243 research outputs found
Planets and Axisymmetric Mass Loss
Bipolar planetary nebulae (PNe), as well as extreme elliptical PNe are formed
through the influence of a stellar companion. But half of all PN progenitors
are not influenced by any stellar companion, and, as I show here, are expected
to rotate very slowly on reaching the upper asymptotic giant branch; hence they
expect to form spherical PNe, unless they are spun-up. But since most PNe are
not spherical, I argue that about 50 percents of AGB stars are spun-up by
planets, even planets having a mass as low as 0.01 times the mass of Jupiter,
so they form elliptical PNe. The rotation by itself will not deform the AGB
wind, but may trigger another process that will lead to axisymmetric mass loss,
e.g., weak magnetic activity, as in the cool magnetic spots model. This model
also explains the transition from spherical to axisymmetric mass loss on the
upper AGB. For such low mass planets to substantially spin-up the stellar
envelope, they should enter the envelope when the star reaches the upper AGB.
This "fine-tuning" can be avoided if there are several planets on average
around each star, as is the case in the solar system, so that one of them is
engulfed when the star reaches the upper AGB.Comment: 8 pages, 1 figure. To appear in the proceedings of the conference,
"Post-AGB Objects (proto-planetary nebulae) as a Phase of Stellar Evolution",
Torun, Poland, July 5-7, 2000, eds. R. Szczerba, R. Tylenda, and S.K. Gorn
UBVJHKLM photometry and modeling of R Coronae Borealis
We present the results of UBVJHKLM photometry of R CrB spanning the period
from 1976 to 2001. Studies of the optical light curve have shown no evidence of
any stable harmonics in the variations of the stellar emission. In the L band
we found semi-regular oscillations with the two main periods of ~3.3 yr and
11.9 yr and the full amplitude of ~0.8 mag and ~0.6 mag, respectively. The
colors of the warm dust shell (resolved by Ohnaka et al. 2001) are found to be
remarkably stable in contrast to its brightness. This indicates that the inner
radius is a constant, time-independent characteristic of the dust shell. The
observed behavior of the IR light curve is mainly caused by the variation of
the optical thickness of the dust shell within the interval \tau(V)= 0.2-0.4.
Anticorrelated changes of the optical brightness (in particular with P ~ 3.3
yr) have not been found. Their absence suggests that the stellar wind of R CrB
deviates from spherical symmetry. The light curves suggest that the stellar
wind is variable. The variability of the stellar wind and the creation of dust
clouds may be caused by some kind of activity on the stellar surface. With some
time lag, periods of increased mass-loss cause an increase in the dust
formation rate at the inner boundary of the extended dust shell and an increase
in its IR brightness. We have derived the following parameters of the dust
shell (at mean brightness) by radiative transfer modeling: inner dust shell
radius r_in ~ 110 R_*, temperature T_dust(r_in) ~ 860 K, dust density
\rho_dust(r_in) ~ 1.1x10^{-20} g cm^-3, optical depth \tau(V) ~ 0.32 at 0.55
micron, mean dust formation rate [dM/dt]_dust ~ 3.1x10^-9 M_sun / yr, mass-loss
rate [dM/dt]_gas ~ 2.1x10^-7 M_sun / yr, size of the amorphous carbon grains
<(~) 0.01 micron, and B-V ~ -0.28.Comment: 9 pages, 6 figures, accepted for publication in A&
The Formation of Cataclysmic Variables with Brown Dwarf Secondaries
The present-day formation of cataclysmic variables (CVs) with brown dwarf
(BD) secondaries (0.013 M_sun < M_sec < 0.075 M_sun) is investigated using a
population synthesis technique. Results from the latest, detailed models for
BDs have been incorporated into the population synthesis code. For our models,
we find that ZACVs with BD secondaries have orbital periods in the range 46 min
to 2.5 hrs. We also find that ZACVs with BD secondaries comprise 18% of the
total, present-day ZACV population. In addition, we find that 80% of ZACVs with
BD secondaries have orbital periods < 78 minutes. This implies that 15% of the
present-day ZACV population should have orbital periods shorter than the
observed orbital period minimum for CVs. We also investigate the dependence of
the present-day formation rate of CVs with BD secondaries on the assumed value
of the common envelope efficiency parameter, alpha_CE, for three different
assumed mass ratio distributions in ZAMS binaries. Surprisingly, we find that
the common envelope process must be extremely inefficient (alpha_CE < 0.1) in
order for CVs with BD secondaries not to be formed. Finally, we find that the
progenitor binaries of ZACVs with BD secondaries have ZAMS orbital separations
< 3 AU and ZAMS primary masses between ~1-10 M_sun, with ~75% of the primary
masses less than ~1.6 M_sun. Interestingly, these ranges in orbital separation
and primary mass place the majority of the progenitor binaries within the
so-called ``brown dwarf desert.''Comment: preprint 27 pages 4 figures; to appear in ApJ April 1, 200
Direct detection of a magnetic field in the photosphere of the single M giant EK Boo: How common is magnetic activity among M giants?
