141 research outputs found
CCD Photometry of Standard Stars at Maidanak Astronomical Observatory in Uzbekstan: Transformations and Comparisons
Observation of standard stars is of crucial importance in stellar photometry.
We have studied the standard transformation relations of the UBVRI CCD
photometric system at the Maidanak Astronomical Observatory in Uzbekistan. All
observations were made with the AZT-22 1.5m telescope, SITe 2k CCD or Fairchild
486 CCD, and standard Bessell UBVRI filters from 2003 August to 2007 September.
We observed many standard stars around the celestial equator observed by SAAO
astronomers. The atmospheric extinction coefficients, photometric zero points,
and time variation of photometric zero points of each night were determined.
Secondary extinction coefficients and photometric zero points were very stable,
while primary extinction coefficients showed a distinct seasonal variation. We
also determined the transformation coefficients for each filter. For B, V, R,
and I filters, the transformation to the SAAO standard system could be achieved
with a straight line or a combination of two straight lines. However, in the
case of the U filter and Fairchild 486 CCD combination, a significant
non-linear correction term - related to the size of Balmer jump or the strength
of the Balmer lines - of up to 0.08 mags was required. We found that our data
matched well the SAAO photometry in V, B-V, V-I, and R-I. But in U-B, the
difference in zero point was about 3.6 mmag and the scatter was about 0.02 mag.
We attribute the relatively large scatter in U-B to the larger error in U of
the SAAO photometry. We confirm the mostly small differences between the SAAO
standard UBVRI system and the Landolt standard system. We also attempted to
interpret the seasonal variation of the atmospheric extinction coefficients in
the context of scattering sources in the earth's atmosphere.Comment: 14 pages, 13 figure
New Size Hierarchies for Two Way Automata
© 2018, Pleiades Publishing, Ltd. We introduce a new type of nonuniform two-way automaton that can use a different transition function for each tape square. We also enhance this model by allowing to shuffle the given input at the beginning of the computation. Then we present some hierarchy and incomparability results on the number of states for the types of deterministic, nondeterministic, and bounded-error probabilistic models. For this purpose, we provide some lower bounds for all three models based on the numbers of subfunctions and we define two witness functions
The Angstrom Project Alert System: real-time detection of extragalactic microlensing
The Angstrom Project is undertaking an optical survey of stellar microlensing
events across the bulge region of the Andromeda Galaxy (M31) using a
distributed network of two-meter class telescopes. The Angstrom Project Alert
System (APAS) has been developed to identify in real time candidate
microlensing and transient events using data from the Liverpool and Faulkes
North robotic telescopes. This is the first time that real-time microlensing
discovery has been attempted outside of the Milky Way and its satellite
galaxies. The APAS is designed to enable follow-up studies of M31 microlensing
systems, including searches for gas giant planets in M31. Here we describe the
APAS and we present a few example light curves obtained during its
commissioning phase which clearly demonstrate its real-time capability to
identify microlensing candidates as well as other transient sources.Comment: 4 pages, submitted to ApJ Letter
The Hot Inner Disk of FU Ori
We have constructed a detailed radiative transfer disk model which reproduces
the main features of the spectrum of the outbursting young stellar object FU
Orionis from ~ 4000 angstrom, to ~ 8 micron. Using an estimated visual
extinction Av~1.5, a steady disk model with a central star mass ~0.3 Msun and a
mass accretion rate ~ 2e-4 Msun/yr, we can reproduce the spectral energy
distribution of FU Ori quite well. With the mid-infrared spectrum obtained by
the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope, we
estimate that the outer radius of the hot, rapidly accreting inner disk is ~ 1
AU using disk models truncated at this outer radius. Inclusion of radiation
from a cooler irradiated outer disk might reduce the outer limit of the hot
inner disk to ~ 0.5 AU. In either case, the radius is inconsistent with a pure
thermal instability model for the outburst. Our radiative transfer model
implies that the central disk temperature Tc > 1000 K out to ~ 0.5 - 1 AU,
suggesting that the magnetorotational instability (MRI) can be supported out to
that distance. Assuming that the ~ 100 yr decay timescale in brightness of FU
