[PDF] Top 20 The field white dwarf mass distribution

... high- mass IMF since they still include bright intermediate-mass stars ...the field white dwarf mass distribution could still provide information about the IMF of local ... See full document

... cooler white dwarf (pri- mary) is of an unusually low surface ...cool white dwarf plus a hotter and rather massive white dwarf that is rapidly ...detailed white ... See full document

... All of these data were reduced using the ULTRACAM pipeline software. Debiassing, flatfielding and sky back- ground subtraction were performed in the standard way. The source flux was determined with aperture photometry ... See full document

... the white dwarf is accurately described by a theoretical mass–radius relation; that the whole of the white dwarf is visible out of eclipse and that the donor star fills its Roche ... See full document

... invoked the existence of an accretion disc wind which dominates the Balmer emission and remains unobscured during primary eclipse. Williams (1989) has suggested that the accretion disc is disrupted by a strong magnetic ... See full document

... Full details of our data-analysis procedures are given in the online supplementary material (29), but we summarize them here. We used the flat-fielded images produced by the Space Telescope Science Institute pipeline ... See full document

... galactic white dwarfs have been studied on numerous occasions with several ...of white dwarfs (Anselowitz et ...in white dwarf kinematics was also prompted by the suggestion that halo ... See full document

... cool white dwarf. Modeling its spectral energy distribution suggests that its mass is ...the white dwarf is > 2 σ , which is discrepant with that of the primary star under ... See full document

... All of these data were reduced using the ULTRACAM pipeline software. Debiassing, flatfielding and sky back- ground subtraction were performed in the standard way. The source flux was determined with aperture photome- try ... See full document

... the mass transfer rate can drop by an order of magnitude or more (see Warner 1999 and Hessman et ...common dwarf novae systems (Osaki, ...the mass transfer rate due to starspots on the secondaries ... See full document

... displaying the typical characteristics of a CV near its period minimum. Crucially, it was the first CV discovered to contain a pulsating WD (van Zyl et al. 2004), by analogy with field WD pulsators that lie in the ... See full document

... around white dwarf WD ...of white dwarf's precursors' wind and the ambient interstellar matter is thoroughly ...this, distribution of the relative flux density of each pixel of the images are ... See full document

... the distribution of the mass ratio and inclination values from our fits in Figure ...primary white dwarf, and the main eclipse in the light curve is the eclipse of this ...the white ... See full document

... uniform distribution the initial mean anomalies for all bodies and ...body’s mass, and we lineally randomized the masses of all fragments for every simulation between those ...the mass of the parent ... See full document

... the white dwarf during the outburst would be slowly extracted by the interaction of the magnetic fi eld with the disk during accretion ...example, mass and angular momentum loss during nova outbursts ... See full document

... convection sets in and modes are driven mostly through the convective driving mechanism. Given that the driving/damping zone in these stars is rather confined near the base of the superficial convection zone, and given ... See full document

... pulse periods of the light curves are the same, the pulse profiles suggest that the UV and the X-ray emission are from di ff erent location within the system. The double-peaked profile of the UV light curve is associated ... See full document

... Angular momentum loss drives the evolution of close binary stars. For short period systems (< 3 hours) gravitational radiation (Kraft et al. 1962; Faulkner 1971) dom- inates whilst for longer period systems (> 3 ... See full document

... Finally, we list the members of the most populated subgroup of white dwarf pulsators with hydrogen atmospheres, the ‘classical’ ZZ Ceti stars, in Table 4. These objects can be treated as products of ... See full document

... The last decade has seen a remarkable increase in our knowledge of the bottom of the main-sequence and of the low-mass stellar and sub-stellar (brown dwarf) population of the solar neighbourhood. Two new ... See full document