We study the fast rotating M5 giant EK Boo by means of spectropolarimetry to
obtain direct and simultaneous measurements of both the magnetic field and
activity indicators, in order to infer the origin of the activity in this
fairly evolved giant. We used the new spectropolarimeter NARVAL at the Bernard
Lyot Telescope (Observatoire du Pic du Midi, France) to obtain a series of
Stokes I and Stokes V profiles for EK Boo. Using the Least Square Deconvolution
technique we were able to detect the Zeeman signature of the magnetic field. We
measured its longitudinal component by means of the averaged Stokes V and
Stokes I profiles. The spectra also permitted us to monitor the CaII K&H
chromospheric emission lines, which are well known as indicators of stellar
magnetic activity. From ten observations obtained between April 2008 and March
2009, we deduce that EK Boo has a magnetic field, which varied in the range of
-0.1 to -8 G. We also determined the initial mass and evolutionary stage of EK
Boo, based on up-to-date stellar evolution tracks. The initial mass is in the
range of 2.0-3.6 M_sun, and EK Boo is either on the asymptotic giant branch
(AGB), at the onset of the thermal pulse phase, or at the tip of the first (or
red) giant branch (RGB). The fast rotation and activity of EK Boo might be
explained by angular momentum dredge-up from the interior, or by the merging of
a binary. In addition, we observed eight other M giants, which are known as
X-ray emitters, or to be rotating fast for their class. For one of these, beta
And, presumably also an AGB star, we have a marginal detection of magnetic
field, and a longitudinal component Bl of about 1G was measured. More
observations like this will answer the question whether EK Boo is a special
case, or whether magnetic activity is, rather, more common among M giants than
expected.Comment: Accepted for publication in Astronomy & Astrophysics, 10 pages, 8
figure
The circumstellar envelope of IRC+10216 from milli-arcsecond to arcmin scales
Aims.Analysis of the innermost regions of the carbon-rich star IRC+10216 and
of the outer layers of its circumstellar envelope have been performed in order
to constrain its mass-loss history. Methods: .We analyzed the high dynamic
range of near-infrared adaptive optics and the deep V-band images of the
circumstellar envelope of IRC+10216 using high angular resolution, collected
with the VLT/NACO and FORS1 instruments. Results: .From the near-infrared
observations, we present maps of the sub-arcsecond structures, or clumps, in
the innermost regions. The morphology of these clumps is found to strongly vary
from J- to L-band. Their relative motion appears to be more complex than
proposed in earlier works: they can be weakly accelerated, have a constant
velocity, or even be motionless with respect to one another. From V-band
imaging, we present a high spatial resolution map of the shell distribution in
the outer layers of IRC+10216. Shells are resolved well up to a distance of
about 90'' to the core of the nebula and most of them appear to be composed of
thinner elongated shells. Finally, by combining the NACO and FORS1 images, a
global view is present to show both the extended layers and the bipolar core of
the nebula together with the real size of the inner clumps. Conclusions: .This
study confirms the rather complex nature of the IRC+10216 circumstellar
environment. In particular, the coexistence at different spatial scales of
structures with very different morphologies (clumps, bipolarity, and almost
spherical external layers) is very puzzling. This confirms that the formation
