321 research outputs found
Weinberg propagator of a free massive particle with an arbitrary spin from the BFV-BRST path integral
The transition amplitude is obtained for a free massive particle of arbitrary
spin by calculating the path integral in the index-spinor formulation within
the BFV-BRST approach. None renormalizations of the path integral measure were
applied. The calculation has given the Weinberg propagator written in the
index-free form with the use of index spinor. The choice of boundary conditions
on the index spinor determines holomorphic or antiholomorphic representation
for the canonical description of particle/antiparticle spin.Comment: 31 pages, Latex, version published in Class. Quantum Gra
An asteroseismic study of the beta Cephei star 12 Lacertae: multisite spectroscopic observations, mode identification and seismic modelling
We present the results of a spectroscopic multisite campaign for the beta
Cephei star 12 (DD) Lacertae. Our study is based on more than thousand
high-resolution high S/N spectra gathered with 8 different telescopes in a time
span of 11 months. In addition we make use of numerous archival spectroscopic
measurements. We confirm 10 independent frequencies recently discovered from
photometry, as well as harmonics and combination frequencies. In particular,
the SPB-like g-mode with frequency 0.3428 1/d reported before is detected in
our spectroscopy. We identify the four main modes as (l1,m1) = (1, 1), (l2,m2)
= (0, 0), (l3,m3) = (1, 0) and (l4,m4) = (2, 1) for f1 = 5.178964 1/d, f2 =
5.334224 1/d, f3 = 5.066316 1/d and f4 = 5.490133 1/d, respectively. Our
seismic modelling shows that f2 is likely the radial first overtone and that
the core overshooting parameter alpha_ov is lower than 0.4 local pressure scale
heights.Comment: 16 pages, 11 figures, accepted in MNRA
Some Aspects of Cost/ Benefit Analysis for In-Service Inspection of PWR Steam Generators
This report discusses a number of aspects of cost/benefit (C/B) analysis for in-service inspection (lSI} of pressurized water reactor (PWR) steam generators (SGs) and identifies several problem areas that must be addressed prior to a full C/B analysis capability. Following a brief review of the impact of SG problems on the productivity of PWR units and of the scope and variability of SG problems among U.S. PWRs, various occupational implications of SG lSI are considered, namely manpower, time, and rad exposure. The opportunities provided by refueling outages in respect to lSI frequency and work time windows are reviewed. Indices for characterizing the nondestructive testing {NDT) information, rad exposure, impact of unscheduled outages attributable to SG problems with the cost is virtually negligible for well-planned ISis. Considering the ALARA constraint on occupational rad exposure, the skilled manpower pool for NDT work appears to be the principal factor limiting lSI scope and frequency. Analysis of the manpower and time requirements for inspection of a 40-unit PWR population indicates, however, that an lSI strategy embodying two campaigns per year and a total population inspection within a 2-year interval is not far beyond current capabilities
Detection of gravity modes in the massive binary V380 Cyg from Kepler spacebased photometry and high-resolution spectroscopy
We report the discovery of low-amplitude gravity-mode oscillations in the
massive binary star V380 Cyg, from 180 d of Kepler custom-aperture space
photometry and 5 months of high-resolution high signal-to-noise spectroscopy.
The new data are of unprecedented quality and allowed to improve the orbital
and fundamental parameters for this binary. The orbital solution was subtracted
from the photometric data and led to the detection of periodic intrinsic
variability with frequencies of which some are multiples of the orbital
frequency and others are not. Spectral disentangling allowed the detection of
line-profile variability in the primary. With our discovery of intrinsic
variability interpreted as gravity mode oscillations, V380 Cyg becomes an
important laboratory for future seismic tuning of the near-core physics in
massive B-type stars.Comment: 5 pages, 4 figures, 2 tables. Accepted for publication in MNRAS
Letter
Towards ensemble asteroseismology of the young open clusters Chi Persei and NGC 6910
As a result of the variability survey in Chi Persei and NGC6910, the number
of Beta Cep stars that are members of these two open clusters is increased to
twenty stars, nine in NGC6910 and eleven in Chi Persei. We compare pulsational
properties, in particular the frequency spectra, of Beta Cep stars in both
clusters and explain the differences in terms of the global parameters of the
clusters. We also indicate that the more complicated pattern of the variability
among B type stars in Chi Persei is very likely caused by higher rotational
velocities of stars in this cluster. We conclude that the sample of pulsating
stars in the two open clusters constitutes a very good starting point for the
ensemble asteroseismology of Beta Cep-type stars and maybe also for other
B-type pulsators.Comment: 4 pages, Astronomische Nachrichten, HELAS IV Conference, Arecife,
Lanzarote, Feb 2010, submitte
First evidence of pulsations in Vega? Results of today's most extensive spectroscopic search
The impact of rapid rotation on stellar evolution theory remains poorly
understood as of today. Vega is a special object in this context as
spectroscopic and interferometric studies have shown that it is a rapid rotator
seen nearly pole one, a rare orientation particularly interesting for seismic
studies. In this paper we present a first systematic search for pulsations in
Vega. The goal of the present work is to detect for the first time pulsations
in a rapidly rotating star seen nearly pole-on. Vega was monitored in
quasi-continuous high-resolution echelle spectroscopy. A total of 4478 spectra
were obtained within 3 individual runs in 2008, 2009 and 2010 at high
resolution. This data set should represent the most extensive high S/N, high
resolution quasi-continuous survey obtained on Vega as of today. Equivalent
photospheric absorption profiles were calculated for the stellar spectrum, but
also for the telluric lines acting as a radial velocity reference. Residual
velocities were analysed and periodic low amplitude variations, potentially
indicative of stellar pulsations, detected. All three data sets revealed the
presence of residual periodic variations: 5.32 and 9.19 c/d, (A approx 6 m/s)
in 2008, 12.71 and 13.25 c/d, (A approx 8 m/s) in 2009 and 5.42 and 10.82 c/d,
(A approx 3-4 m/s) in 2010. A Lomb-Scargle periodogram of each velocity bin of
the equivalent profile was performed for the 2010 run, not showing the presence
of any higher order nrp mode. It is too early to conclude that the variations
are due to stellar pulsations, and a confirmation of the detection with a
highly stable spectrograph is a necessary next step. If pulsations are
confirmed, their very small amplitudes show that the star would belong to a
category of very "quiet" pulsators
Usefulness of electroanatomical mapping during transseptal endocardial left ventricular lead implantation
AimFailure rate to implant left ventricular (LV) lead
transvenously is 4-8% in cardiac resynchronization therapy (CRT)
patients. Epicardial lead placement is an alternative method and
if not applicable case reports and small series showed the
feasibility of endocardial LV lead implantation.
