39 research outputs found
Evolution of the Symbiotic Nova PU Vul -- Outbursting White Dwarf, Nebulae, and Pulsating Red Giant Companion
We present a composite light-curve model of the symbiotic nova PU Vul (Nova
Vulpeculae 1979) that shows a long-lasted flat optical peak followed by a slow
decline. Our model light-curve consists of three components of emission, i.e.,
an outbursting white dwarf (WD), its M-giant companion, and nebulae. The WD
component dominates in the flat peak while the nebulae dominate after the
photospheric temperature of the WD rises to log T (K) >~ 4.5, suggesting its WD
origin. We analyze the 1980 and 1994 eclipses to be total eclipses of the WD
occulted by the pulsating M-giant companion with two sources of the nebular
emission; one is an unocculted nebula of the M-giant's cool-wind origin and the
other is a partially occulted nebula associated to the WD. We confirmed our
theoretical outburst model of PU Vul by new observational estimates, that
spanned 32 yr, of the temperature and radius. Also our eclipse analysis
confirmed that the WD photosphere decreased by two orders of magnitude between
the 1980 and 1994 eclipses. We obtain the reddening E(B-V) ~ 0.3 and distance
to PU Vul d ~ 4.7 kpc. We interpret the recent recovery of brightness in terms
of eclipse of the hot nebula surrounding the WD, suggesting that hydrogen
burning is still going on. To detect supersoft X-rays, we recommend X-ray
observations around June 2014 when absorption by neutral hydrogen is minimum.Comment: 16 pages including 8 figs, to appear in Ap
On the effect of emission lines on the UBVR photometry
We investigate the effect on the U, B, V, Rc and Rj magnitudes of the removal
of emission lines from a spectrum. We determined "Dm" corrections from the
ratio of fluxes with and without emission lines, transmitted from the object
through the photometric filter. An exact and a simplified approach for
operative use were applied. The effect was demonstrated for classical symbiotic
stars, symbiotic novae and the classical nova V1974 Cyg. It was found that
about 20-30, 30-40, 10 and 26/20 percents of the observed flux in the U, B, V
and Rc/Rj filter, respectively, is radiated in the emission lines of the
investigated classical symbiotic stars. The largest effect was found for
symbiotic novae (RR Tel and V1016 Cyg) and the classical nova V1974 Cyg at 210
days (in average of 74, 79, 56 and 66/60 percents). Examples for practical
application are suggested.Comment: 8 pages, 6 figures, 2 tables, New Astron. in pres
The Continuing Slow Decline of AG Pegasi
We analyze optical and ultraviolet observations of the symbiotic binary AG
Pegasi acquired during 1992-97. The bolometric luminosity of the hot component
declined by a factor of 2-3 from 1980-1985 to 1997. Since 1992, the effective
temperature of the hot component may have declined by 10%-20%, but this decline
is comparable to the measurement errors. Optical observations of H-beta and He
I emission show a clear illumination effect, where high energy photons from the
hot component ionize the outer atmosphere of the red giant. Simple illumination
models generally account for the magnitude of the optical and ultraviolet
emission line fluxes. High ionization emission lines - [Ne V], [Mg V], and [Fe
VII] - suggest mechanical heating in the outer portions of the photoionized red
giant wind. This emission probably originates in a low density region
30-300 AU from the central binary.Comment: 17 pages, 7 pages, 5 tables; to be published in the Astronomical
Journal, July 200
The remarkable properties of the symbiotic star AE Circinus
We present new optical spectroscopy and photometry, 2MASS infrared
observations and 24 years of combined AAVSO and AFOEV photometry of the
symbiotic star candidate \ae. The long-term light curve is characterized by
outbursts lasting several years and having a slow decline of mag/day. The whole range of variability of the star in the band is
about 4 magnitudes. The periodogram of the photometric data reveals strong
signals at 342 and 171 days. The presence of the emission feature at
6830 \AA at minimum and the detection of absorption lines of a
K5 type star confirm the symbiotic classification and suggest that AE Cir is a
new member of the small group of s-type yellow symbiotic stars. We estimate a