of AGB winds is far more complex than usually assumed in current models.Comment: Published in Astronomy & Astrophysics, 2006, 455, 18
High resolution soft X-ray spectroscopy of the elliptical galaxy NGC 5044. Results from the reflection grating spectrometer on-board XMM-Newton
The results from an X-ray spectroscopic study of the giant elliptical galaxy
NGC5044 in the center of a galaxy group are presented. The line dominated soft
X-ray spectra (mainly Fe-L and O VIII Ly_a) from the diffuse gas are resolved
for the first time in this system with the Reflection Grating Spectrometers
on-board XMM-Newton and provide a strong constraint on the temperature
structure. The spectra integrated over 2' (\sim 20kpc) in full-width can be
described by a two temperature plasma model of 0.7keV and 1.1keV. Most of the
latter component is consistent with originating from off-center regions.
Compared to the isobaric cooling flow prediction, the observation shows a clear
cut-off below a temperature of 0.6 +-0.1keV. Furthermore, the Fe and O
abundances within the central 10--20kpc in radius are accurately measured to be
0.55+-0.05 and 0.25+-0.1 times the solar ratios, respectively. The observed
cut-off temperature of this galaxy and other central galaxies in galaxy groups
and clusters are compared with the scale of the galaxy and properties of the
surrounding intra-cluster medium. Based on this comparison, the origin of the
lack of predicted cool emission is discussed.Comment: Accepted for publication in Astronomy & Astrophysic
A collimated, ionized bipolar structure and a high density torus in the young planetary nebula IRAS 17347-3139
We present observations of continuum (lambda = 0.7, 1.3, 3.6 and 18 cm) and
OH maser (lambda = 18 cm) emission toward the young planetary nebula IRAS
17347-3139, which is one of the three planetary nebulae that are known to
harbor water maser emission. From the continuum observations we show that the
ionized shell of IRAS 17347-3139 consists of two main structures: one extended
(size ~1". 5) with bipolar morphology along PA=-30 degrees, elongated in the
same direction as the lobes observed in the near-infrared images, and a central
compact structure (size ~0". 25) elongated in the direction perpendicular to
the bipolar axis, coinciding with the equatorial dark lane observed in the
near-infrared images. Our image at 1.3 cm suggests the presence of dense walls
in the ionized bipolar lobes. We estimate for the central compact structure a
value of the electron density at least ~5 times higher than in the lobes. A
high resolution image of this structure at 0.7 cm shows two peaks separated by
about 0". 13 (corresponding to 100-780 AU, using a distance range of 0.8-6
kpc). This emission is interpreted as originating in an ionized equatorial
torus-like structure, from whose edges the water maser emission might be
arising. We have detected weak OH 1612 MHz maser emission at VLSR ~ -70 km/s
associated with IRAS 17347-3139. We derive a 3 sigma upper limit of < 35% for
the percentage of circularly polarized emission. Within our primary beam, we
detected additional OH 1612 MHz maser emission in the LSR velocity ranges -5 to
-24 and -90 to -123 km/s, associated with the sources 2MASS J17380406-3138387
and OH 356.65-0.15, respectively.Comment: 26 pages, 8 figures. Accepted for publication in Ap
Rotational velocities of the giants in symbiotic stars: III. Evidence of fast rotation in S-type symbiotics
We have measured the projected rotational velocities (vsini) in a number of
symbiotic stars and M giants using high resolution spectroscopic observations.
