65 research outputs found
Stellar explosion in the weak field approximation of the Brans-Dicke theory
We treat a very crude model of an exploding star, in the weak field
approximation of the Brans-Dicke theory, in a scenario that resembles some
characteristics data of a Type Ia Supernova. The most noticeable feature, in
the electromagnetic component, is the relationship between the absolute
magnitude at maximum brightness of the star and the decline rate in one
magnitude from that maximum. This characteristic has become one of the most
accurate method to measure luminosity distances to objects at cosmological
distances. An interesting result is that the active mass associated with the
scalar field is totally radiated to infinity, representing a mass loss in the
ratio of the "tensor" component to the scalar component of 1 to ( is the Brans-Dicke parameter), in agreement with a general result
of Hawking. Then, this model shows explicitly, in a dynamical case, the
mechanism of radiation of scalar field, which is necessary to understand the
Hawking result.Comment: 11 pages, no figures. Published in Class. Quantum Gravity V22 (2005
Using Ultra Long Period Cepheids to Extend the Cosmic Distance Ladder to 100 Mpc and Beyond
We examine the properties of 17 long period (80-180 days) and very luminous
(median absolute magnitude of M_I= -7.93 and M_V= -7.03) Cepheids to see if
they can serve as an useful distance indicator. We find that these Ultra Long
Period (ULP) Cepheids have a relatively shallow Period-Luminosity (PL)
relation, so in fact they are more "standard candle"-like than classical
Cepheids. In the reddening-free Wesenheit index, the slope of the ULP PL
relation is ~10 times less steep than the standard PL relation for the SMC
Cepheids. The scatter of our sample about the W_I PL relation is 0.22 mag,
approaching that of classical Cepheids and Type Ia Supernovae. We expect this
scatter to decrease as bigger and more uniform samples of ULP Cepheids are
obtained. We also measure a non-zero period derivative for one ULP Cepheid (SMC
HV829) and use the result to probe evolutionary models and mass loss of massive
stars. ULP Cepheids main advantage over classical Cepheids is that they are
more luminous, and as such show great potential as stellar distance indicators
to galaxies up to 100 Mpc and beyond.Comment: Accepted for Publication in ApJ. 11 pages, 8 figure
A Cepheid is No More: Hubble's Variable 19 in M33
We report on the remarkable evolution in the light curve of a variable star
discovered by Hubble (1926) in M33 and classified by him as a Cepheid. Early in
the 20th century, the variable, designated as V19, exhibited a 54.7 day period,
an intensity-weighted mean B magnitude of 19.59+/-0.23 mag, and a B amplitude
of 1.1 mag. Its position in the P-L plane was consistent with the relation
derived by Hubble from a total of 35 variables. Modern observations by the
DIRECT project show a dramatic change in the properties of V19: its mean B
magnitude has risen to 19.08 +/- 0.05 mag and its B amplitude has decreased to
less than 0.1 mag. V19 does not appear to be a classical (Population I) Cepheid
variable at present, and its nature remains a mystery. It is not clear how
frequent such objects are nor how often they could be mistaken for classical
Cepheids.Comment: Accepted for publication in the Astrophysical Journal Letters.
Finding charts and photometry data can be downloaded from
http://cfa-www.harvard.edu/~kstanek/DIRECT
Direct imaging of a massive dust cloud around R Coronae Borealis
We present recent polarimetric images of the highly variable star R CrB using
ExPo and archival WFPC2 images from the HST. We observed R CrB during its
current dramatic minimum where it decreased more than 9 mag due to the
formation of an obscuring dust cloud. Since the dust cloud is only in the
line-of-sight, it mimics a coronograph allowing the imaging of the star's
circumstellar environment. Our polarimetric observations surprisingly show
another scattering dust cloud at approximately 1.3" or 2000 AU from the star.