distance of 9.4 kpc. Our spectrum taken at the high state shows a much flatter
spectral energy distribution, the disappearance of the 6830 \AA
emission feature and the weakness of the He II 4686 emission relative to the
Balmer emission lines. Our observations indicate the presence of emission line
flickering in time scales of minutes in 2001. The peculiar character of \ae is
revealed in the visibility of the secondary star at the high and low state, the
light curve resembling a dwarf nova superoutburst and the relatively short low
states. The data are hard to reconciliate with standard models for symbiotic
star outbursts.Comment: accepted for publication in MNRAS, 7 figure
The historical light curve of the symbiotic star AG Draconis: intense, magnetically induced cyclic activity
We analyze an optical light curve of the symbiotic system AG Draconis
covering the last 120 years of its history. During the first 32 years the
system was in a quiescence state. Around the year 1922 the star's quiescence
luminosity brightened by 0.29 mag. The last 82 years of the light curve (LC)
are characterized by a series of outbursts of 1-2 magnitude in brightness and
about 100 days in duration. The outbursts are distributed along the time axis
in 6 clusters with a quasi-periodic cycle of some 5300 days. The time intervals
among the outbursts themselves are integral numbers of the period 373.5 days.
During quiescence states the LC oscillates with the binary period of the system
of 550 d. The LC contains also a weak periodic signal with a period of 350 d,
attributed to pulsations of the giant star. Another period of 1160 d is also
present in the light curve, being the sidereal rotation period of the giant
star. We suggest that the outbursts are events of intense mass transfer from
the giant onto the hot component. These are modulated by an interplay between a
solar-like magnetic dynamo cycle operating in the outer layers of the giant,
and a tidal deformation of these layers that circulates the surface of the
giant with the synodic diurnal period of 373.5 Earth days. AG Dra is the 5th
symbiotic system with a light curve that reflects such an intense magnetic and
magnetically modulated activity. (Abridged)Comment: 10 pages, 4 figures. Accepted for publication in MNRA
Structure of the hot object in the symbiotic prototype Z And during its 2000-03 active phase
Aims: To investigate structure of the hot object in the symbiotic prototype Z
And during its major 2000-03 active phase. Methods: Analysis of the far
ultraviolet, optical low- and high-resolution spectroscopy and UBVR photometry.
Reconstruction of the spectral energy distribution (SED) during the outburst.
The Raman scattering process. Results: At the initial stages of the outburst
the hot object was characterized by the two-temperature spectrum (a warm
stellar radiation and a strong nebular emission) with signatures of a
mass-outflow at moderate (100-200 km/s) and very high (1000-2000 km/s)
velocities. The corresponding structure of the hot object consists of an
optically thick, slowly-expanding disk-like material encompassing the accretor
at the orbital plane and a fast optically thin wind over the remainder of the
star. A striking similarity of [FeVII]6087 and Raman 6825 profiles at/after the
dilution of the disk suggested their origin within the interaction zone where
the winds from the binary components collide.Comment: 18 pages (printed format), 9 figures, 4 tables, 2 appendices;
accepted for publication in A&A (02/03/2006
Disentangling the composite continuum of symbiotic binaries I. S-type systems
We describe a method of disentangling the composite,0.12-5 microns continuum
of symbiotic binaries.The observed SED is determined by the IUE/HST archival
spectra and flux-points corresponding to the optical UBVRI and infrared JHKLM
photometric measurements. The modeled SED is given by superposition of fluxes
from the cool giant, hot stellar source and nebula including the effect of the
Rayleigh scattering process and considering influence of the iron curtain
absorptions.We applied this method to 21 S-type symbiotic stars during
quiescence, activity and eclipses.Comment: 37 pages in printed format, 27 figures, 4 tables, accepted for
publication in Astronomy and Astrophysic