801 research outputs found
Photometric Variability in the Faint Sky Variability Survey
The Faint Sky Variability Survey (FSVS) is aimed at finding photometric
and/or astrometric variable objects between 16th and 24th mag on time-scales
between tens of minutes and years with photometric precisions ranging from 3
millimag to 0.2 mag. An area of 23 deg, located at mid and high Galactic
latitudes, was covered using the Wide Field Camera (WFC) on the 2.5-m Isaac
Newton Telescope (INT) on La Palma. Here we present some preliminary results on
the variability of sources in the FSVS.Comment: 4 pages, 3 figures, to appear in 14th European Workshop on White
Dwarfs, ASP Conference Series, eds. D. Koester, S. Moehle
The unusual 2006 dwarf nova outburst of GK Perseii
The 2006 outburst of GK Perseii differed significantly at optical and
ultraviolet wavelengths from typical outbursts of this object. We present
multi-wavelength (X-ray, UV and optical) Swift and AAVSO data, giving
unprecedented broad-band coverage of the outburst, allowing us to follow the
evolution of the longer-than-normal 2006 outburst across these wavelengths. In
the optical and UV we see a triple-peaked morphology with maximum brightness
~1.5 magnitudes lower than in previous years. In contrast, the peak hard X-ray
flux is the same as in previous outbursts. We resolve this dichotomy by
demonstrating that the hard X-ray flux only accounts for a small fraction of
the total energy liberated during accretion, and interpret the optical/UV
outburst profile as arising from a series of heating and cooling waves
traversing the disc, caused by its variable density profile.Comment: 9 pages, 7 figures, accepted for publication in MNRA
Changes in Number and Weight of Wheat and Triticale Grains to Manipulation in Source-Sink Relationship
The source-sink ratio experimental manipulation has helped to define whether a crop is limited by source or sink or co-limited by both. There is no evidence in triticale of source-sink manipulations effects on yield and yield components. Two experiments were accomplished during 2008 and 2009 growing seasons at the Universidad AutĂłnoma del Estado de MĂ©xico, MĂ©xico, and one in 2010 at the National Institute of Agricultural Technology in Pergamino, Argentina. Two triticale cultivars (line 4 and 7) and one wheat cultivar (Tollocan) were used. Source-sink relations were modified at anthesis by thinning, degraining, shading, and total defoliation procedures. Changes in the source-sink relation affected yields in both species differentially. The changes in yield due to cultivars and treatments were explained mainly by the number of grains rather than by their individual grain weight. The number of grains was affected by all treatments in both species, while the individual grain weight was increased by thinning and degraining mainly in triticale. A greater number of fertile florets in triticale were associated with their higher rate of abortion compared to wheat. These results could help to better understand crop management and genetic improvement.Fil: Ballesteros Rodriguez, E.. Universidad Nacional AutĂłnoma de MĂ©xico; MĂ©xicoFil: Martinez Rueda, C.G.. Universidad Nacional AutĂłnoma de MĂ©xico; MĂ©xicoFil: Morales Rosales, E.J.. Universidad Nacional AutĂłnoma de MĂ©xico; MĂ©xicoFil: Estrada Campuzano, G.. Universidad Nacional AutĂłnoma de MĂ©xico; MĂ©xicoFil: GonzĂĄlez, Fernanda Gabriela. Instituto Nacional de TecnologĂa Agropecuaria. Centro Regional Buenos Aires Norte. EstaciĂłn Experimental Agropecuaria Pergamino; Argentina. Consejo Nacional de Investigaciones CientĂficas y TĂ©cnicas; Argentin
PG 1018â047 : the longest period subdwarf B binary
About 50 per cent of all known hot subdwarf B stars (sdBs) reside in close (short-period) binaries, for which common-envelope ejection is the most likely formation mechanism. However, Han et al. predict that the majority of sdBs should form through stable mass transfer leading to long-period binaries. Determining orbital periods for these systems is challenging and while the orbital periods of âŒ100 short-period systems have been measured, there are no periods measured above 30 d. As part of a large programme to characterize the orbital periods of sdB binaries and their formation history, we have found that PG 1018â047 has an orbital period of 759.8 ± 5.8 d, easily making it the longest period ever detected for a sdB binary. Exploiting the Balmer lines of the subdwarf primary and the narrow absorption lines of the companion present in the spectra, we derive the radial velocity amplitudes of both stars, and estimate the mass ratio MMS/MsdB= 1.6 ± 0.2. From the combination of visual and infrared photometry, the spectral type of the companion star is determined to be mid-K
DE Canum Venaticorum: A Bright, Eclipsing Red DwarfâWhite Dwarf Binary
Close white dwarf - red dwarf binaries must have gone through a common-envelope phase during their evolution. DE CVn is a detached white dwarf - red dwarf binary with a relatively short (~8.7 hours) orbital period. Its brightness and the presence of eclipses makes this system ideal for a more detailed study. From a study of photometric and spectroscopic observations of DE CVn we derive the system parameters which we discuss in the frame work of common-envelope evolution. Photometric observations of the eclipses are used to determine an accurate ephemeris. From a model fit to an average low-resolution spectrum of DE CVn we constrain the temperature of the white dwarf and the spectral type of the red dwarf. The eclipse light curve is analysed and combined with the radial velocity curve of the red dwarf determined from time-resolved spectroscopy to derive constraints on the inclination and the masses of the components in the system
The binary properties of the pulsating subdwarf B eclipsing binary PG 1336-018 (NY Virginis)
Aims. We present an unbiased orbit solution and mass determination of the components of the eclipsing binary PG1336â018 as a critical test for the formation scenarios of subdwarf B stars.
