198 research outputs found
On the nature of V2282 Sgr
The star V2282 Sgr is positionally consistent with a strong Chandra X-ray and
a Spitzer/IRAC MIR source. We derived its long term -band light curve from
the photographic archives of the Asiago and Catania Observatories, covering the
years from 1965 to 1984. CCD photometry in Summer 2009 was re-analyzed.
Optical spectra were secured at Loiano Observatory in 2011 and 2012. J H K
photometry, obtained from several experiments in different epochs was compared
and the Spitzer images were re-analyzed.
V2282 Sgr was found to be irregular variable in all wavelengths.
Spectroscopically, it shows strong emission features (H Balmer lines, [NII]6584
AA and [OIII]5007/4959 AA) while the Na D doublet is very strong, indicating a
circumstellar envelope. A single thermal energy distribution cannot reproduce
the observed SED, while it can be explained as the sum of a G-type star plus a
variable circumstellar disc, which mimics a class 0/I object. Most likely,
V2282 Sgr is a 1-2 mass pre main sequence star with an accretion
disk.Comment: 13 pages, 7 figure, in press on Baltic Astronom
Wind and nebula of the M33 variable GR290 (WR/LBV)
Context: GR290 (M33/V532=Romano's Star) is a suspected post-LBV star located
in M33 galaxy that shows a rare Wolf-Rayet spectrum during its minimum light
phase. In spite of many studies, its atmospheric structure, its circumstellar
environment and its place in the general context of massive stars evolution is
poorly known. Aims: Detailed study of its wind and mass loss, and study of the
circumstellar environment associated to the star. Methods: Long-slit spectra of
GR290 were obtained during its present minimum luminosity phase with the GTC
together with contemporaneous BVRI photometry. The data were compared with
non-LTE model atmosphere synthetic spectra computed with CMFGEN and with CLOUDY
models for ionized interstellar medium regions. Results: The current
mag, is the faintest at which this source has ever been observed. The non-LTE
models indicate effective temperature =27-30 kK at radius
=27-21 Rsun and mass loss rate Msun
yr. The terminal wind speed =620 is faster
than ever before recorded while the current luminosity Lsun is the lowest ever deduced. It is overabundant in He and N and
underabundant in C and O. It is surrounded by an unresolved compact HII region
with dimensions 4 pc, from where H-Balmer, HeI lines and [OIII] and [NII]
are detected. In addition, we find emission from a more extended interstellar
medium (ISM) region which appears to be asymmetric, with a larger extent to the
East (16-40 pc) than to the West. Conclusions: In the present long lasting
visual minimum, GR290 is in a lower bolometric luminosity state with higher
mass loss rate. The nearby nebular emission seems to suggest that the star has
undergone significant mass loss over the past years and is nearing
the end stages of its evolution.Comment: submitted to A&A, 12 pages, 9 figures, 7 table
A New Fast Silicon Photomultiplier Photometer
The realization of low-cost instruments with high technical performance is a
goal which deserves some efforts in an epoch of fast technological
developments: indeed such instruments can be easily reproduced and therefore
allow to open new research programs in several Observatories. We realized a
fast optical photometer based on the SiPM technology, using commercially
available modules. Using low-cost components we have developed a custom
electronic chain to extract the signal produced by a commercial MPPC module
produced by Hamamatsu, in order to obtain sub millisecond sampling of the light
curve of astronomical sources, typically pulsars. In the early February 2011 we
observed the Crab Pulsar at the Cassini telescope with our prototype
photometer, deriving its period, power spectrum and shape of its light curve in
very good agreement with the results obtained in the past with other
instruments.Comment: Accepted for Publications of the Astronomical Society of Pacific
(PASP), 8 pages, 8 figure
Dust formation in the winds of AGBs: the contribution at low metallicities
We present new models for the evolution of stars with mass in the range 1Msun
< M < 7.5Msun, followed from the pre-main-sequence through the asymptotic giant
branch phase. The metallicity adopted is $Z=3*10^{-4} (which, with an
alpha-enhancement of +0.4, corresponds to [Fe/H]=-2). Dust formation is
described by following the growth of dust grains of various types as the wind
expands from the stellar surface.
Models with mass M>3Msun experience Hot Bottom Burning, thus maintaining the
surface C/O below unity. Unlike higher Z models, the scarcity of silicon
available in the envelope prevents the formation of silicates in meaningful
quantities, sufficient to trigger the acceleration of the wind via radiation
pressure on the dust grains formed. No silicate formation occurs below a
threshold metallicity of Z=10^{-3}.
Low--mass stars, with M< 2.5Msun become carbon stars, forming solid carbon
dust in their surroundings. The total dust mass formed depends on the uncertain
extent of the inwards penetration of the convective envelope during the Third
Dredge--Up episodes following the Thermal Pulses. Carbon grains have sizes 0.08
micron < a_C < 0.12 micron and the total amount of dust formed (increasing with
the mass of the star) is M_C=(2-6)*10^{-4}Msun.
Our results imply that AGB stars with Z=3*10^{-4} can only contribute to
carbon dust enrichment of the interstellar medium on relatively long
timescales, > 300 Myr, comparable to the evolutionary time of a 3Msun star. At
lower metallicities the scarcity of silicon available and the presence of Hot
Bottom Burning even in M< 2Msun, prevents the formation of silicate and carbon
grains. We extrapolate our conclusion to more metal--poor environments, and
deduce that at Z < 10^{-4} dust enrichment is mostly due to metal condensation
in supernova ejecta.Comment: 13 pages, 8 figures, accepted for publication on MNRA
SiFAP: A New Fast Astronomical Photometer
A fast photometer based on SiPM technology was developed and tested at the University of Rome "La Sapienza" and at the Bologna Observatory. In this paper we present the improvements applied to our instrument, concerning new cooled sensors, a new version of the electronics and an upgraded control timing software
V2282 Sgr Revisited
The nature of V2282 Sgr is examined on the basis of several multiband observations: a 20 years long I-band light curve of V2282 Sgr obtained from archive photographic plates of the Asiago and Catania Observatories; a CCD R-band light curve obtained at Cornero Observatory; JHK photometry from 2MASS and UKDISS; Spitzer IRAC and MIPS images; optical spectra from Loiano Observatory; X-ray flux from CHANDRA. The star has a K-type spectrum with strong emission lines and is irregularly variable at all wavebands. The overall evidences suggest that V2282 Sgr is a Pre Main Sequence star with an accretion disk
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