The rotational velocity of the sdOB primary of the eclipsing binary system LB 3459 (AA Dor)

We present an analysis of the rotational velocity of the primary of LB 3459 based on 107 new high-resolution and high-S/N ESO VLT UVES spectra. 105 of them cover a complete orbital period (0.26 d) of this binary system. We have determined an orbital period of P = 22600.702 +/- 0.005 sec, a radial velocity amplitude of A_1 = 39.19 +/- 0.05 km/sec, and T_0 = 2451917.152690 +/- 0.000005. From simulations of the He II 4686A line profile (based on NLTE model atmosphere calculations), we derive v_rot = 47 +/- 5 km/sec. We present an animation which shows the orbital movement of the binary system, its synthetic lightcurve, and compares the phase-dependent variation of the predicted with the observed He II 4686A line profile. The radius of the cool component is almost the same size like Jupiter but its mass is about 70 times higher than Jupiter's mass. Thus, from its present mass (M_2 = 0.066 M_sun), the secondary of LB 3459 lies formally within the brown-dwarf mass range (0.013 - 0.08 M_sun). It might be a former planet which has survived the previous common-envelope phase and even has gained mass.Comment: 7 pages, 11 Postscript figures, to appear in A&

The mass ratio and the orbital parameters of the sdOB binary AA Doradus

The time sequence of 105 spectra covering one full orbital period of AA Dor has been analyzed. Direct determination of Vsini for the sdOB component from 97 spectra outside of the eclipse for the lines MgII 4481 A and SiIV 4089 A clearly indicated a substantially smaller value than estimated before. Detailed modelling of line profile variations for 8 spectra during the eclipse for the MgII 4481 A line, combined with the out-of-eclipse fits, gave Vsini = 31.8+/-1.8 km/s. The previous determinations of Vsini, based on the HeII 4686 A line, appear to be invalid because of the large natural broadening of the line. With the assumption of the solid-body, synchronous rotation of the sdOB primary, the measured values of the semi-amplitude K1 and Vsini lead to the mass ratio q = 0.213+/-0.013 which in turn gives K2 and thus the masses and radii of both components. The sdOB component appears to be less massive than assumed before, M1 = 0.25+/-0.05 Msol, but the secondary has its mass-radius parameters close to theoretically predicted for a brown dwarf, M2 = 0.054+/-0.010 Msol and R2 = 0.089+/-0.005 Rsol. Our results do not agree with the recent determination of Vuckovic et al. 2008 based on a K2 estimate from line-profile asymmetries.Comment: Accepted by MNRA

Subaru and Swift observations of V652 Herculis: resolving the photospheric pulsation

High-resolution spectroscopy with the Subaru High Dispersion Spectrograph, and Swift ultraviolet photometry are presented for the pulsating extreme helium star V652 Her. Swift provides the best relative ultraviolet photometry obtained to date, but shows no direct evidence for a shock at ultraviolet or X-ray wavelengths. Subaru has provided high spectral and high temporal resolution spectroscopy over six pulsation cycles (and eight radius minima). These data have enabled a line-by-line analysis of the entire pulsation cycle and provided a description of the pulsating photosphere as a function of optical depth. They show that the photosphere is compressed radially by a factor of at least 2 at minimum radius, that the phase of radius minimum is a function of optical depth and the pulse speed through the photosphere is between 141 and 239 km s−1 (depending how measured) and at least 10 times the local sound speed. The strong acceleration at minimum radius is demonstrated in individual line profiles; those formed deepest in the photosphere show a jump discontinuity of over 70 kms−1 on a time-scale of 150 s. The pulse speed and line profile jumps imply a shock is present at minimum radius. These empirical results provide input for hydrodynamical modelling of the pulsation and hydrodynamical plus radiative transfer modelling of the dynamical spectra

FUSE spectroscopy of sdOB primary of the post common-envelope binary LB 3459 (AA Dor)