On the basis of our measurements and data from the literature, we compare the
rotation of mass-donors in symbiotics with vsini of field giants and find that:
(1) the K giants in S-type symbiotics rotate at vsini>4.5 km/s, which is 2-4
times faster than the field K giants;
(2) the M giants in S-type symbiotics rotate on average 1.5 times faster than
the field M giants. Statistical tests show that these differences are highly
significant: p-value < 0.001 in the spectral type bins K2III-K5III,
M0III-M6III, and M2III-M5III;
(3) our new observations of D'-type symbiotics also confirm that they are
fast rotators.
As a result of the rapid rotation, the cool giants in symbiotics should have
3-30 times larger mass loss rates. Our results suggest also that bipolar
ejections in symbiotics seem to happen in objects where the mass donors rotate
faster than the orbital period.
All spectra used in our series of papers can be obtained upon request from
the authors.Comment: MNRAS (accepted), 7 pages, 5 figure
Constraining the Absolute Orientation of Eta Carinae's Binary Orbit: A 3-D Dynamical Model for the Broad [Fe III] Emission
We present a three-dimensional (3-D) dynamical model for the broad [Fe III]
emission observed in Eta Carinae using the Hubble Space Telescope/Space
Telescope Imaging Spectrograph (HST/STIS). This model is based on full 3-D
Smoothed Particle Hydrodynamics (SPH) simulations of Eta Car's binary colliding
winds. Radiative transfer codes are used to generate synthetic spectro-images
of [Fe III] emission line structures at various observed orbital phases and
STIS slit position angles (PAs). Through a parameter study that varies the
orbital inclination i, the PA {\theta} that the orbital plane projection of the
line-of-sight makes with the apastron side of the semi-major axis, and the PA
on the sky of the orbital axis, we are able, for the first time, to tightly
constrain the absolute 3-D orientation of the binary orbit. To simultaneously
reproduce the blue-shifted emission arcs observed at orbital phase 0.976, STIS
slit PA = +38 degrees, and the temporal variations in emission seen at negative
slit PAs, the binary needs to have an i \approx 130 to 145 degrees, {\theta}
\approx -15 to +30 degrees, and an orbital axis projected on the sky at a PA
\approx 302 to 327 degrees east of north. This represents a system with an
orbital axis that is closely aligned with the inferred polar axis of the
Homunculus nebula, in 3-D. The companion star, Eta B, thus orbits clockwise on
the sky and is on the observer's side of the system at apastron. This
orientation has important implications for theories for the formation of the
Homunculus and helps lay the groundwork for orbital modeling to determine the
stellar masses.Comment: 23 pages, 12 color figures, plus 2 online-only appendices (available
in the /anc folder of the Source directory). Accepted for publication in
MNRA
V1309 Scorpii: merger of a contact binary
Stellar mergers are expected to take place in numerous circumstences in the
evolution of stellar systems. In particular, they are considered as a plausible
origin of stellar eruptions of the V838 Mon type. V1309 Sco is the most recent
eruption of this type in our Galaxy. The object was discovered in September
2008. Our aim is to investigate the nature of V1309 Sco. V1309 Sco has been
photometrically observed in course of the OGLE project since August 2001. We
analyse these observations in different ways. In particular, periodogram
analyses were done to investigate the nature of the observed short term
variability of the progenitor. We find out that the progenitor of V1309 Sco was
a contact binary with an orbital period of ~1.4 day. This period was decreasing
with time. Similarly the light curve of the binary was also evolving,
indicating that the system evolved toward its merger. The violent phase of the
merger, marked by the systematic brightenning of the object, started in March
2008, i.e. half a year before the outburst discovery. We also investigate the
observations of V1309 Sco during the outburst and the decline and show that
they can be fully accounted for within the merger hypothesis. For the first
time in the literature we show, from direct observations, that contact binaries
indeed end up by merging into a single object, as it was suggested in numerous
theoretical studies of these systems. Our study also shows that stellar mergers
indeed result in eruptions of the V838 Mon type.Comment: accepted to Astronomy & Astrophysic
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