We find that to obtain a decrease in the stellar light of 9 mag and with 30% of
the light being reemitted at infrared wavelengths (from R CrB's SED) the grains
in R CrB's circumstellar environment must have a very low albedo of
approximately 0.07%. We show that the properties of the dust clouds formed
around R CrB are best fitted using a combination of two distinct populations of
grains size. The first are the extremely small 5 nm grains, formed in the low
density continuous wind, and the second population of large grains (~0.14
{\mu}m) which are found in the ejected dust clouds. The observed scattering
cloud, not only contains such large grains, but is exceptionally massive
compared to the average cloud.Comment: 8 pages, 7 figures published in A&
The Stony Brook / SMARTS Atlas of mostly Southern Novae
We introduce the Stony Brook / SMARTS Atlas of (mostly) Southern Novae. This
atlas contains both spectra and photometry obtained since 2003. The data
archived in this atlas will facilitate systematic studies of the nova
phenomenon and correlative studies with other comprehensive data sets. It will
also enable detailed investigations of individual objects. In making the data
public we hope to engender more interest on the part of the community in the
physics of novae. The atlas is on-line at
\url{http://www.astro.sunysb.edu/fwalter/SMARTS/NovaAtlas/} .Comment: 11 figures; 5 table
Classical novae from the POINT-AGAPE microlensing survey of M31 -- I. The nova catalogue
The POINT-AGAPE survey is an optical search for gravitational microlensing
events towards the Andromeda Galaxy (M31). As well as microlensing, the survey
is sensitive to many different classes of variable stars and transients. Here
we describe the automated detection and selection pipeline used to identify M31
classical novae (CNe) and we present the resulting catalogue of 20 CN
candidates observed over three seasons. CNe are observed both in the bulge
region as well as over a wide area of the M31 disk. Nine of the CNe are caught
during the final rise phase and all are well sampled in at least two colours.
The excellent light-curve coverage has allowed us to detect and classify CNe
over a wide range of speed class, from very fast to very slow. Among the
light-curves is a moderately fast CN exhibiting entry into a deep transition
minimum, followed by its final decline. We have also observed in detail a very
slow CN which faded by only 0.01 mag day over a 150 day period. We
detect other interesting variable objects, including one of the longest period
and most luminous Mira variables. The CN catalogue constitutes a uniquely
well-sampled and objectively-selected data set with which to study the
statistical properties of classical novae in M31, such as the global nova rate,
the reliability of novae as standard-candle distance indicators and the
dependence of the nova population on stellar environment. The findings of this
statistical study will be reported in a follow-up paper.Comment: 21 pages, 13 figures, re-submitted for publication in MNRAS, typos
corrected, references updated, figures 5-9 made cleare
Kepler photometry of RRc stars: peculiar double-mode pulsations and period doubling
We present the analysis of four first overtone RR Lyrae stars observed with the Kepler space telescope, based on data obtained over nearly 2.5 yr. All four stars are found to be multiperiodic.
The strongest secondary mode with frequency f2 has an amplitude of a few mmag, 20–45 times lower than the main radial mode with frequency f1. The two oscillations have a period ratio of P2/P1 = 0.612–0.632 that cannot be reproduced by any two radial modes. Thus, the secondary mode is non-radial. Modes yielding similar period ratios have also recently been discovered in other variables of the RRc and RRd types. These objects form a homogenous group and constitute a new class of multimode RR Lyrae pulsators, analogous to a similar class of multimode classical Cepheids in the Magellanic Clouds. Because a secondary mode with P2/P1 ∼ 0.61 is found in almost every RRc and RRd star observed from space, this form of multiperiodicity must be common. In all four Kepler RRc stars studied, we find subharmonics of f2 at ∼1/2f2 and at ∼3/2f2. This is a signature of period doubling of the secondary oscillation, and is the first detection of period doubling in RRc stars. The amplitudes and phases of f2 and its subharmonics are variable on a time-scale of 10–200 d. The dominant radial mode also shows variations on the same time-scale, but with much smaller amplitude. In three Kepler RRc stars we detect additional periodicities, with amplitudes below 1 mmag, that must correspond to non-radial g-modes. Such modes never before have been observed in RR Lyrae variables
Ultraviolet Study of the Active Interacting Binary Star R Arae using Archival IUE Data
The eclipsing and strongly interacting binary star system R Arae (HD149730)
is in a very active and very short-lived stage of its evolution. R Ara consists
of a B9V primary and an unknown secondary. We have collected the International
Ultraviolet Explorer (IUE) archival data on R Ara, with most of the data being
studied for the first time. There are 117 high resolution IUE spectra taken in
1980, 1982, 1985, 1989, and 1991. We provide photometric and spectroscopic
evidence for mass transfer and propose a geometry for the accretion structure.
