10^{32 ergs/s and 3x10^34 ergs/s for the Sgr and Car fields respectively. We have identified a total of 80 sources in the Sgr field and 53 sources in the Car field. Although the source numbers are roughly consistent with the expected number of background AGN, we found a small fraction of X-ray sources which were soft and could be located in the host dSph. Follow-up optical/IR observations may help to identify their optical counterparts and hence determine their nature
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