5,607 research outputs found
Spectroscopic observations of the eclipsing Polar MN Hya (RX J0929--24)
We present low--medium resolution optical spectroscopy of the eclipsing AM
Her system MN Hya (RX J0929--24). We determine the magnetic field strength at
the primary accretion region of the white dwarf to be 42MG from the spacing of
cyclotron features visible during ~0.4--0.7. From spectra taken during the
eclipse we find that the secondary has a M3--4 spectral type. Combined with the
eclipse photometry of Sekiguchi, Nakada & Bassett and an estimate of the
interstellar extinction we find a distance of ~300--700pc. We find unusual line
variations at phase ~0.9: Halpha is seen in absorption and emission. This is at
the same point in the orbital phase that a prominent absorption dip is seen in
soft X-rays.Comment: accepted by MNRAS, 7 pages, 5 fig
The X-ray eclipse of OY Car resolved with XMM-Newton: X-ray emission from the polar regions of the white dwarf
We present the XMM-Newton X-ray eclipse lightcurve of the dwarf nova OY Car.
The eclipse ingress and egress are well resolved for the first time in any
dwarf nova placing strong constraints on the size and location of the X-ray
emitting region. We find good fits to a simple linear eclipse model, giving
ingress/egress durations of 30+/-3 sec. Remarkably this is shorter than the
ingress/egress duration of the sharp eclipse in the optical as measured by Wood
et al. (1989) and ascribed to the white dwarf (43+/-2 sec). We also find that
the X-ray eclipse is narrower than the optical eclipse by 14+/-2 sec, which is
precisely the difference required to align the second and third contact points
of the X-ray and optical eclipses. We discuss these results and conclude that
X-ray emission in OY Car most likely arises from the polar regions of the white
dwarf.
Our data were originally reported by Ramsay et al (2001), but they did not
make a quantitative measurement of eclipse parameters. We have also corrected
important timing anomalies present in the data available at that time.Comment: 6 pages, 5 figures; accepted for publication in MNRA
Economic geology of the Avoca mineralized belt S.E. Ireland and Parys Mountain, Anglesey
Imperial Users onl
Disorder effect in low dimensional superconductors
The quasiparticle density of states (DOS), the energy gap, the superfluid
density , and the localization effect in the s- and d-wave
superconductors with non-magnetic impurity in two dimensions (2D) are studied
numerically. For strong (unitary) scatters, we find that it is the range of the
scattering potential rather than the symmetry of the superconducting pairing
which is more important in explaining the impurity dependences of the specific
heat and the superconducting transition temperature in Zn doped YBCO. The
localization length is longer in the d-wave superconducting state than in the
normal state, even in the vicinity of the Fermi energy.Comment: 2 pages, uuencoded compressed postscript file, IRC-940610
Continuous wave detector has wide frequency range
Portable battery-operated detector indicates the presence of steady state signals exceeding a predetermined value over a wide frequency range by the closure of output relay contacts. It was designed to monitor electronic equipment used in the Saturn 2 program
GALEX ultraviolet observations of stellar variability in the Hyades and Pleiades clusters
We present GALEX near ultraviolet (NUV:1750 - 2750A) and far ultraviolet
(FUV: 1350 - 1750A) imaging observations of two 1.2 degree diameter fields in
the Hyades and Pleiades open clusters in order to detect possible UV
variability of the member stars. We have performed a detailed software search
for short-term UV flux variability during these observations of the approx 400
sources detected in each of the Hyades and Pleiades fields to identify
flare-like (dMe) stellar objects. This search resulted in the detection of 16
UV variable sources, of which 13 can be directly associated with probable
M-type stars. The other UV sources are G-type stars and one newly discovered RR
Lyrae star, USNOB1.0 1069-0046050, of period 0.624 day and distance 4.5-7.0
kpc. Light curves of photon flux versus time are shown for 7 flare events
recorded on six probable dMe stars. UV energies for these flares span the range
2E27 to 5E29 erg, with a corresponding NUV variability change of 1.82 mag. Only
one of these flare events (on the star Cl* Melotte 25 LH129) can definitely be
associated with an origin on a member the Hyades cluster itself. Finally, many
of our M-type candidates show long periods of enhanced UV activity but without
the associated rapid increase in flux that is normally associated with a flare
event. However, the total UV energy output during such periods of increased
activity is greater than that of many short-term UV flares. These intervals of
enhanced low-level UV activity concur with the idea that, even in quiescence,
the UV emission from dMe stars may be related to a superposition of many small
flare events possessing a wide range of energies.Comment: PASP Submitte
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