We use colour scale radial velocity plots to view the complicated behavior of
the blended absorption features and to distinguish the motions of hotter and
cooler regions within the system. We observed a primary eclipse of R Ara in
2008 and have verified that its period is increasing. A model of the system and
its evolutionary status is presented.Comment: 13 pages, 15 figures, accepted for publication in MNRA
New Baade-Wesselink distances and radii for four metal-rich Galactic Cepheids
We provided accurate estimates of distances, radii and iron abundances for
four metal-rich Cepheids, namely V340 Ara, UZ Sct, AV Sgr and VY Sgr. The main
aim of this investigation is to constrain their pulsation properties and their
location across the Galactic inner disk. We adopted new accurate NIR (J,H,K)
light curves and new radial velocity measurements for the target Cepheids to
determinate their distances and radii using the Baade-Wesselink technique. In
particular, we adopted the most recent calibration of the IR surface brightness
relation and of the projection factor. Moreover, we also provided accurate
measurements of the iron abundance of the target Cepheids. Current distance
estimates agree within one sigma with similar distances based either on
empirical or on theoretical NIR Period-Luminosity relations. However, the
uncertainties of the Baade-Wesselink distances are on average a factor of 3-4
smaller when compared with errors affecting other distance determinations. Mean
Baade-Wesselink radii also agree at one sigma level with Cepheid radii based
either on empirical or on theoretical Period-Radius relations. Iron abundances
are, within one sigma, similar to the iron contents provided by Andrievsky and
collaborators, thus confirming the super metal-rich nature of the target
Cepheids. We also found that the luminosity amplitudes of classical Cepheids,
at odds with RR Lyrae stars, do not show a clear correlation with the
metal-content. This circumstantial evidence appears to be the consequence of
the Hertzsprung progression together with the dependence of the topology of the
instability strip on metallicity, evolutionary effects and binaries.Comment: 9 pages, 7 figures, A&A accepte
Two Mathematically Equivalent Versions of Maxwell's Equations
This paper is a review of the canonical proper-time approach to relativistic
mechanics and classical electrodynamics. The purpose is to provide a physically
complete classical background for a new approach to relativistic quantum
theory. Here, we first show that there are two versions of Maxwell's equations.
The new version fixes the clock of the field source for all inertial observers.
However now, the (natural definition of the effective) speed of light is no
longer an invariant for all observers, but depends on the motion of the source.
This approach allows us to account for radiation reaction without the
Lorentz-Dirac equation, self-energy (divergence), advanced potentials or any
assumptions about the structure of the source. The theory provides a new
invariance group which, in general, is a nonlinear and nonlocal representation
of the Lorentz group. This approach also provides a natural (and unique)
definition of simultaneity for all observers. The corresponding particle theory
is independent of particle number, noninvariant under time reversal (arrow of
time), compatible with quantum mechanics and has a corresponding positive
definite canonical Hamiltonian associated with the clock of the source.
We also provide a brief review of our work on the foundational aspects of the
corresponding relativistic quantum theory. Here, we show that the standard
square-root and the Dirac equations are actually two distinct
spin- particle equations.Comment: Appeared: Foundations of Physic
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