LB 3459 (AA Dor) is an eclipsing, close, post common-envelope binary consisting of an sdOB primary star and an unseen secondary with an extraordinarly low mass - formally a brown dwarf. A recent NLTE spectral analysis shows a discrepancy with the surface gravity, which is derived from analyses of radial-velocity and lightcurves. We aim at precisely determing of the photospheric parameters of the primary, especially of the surface gravity, and searching for weak metal lines in the far UV. We performed a detailed spectral analysis of the far-UV spectrum of LB 3459 obtained with FUSE by means of state-of-the-art NLTE model-atmosphere techniques. A strong contamination of the far-UV spectrum of LB 3459 by interstellar line absorption hampers a precise determination of the photospheric properties of its primary star. Its effective temperature (42 kK) was confirmed by the evaluation of new ionization equilibria. For the first time, phosphorus and sulfur have been identified in the spectrum of LB 3459. Their photospheric abundances are solar and 0.01 times solar, respectively. From the C III 1174-1177A multiplet, we can measure the rotational velocity of 35 +/- 5 km/sec of the primary of LB 3459 and confirm that the rotation is bound. From a re-analysis of optical and UV spectra, we determine a higher log g = 5.3 (cgs) that reduces the discrepancy in mass determination in comparison to analyses of radial-velocity and lightcurves. However, the problem is not completely solved.Comment: 10 pages, 15 figure

Rural Homeownership and Labor Mobility in the U.S.

Labor and Human Capital,

Radial velocity variations of the pulsating subdwarf B star PG 1605+072

We present an analysis of high-speed spectroscopy of the pulsating subdwarf B star PG 1605+072. Periodic radial motions are detected at frequencies similar to those reported for photometric variations in the star, with amplitudes of up to 6 km/s. Differences between relative strengths for given frequency peaks for our velocity data and previously measured photometry are probably a result of shifting of power between modes over time. Small differences in the detected frequencies may also indicate mode-shifting. We report the detection of line-shape variations using the moments of the cross correlation function profiles. It may be possible to use the moments to identify the star's pulsation modes.Comment: 5 pages, 6 figure

An Investigation of Incipient Melting During Solution Heat Treatment of 7050 Aluminum Forgings and Its Effect on Corrosion Properties

7050 alloy (6.2Zn-2.3Mg-2.3Cu-0.12Zr) is a structural aluminum alloy commonly used in the aerospace industry. Its rich chemistry makes it susceptible to incipient melting. Incipient melting is a phenomenon where areas with high local alloy content melt before the rest of the material. This can cause a degradation of mechanical and corrosion properties. A six by four factor solution heat treatment trial was conducted. Six solution heat treatment temperatures, 890- 940°F in 10°F increments, and four times, 1, 2, 4, and 6 hours, were used. Incipient melting was observed in the 910°F, 6 hour solution heat treatment and all 920-940°F solution heat treatments. Solution heat treatment temperature was shown to be the more important factor. Little microstructural variance was seen among the different solution heat treatment times at a single temperature. Literature suggested that incipient melting would pit preferentially and increase susceptibility to intergranular attack. All 4 hour solution heat treatments were tested for pitting corrosion susceptibility by immersion of metallographic samples in a 0.1M NaCl solution. Samples with incipient melting present did not show preferential pitting. The same samples were tested for intergranular attack susceptibility according to AMS 2772 and ASTM G110. Samples with incipient melting showed no increase in sensitivity to intergranular attack. Neither of the corrosion properties tested degraded in the expected manner

The Transition to Adulthood and Independence: a Study of Young People Leaving Residential Care

The transition to adulthood is difficult for most young people. It is a time when young people make important decisions about their lives including their future education, career and living arrangements. Most young people have strong family and social networks to support them in these decisions. However, young people leaving residential care are often expected to make this transition abruptly and at a young age with no family or social networks to support them. The leaving and aftercare supports provided by the State are often not sufficient to provide for the needs of these young people leaving them at risk of homelessness, substance abuse, low levels of educational attainment and unemployment. In order to gain a better understanding of the experiences of care leavers this study explores the journey of twenty young people who had travelled into, through and from the residential care system. In doing so, the differences and similarities of the participant’s pre-care and in-care experiences were explored as well as the difficulties and challenges they faced throughout their journey, along with the experiences that shaped and informed their transition to adulthood and independence. The study identified three distinct transitions from residential care, those that had travelled a smooth transition, those that had experienced an unstable transition but whose circumstances improved over time and those whose transition was volatile or considerably more problematic and who are still mired in precarious social circumstances. The transitions highlight the diversity of the participants’ experiences in such a way that emphasize more clearly the supports that enable some participants to transition successfully and the barriers that lead others towards social exclusion. The findings indicate that the participants’ outcomes upon leaving residential care were ultimately dependent on the level of preparation given prior to leaving residential care, the level of the young person’s involvement in the leaving care process, the type of post-care housing/accommodation offered and the availability or absence of resources and supports post residential care. What is important about this research is the detailed and reflective accounts provided by young people, which give human resonance to the care leavers’ experiences