363 research outputs found
Photometric Studies of a WZ Sge-Type Dwarf Nova Candidate, ASAS160048-4846.2
We report on our time-resolved CCD photometry during the 2005 June
superoutburst of a WZ Sge-type dwarf nova candidate, ASAS 160048-4846.2. The
ordinary superhumps underwent a complex evolution during the superoutburst. The
superhump amplitude experienced a regrowth, and had two peaks. The superhump
period decreased when the superhump amplitude reached to the first maximum,
successively gradually increased until the second maximum of the amplitude, and
finally decreased again. Investigating other SU UMa-type dwarf novae which show
an increase of the superhump period, we found the same trend of the superhump
evolution in superoutbursts of them. We speculate that the superhump regrowth
in the amplitude has a close relation to the increase of the superhump period,
and all of SU UMa-type dwarf novae with a superhump regrowth follow the same
evolution of the ordinary superhumps as that of ASAS 160048-4846.2.Comment: 7 pages, 4 figure
Inverse anisotropic diffusion from power density measurements in two dimensions
This paper concerns the reconstruction of an anisotropic diffusion tensor
from knowledge of internal functionals
of the form with for
solutions of the elliptic equation on a two
dimensional bounded domain with appropriate boundary conditions. We show that
for I=4 and appropriately chosen boundary conditions, may uniquely and
stably be reconstructed from such internal functionals, which appear in
coupled-physics inverse problems involving the ultrasound modulation of
electrical or optical coefficients. Explicit reconstruction procedures for the
diffusion tensor are presented and implemented numerically.Comment: 27 pages, 6 figure
Explosion of a massive, He-rich star at z=0.16
We present spectroscopic and photometric data of the peculiar SN 2001gh,
discovered by the 'Southern inTermediate Redshift ESO Supernova Search'
(STRESS) at a redshift z=0.16. SN 2001gh has relatively high luminosity at
maximum (M_B = -18.55 mag), while the light curve shows a broad peak. An
early-time spectrum shows an almost featureless, blue continuum with a few weak
and shallow P-Cygni lines that we attribute to HeI. HeI lines remain the only
spectral features visible in a subsequent spectrum, obtained one month later. A
remarkable property of SN 2001gh is the lack of significant spectral evolution
over the temporal window of nearly one month separating the two spectra. In
order to explain the properties of SN 2001gh, three powering mechanism are
explored, including radioactive decays of a moderately large amount of 56Ni,
magnetar spin-down, and interaction of SN ejecta with circumstellar medium. We
favour the latter scenario, with a SN Ib wrapped in a dense, circumstellar
shell. The fact that no models provide an excellent fit with observations,
confirms the troublesome interpretation of the nature of SN 2001gh. A rate
estimate for SN 2001gh-like event is also provided, confirming the intrinsic
rarity of these objects.Comment: 11 pages, 8 figures, 3 tables. Accepted by MNRA
Mission conjointe NMA/PRIFAS d´étude et de prospective dans Le Sudeste du Bresil, du 27 octobre au 10 novembre 1990.
bitstream/item/116959/1/1589.pd
The 2005 July Superoutburst of the Dwarf Nova 2QZ J021927.9-304545: the SU UMa Nature Confirmed
We report on time-resolved photometry of the 2005 July superoutburst of the
dwarf nova, 2QZ J021927.9-304545. The resultant light curves showed conspicuous
superhumps with a period of 0.081113(19) days, confirming the SU UMa nature of
the object. Although we missed the maximum phase of the outburst, the amplitude
of the superoutburst well exceeded 5 mag. This value is slightly larger than
that of typical SU UMa-type dwarf novae. The superhump period decreased as time
elapsed, as can be seen in most SU UMa-type dwarf novae. Based on the archive
of ASAS-3, the recurrence time of a superoutburst of the variable turned out to
be about 400 days. This value is typical of well known SU UMa stars. The
distance to this system was roughly estimated as 370(+20, -60) pc using an
empirical relation.Comment: 6 pages, 7 figures, accepted for publication in PAS
The Type IIn Supernova SN 2010bt: The Explosion of a Star in Outburst
Indexación: Scopus.It is well known that massive stars (M > 8 M ) evolve up to the collapse of the stellar core, resulting in most cases in a supernova (SN) explosion. Their heterogeneity is related mainly to different configurations of the progenitor star at the moment of the explosion and to their immediate environments. We present photometry and spectroscopy of SN 2010bt, which was classified as a Type IIn SN from a spectrum obtained soon after discovery and was observed extensively for about 2 months. After the seasonal interruption owing to its proximity to the Sun, the SN was below the detection threshold, indicative of a rapid luminosity decline. We can identify the likely progenitor with a very luminous star (log L/L ≈ 7) through comparison of Hubble Space Telescope images of the host galaxy prior to explosion with those of the SN obtained after maximum light. Such a luminosity is not expected for a quiescent star, but rather for a massive star in an active phase. This progenitor candidate was later confirmed via images taken in 2015 (∼5 yr post-discovery), in which no bright point source was detected at the SN position. Given these results and the SN behavior, we conclude that SN 2010bt was likely a Type IIn SN and that its progenitor was a massive star that experienced an outburst shortly before the final explosion, leading to a dense H-rich circumstellar environment around the SN progenitor. © 2018. The American Astronomical Society. All rights reserved.https://iopscience.iop.org/article/10.3847/1538-4357/aac51
Photometric Studies of New Southern SU UMa-type dwarf novae, FL Triangulum Australe and CTCV J0549-4921
We report time-resolved optical CCD photometry on newly discovered SU
UMa-type dwarf novae, FL TrA and CTCV J0549-4921. During the 2006 August
outburst, we detected superhumps with a period of 0.59897(11) days for FL TrA,
clarifying the SU UMa nature of the system. On the first night of our
observations on FL TrA, the object showed no superhumps. This implies that it
takes a few days for full development of superhumps. The superhump period
variation diagram of FL TrA was similar to that observed in some WZ Sge stars
and short period SU UMa-type stars. This indicates that the system is closely
related to WZ Sge stars and SU UMa stars having short orbital periods. For CTCV
J0549-4921, the candidates of the mean superhump period are 0.083249(10) days
and 0.084257(8) days, respectively. Due to a lack of the observations, we
cannot determine the true superhump period, but the latter period is favorable.
Using the ASAS-3 archive, it turned out that the system shows only four
outbursts over the past 6 years. The outburst amplitude of CTCV J0549-4921 was
relatively small, with about 4.5 mag. One possibility is that mass evaporation
may play a role during quiescence.Comment: 7 pages, 8 figures, published for PASJ vol.6
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