Electroanatomical mapping might be a useful tool to guide this
procedure.Methods and resultsFour patients had undergone
endocardial LV lead implantation after unsuccessful transvenous
implantation or epicardial LV lead dysfunction using the
transseptal approach. Electroanatomical mapping was used to mark
the location of the transseptal puncture. This location point
guided the mapping catheter from the subclavian access and
facilitated positioning of the LV lead at the adjacent latest
activation area of the left ventricle detected by activation
mapping. Endocardial active fixation LV leads were successfully
implanted in all patients with stable electrical parameters
immediately after implantation and over a mean follow-up of 18.3
months (lead impedance 520 +/- 177 vs. 439 +/- 119 Omega and
pacing threshold 0.8 +/- 0.2 V, 0.5 ms vs. 0.6 +/- 0.1 V, 0.5
ms, respectively). Patients were maintained on anticoagulation
therapy with a target international normalized ratio of 3.5-4.5
and did not show any thromboembolic, haemorrhagic events, or
infection. Echocardiography showed significant improvement of LV
systolic function with marked improvement of the functional
status.ConclusionsElectroanatomical mapping is a useful
technical tool to guide endocardial LV lead implantation. It
helps to identify the location of the transseptal puncture and
the use of activation mapping might facilitate location of the
optimal lead positions during CRT
Multisite spectroscopic seismic study of the beta Cep star V2052 Oph: inhibition of mixing by its magnetic field
We used extensive ground-based multisite and archival spectroscopy to derive
observational constraints for a seismic modelling of the magnetic beta Cep star
V2052 Ophiuchi. The line-profile variability is dominated by a radial mode
(f_1=7.14846 d^{-1}) and by rotational modulation (P_rot=3.638833 d). Two
non-radial low-amplitude modes (f_2=7.75603 d^{-1} and f_3=6.82308 d^{-1}) are
also detected. The four periodicities that we found are the same as the ones
discovered from a companion multisite photometric campaign (Handler et al.
2012) and known in the literature. Using the photometric constraints on the
degrees l of the pulsation modes, we show that both f_2 and f_3 are prograde
modes with (l,m)=(4,2) or (4,3). These results allowed us to deduce ranges for
the mass (M \in [8.2,9.6] M_o) and central hydrogen abundance (X_c \in
[0.25,0.32]) of V2052 Oph, to identify the radial orders n_1=1, n_2=-3 and
n_3=-2, and to derive an equatorial rotation velocity v_eq \in [71,75] km
s^{-1}. The model parameters are in full agreement with the effective
temperature and surface gravity deduced from spectroscopy. Only models with no
or mild core overshooting (alpha_ov \in [0,0.15] local pressure scale heights)
can account for the observed properties. Such a low overshooting is opposite to
our previous modelling results for the non-magnetic beta Cep star theta Oph
having very similar parameters, except for a slower surface rotation rate. We
discuss whether this result can be explained by the presence of a magnetic
field in V2052 Oph that inhibits mixing in its interior.Comment: 12 pages, 6 figures and 5 tables; accepted for publication in MNRAS
on 2012 August 1
Close binary stars in the solar-age Galactic open cluster M67
We present multi-colour time-series CCD photometry of the solar-age galactic
open cluster M67 (NGC 2682). About 3600 frames spread over 28 nights were
obtained with the 1.5 m Russian-Turkish and 1.2 m Mercator telescopes.
High-precision observations of the close binary stars AH Cnc, EV Cnc, ES Cnc,
the Scuti type systems EX Cnc and EW Cnc, and some long-period
variables belonging to M67 are presented. Three full multi-colour light curves
of the overcontact binary AH Cnc were obtained during three observing seasons.
Likewise we gathered three light curves of EV Cnc, an EB-type binary, and two
light curves of ES Cnc, a blue straggler binary. Parts of the light change of
long-term variables S1024, S1040, S1045, S1063, S1242, and S1264 are obtained.
Period variation analysis of AH Cnc, EV Cnc, and ES Cnc were done using all
times of mid-eclipse available in the literature and those obtained in this
study. In addition, we analyzed multi-colour light curves of the close binaries
and also determined new frequencies for the Scuti systems. The
physical parameters of the close binary stars were determined with simultaneous
solutions of multi-colour light and radial velocity curves. Finally we
determined the distance of M67 as 857(33) pc via binary star parameters, which
is consistent with an independent method from earlier studies.Comment: 12 pages, 9 Figures, 13 Table
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