Methods. We obtained high-resolution time series VLT/UVES spectra and high-speed multicolour VLT/ULTRACAM photometric
observations of PG1336â018, a rapidly pulsating subdwarf B star in a short period eclipsing binary.
Results. Combining the radial velocity curve obtained from the VLT/UVES spectra with the VLT/ULTRACAM multicolour
lightcurves, we determined numerical orbital solutions for this eclipsing binary. Due to the large number of free parameters and their strong correlations, no unique solution could be found, only families of solutions. We present three solutions of equal statistical
significance, two of which are compatible with the primary having gone through a core He-flash and a common-envelope phase described by the α-formalism. These two models have an sdB primary of 0.466 M and 0.389 M, respectively. Finally, we report the detection of the Rossiter-McLaughlin effect for PG1336â018
Short timescale variability in the Faint Sky Variability Survey
We present the V band variability analysis of the point sources in the Faint
Sky Variability Survey on time scales from 24 minutes to tens of days. We find
that about one percent of the point sources down to V = 24 are variables. We
discuss the variability detection probabilities for each field depending on
field sampling, amplitude and timescale of the variability. The combination of
colour and variability information allows us to explore the fraction of
variable sources for different spectral types. We find that about 50 percent of
the variables show variability timescales shorter than 6 hours. The total
number of variables is dominated by main sequence sources. The distribution of
variables with spectral type is fairly constant along the main sequence, with 1
per cent of the sources being variable, except at the blue end of the main
sequence, between spectral types F0--F5, where the fraction of variable sources
increases to about 2 percent. For bluer sources, above the main sequence, this
percentage increases to about 3.5. We find that the combination of the sampling
and the number of observations allows us to determine the variability
timescales and amplitudes for a maximum of 40 percent of the variables found.
About a third of the total number of short timescale variables found in the
survey were not detected in either B or/and I. These show a similar variability
timescale distribution to that found for the variables detected in all three
bands.Comment: 14 pages, 12 figures and 4 tables. Accepted for publication in MNRA
Compton Scattering of Fe K alpha Lines in Magnetic Cataclysmic Variables
Compton scattering of X-rays in the bulk flow of the accretion column in
magnetic cataclysmic variables (mCVs) can significantly shift photon energies.
We present Monte Carlo simulations based on a nonlinear algorithm demonstrating
the effects of Compton scattering on the H-like, He-like and neutral Fe K alpha
lines produced in the post-shock region of the accretion column. The peak line
emissivities of the photons in the post-shock flow are taken into consideration
and frequency shifts due to Doppler effects are also included. We find that
line profiles are most distorted by Compton scattering effects in strongly
magnetized mCVs with a low white dwarf mass and high mass accretion rate and
which are viewed at an oblique angle with respect to the accretion column. The
resulting line profiles are most sensitive to the inclination angle. We have
also explored the effects of modifying the accretion column width and using a
realistic emissivity profile. We find that these do not have a significant
overall effect on the resulting line profiles. A comparison of our simulated
line spectra with high resolution Chandra/HETGS observations of the mCV GK Per
indicates that a wing feature redward of the 6.4 keV line may result from
Compton recoil near the base of the accretion column.Comment: Accepted for publication in MNRAS, 10 pages with 8 figure
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
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