Ori represents the viscous timescale of the hot inner disk, we estimate the
viscosity parameter (alpha) to be ~ 0.2 - 0.02 in the outburst state,
consistent with numerical simulations of MRI in disks. The radial extent of the
high mass accretion region is inconsistent with the model of Bell & Lin, but
may be consistent with theories incorporating both gravitational instability
and MRI.Comment: 32 pages, 10 figures, to appear in the Astrophysical Journa
Quantum Algorithm for Dynamic Programming Approach for DAGs. Applications for Zhegalkin Polynomial Evaluation and Some Problems on DAGs
In this paper, we present a quantum algorithm for dynamic programming
approach for problems on directed acyclic graphs (DAGs). The running time of
the algorithm is , and the running time of the
best known deterministic algorithm is , where is the number of
vertices, is the number of vertices with at least one outgoing edge;
is the number of edges. We show that we can solve problems that use OR,
AND, NAND, MAX and MIN functions as the main transition steps. The approach is
useful for a couple of problems. One of them is computing a Boolean formula
that is represented by Zhegalkin polynomial, a Boolean circuit with shared
input and non-constant depth evaluating. Another two are the single source
longest paths search for weighted DAGs and the diameter search problem for
unweighted DAGs.Comment: UCNC2019 Conference pape
Multi-wavelength observations of afterglow of GRB 080319B and the modeling constraints
We present observations of the afterglow of GRB 080319B at optical, mm and
radio frequencies from a few hours to 67 days after the burst. Present
observations along with other published multi-wavelength data have been used to
study the light-curves and spectral energy distributions of the burst
afterglow. The nature of this brightest cosmic explosion has been explored
based on the observed properties and it's comparison with the afterglow models.
Our results show that the observed features of the afterglow fits equally good
with the Inter Stellar Matter and the Stellar Wind density profiles of the
circum-burst medium. In case of both density profiles, location of the maximum
synchrotron frequency is below optical and the value of cooling break
frequency is below rays, s after the burst. Also, the
derived value of the Lorentz factor at the time of naked eye brightness is
with the corresponding blast wave size of cm. The
numerical fit to the multi-wavelength afterglow data constraints the values of
physical parameters and the emission mechanism of the burst.Comment: 8 Pages, 3 Figures, Accepted for publication to Astronomy and
Astrophysics on 02/04/200
Accretion dynamics in the classical T Tauri star V2129 Oph
We analyze the photometric and spectroscopic variability of the classical T
Tauri star V2129 Oph over several rotational cycles to test the dynamical
predictions of magnetospheric accretion models. The photometric variability and
the radial velocity variations in the photospheric lines can be explained by
rotational modulation due to cold spots, while the radial velocity variations
of the He I (5876 \AA) line and the veiling variability are due to hot spot
rotational modulation. The hot and cold spots are located at high latitudes and
about the same phase, but the hot spot is expected to sit at the chromospheric
level, while the cold spot is at the photospheric level. Using the
dipole+octupole magnetic-field configuration previously proposed in the
literature for the system, we compute 3D MHD magnetospheric simulations of the
star-disk system. We use the simulation's density, velocity and scaled
temperature structures as input to a radiative transfer code, from which we
calculate theoretical line profiles at all rotational phases. The theoretical
profiles tend to be narrower than the observed ones, but the qualitative
behavior and the observed rotational modulation of the H\alpha and H\beta
emission lines are well reproduced by the theoretical profiles. The
spectroscopic and photometric variability observed in V2129 Oph support the
general predictions of complex magnetospheric accretion models with
non-axisymmetric, multipolar fields.Comment: Accepted by Astronomy and Astrophysic
Reflected Light from Sand Grains in the Terrestrial Zone of a Protoplanetary Disk
We show that grains have grown to ~mm size (sand sized) or larger in the
terrestrial zone (within ~3 AU) of the protoplanetary disk surrounding the 3
Myr old binary star KH 15D. We also argue that the reflected light in the
system reaches us by back scattering off the far side of the same ring whose
near side causes the obscuration.Comment: 22 pages, 5 figures. To be published in Nature, March 13, 2008.
Contains a Supplemen
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