3,507 research outputs found
Orbital Solutions and Absolute Elements of the Eclipsing Binary MY Cygni
Differential UBV photoelectric photometry for the eclipsing binary MY Cyg is presented. The Wilson-Devinney program is used to simultaneously solve the three light curves together with previously published radial velocities. A comparison is made with the previous solution found with the Russell-Merrill method. We examine the long-term apsidal motion of this well-detached, slightly eccentric system. We determine absolute dimensions, discuss metallicity/Am-star issues, and estimate the evolutionary status of the stars
A refined analysis of the low-mass eclipsing binary system T-Cyg1-12664
The observational mass-radius relation of main sequence stars with masses
between ~0.3 and 1.0 Msun reveals deviations between the stellar radii
predicted by models and the observed radii of stars in detached binaries. We
generate an accurate physical model of the low-mass eclipsing binary
T-Cyg1-12664 in the Kepler mission field to measure the physical parameters of
its components and to compare them with the prediction of theoretical stellar
evolution models. We analyze the Kepler mission light curve of T-Cyg1-12664 to
accurately measure the times and phases of the primary and secondary eclipse.
In addition, we measure the rotational period of the primary component by
analyzing the out-of-eclipse oscillations that are due to spots. We accurately
constrain the effective temperature of the system using ground-based absolute
photometry in B, V, Rc, and Ic. We also obtain and analyze V, Rc, Ic
differential light curves to measure the eccentricity and the orbital
inclination of the system, and a precise Teff ratio. From the joint analysis of
new radial velocities and those in the literature we measure the individual
masses of the stars. Finally, we use the PHOEBE code to generate a physical
model of the system. T-Cyg1-12664 is a low eccentricity system, located
d=360+/-22 pc away from us, with an orbital period of P=4.1287955(4) days, and
an orbital inclination i=86.969+/-0.056 degrees. It is composed of two very
different stars with an active G6 primary with Teff1=5560+/-160 K,
M1=0.680+/-0.045 Msun, R1=0.799+/-0.017 Rsun, and a M3V secondary star with
Teff2=3460+/-210 K, M2=0.376+/-0.017 Msun, and R2=0.3475+/-0.0081 Rsun. The
primary star is an oversized and spotted active star, hotter than the stars in
its mass range. The secondary is a cool star near the mass boundary for fully
convective stars (M~0.35 Msun), whose parameters appear to be in agreement with
low-mass stellar model.Comment: 18 pages, 15 figures, 15 table
Morphological response of variable river discharge and wave forcing at a bar-built estuary
17 USC 105 interim-entered record; under review.The article of record as published may be found at https://doi.org/10.1016/j.ecss.2021.107438Observations of morphological evolution at Carmel River State Beach, Carmel, CA, USA, were made during two winter periods where the estuary underwent transitions from closed to open states episodically during each observation period. However, each winter was climatologically distinct: the first (Dec 2016–May 2017) was a high river discharge year (several events >200 m³ /s) with westerly offshore waves and the second (Dec 2017–May 2018) was a low river discharge year with northwesterly offshore waves. The morphological response of the beach was measured using Structure-from-Motion from both aircraft and unmanned aerial vehicles (UAVs) and shows two distinct seasonal trends. The first (in 2016–2017) indicates rapid (hours) and frequent (days-weeks) migration of the river breach channel across the span of the beach. The second (in 2017–2018) indicates no migration of the initial breach channel, despite multiple breach events. Analysis of the offshore wave energy using the Coastal Data Information Program (CDIP) hindcast model results indicate a stronger longshore wave radiation stress during the migratory breach year. In addition, discharge rates during this year were more than three times stronger than the non-migratory year, indicating a stronger offshore jet from the breach site. These observations support the hypothesis that migration requires both a strong river discharge and a longshore wave radiation stress component.Naval Postgraduate School Naval Research ProgramOffice of Naval Research-CRUSER Progra
The Fate of Binaries in the Galactic Center: The Mundane and the Exotic
The Galactic Center (GC) is dominated by the gravity of a super-massive black
hole (SMBH), Sagittarius A, and is suspected to contain a sizable
population of binary stars. Such binaries form hierarchical triples with the
SMBH, undergoing Eccentric Kozai-Lidov (EKL) evolution, which can lead to high
eccentricity excitations for the binary companions' mutual orbit. This effect
can lead to stellar collisions or Roche-lobe crossings, as well as orbital
shrinking due to tidal dissipation. In this work we investigate the dynamical
and stellar evolution of such binary systems, especially with regards to the
binaries' post-main-sequence evolution. We find that the majority of binaries
(~75%) is eventually separated into single stars, while the remaining binaries
(~25%) undergo phases of common-envelope evolution and/or stellar mergers.
These objects can produce a number of different exotic outcomes, including
rejuvenated stars, G2-like infrared-excess objects, stripped giant stars, Type
Ia supernovae (SNe), cataclysmic variables (CVs), symbiotic binaries (SBs), or
compact object binaries. We estimate that, within a sphere of 250 Mpc radius,
about 7.5 to 15 Type Ia SNe per year should occur in galactic nuclei due to
this mechanism, potentially detectable by ZTF and ASAS-SN. Likewise we estimate
that, within a sphere of 1 Gpc volume, about 10 to 20 compact object
binaries form per year that could become gravitational wave sources. Based on
results of EKL-driven compact object binary mergers in galactic nuclei by Hoang
at al. (2018), this compact object binary formation rate translates to about 15
to 30 events per year detectable by Advanced LIGO.Comment: 8 pages, 3 figures, accepted by Ap
Classifying the unknown: discovering novel gravitational-wave detector glitches using similarity learning
The observation of gravitational waves from compact binary coalescences by
LIGO and Virgo has begun a new era in astronomy. A critical challenge in making
detections is determining whether loud transient features in the data are
caused by gravitational waves or by instrumental or environmental sources. The
citizen-science project \emph{Gravity Spy} has been demonstrated as an
efficient infrastructure for classifying known types of noise transients
(glitches) through a combination of data analysis performed by both citizen
volunteers and machine learning. We present the next iteration of this project,
using similarity indices to empower citizen scientists to create large data
sets of unknown transients, which can then be used to facilitate supervised
machine-learning characterization. This new evolution aims to alleviate a
persistent challenge that plagues both citizen-science and instrumental
detector work: the ability to build large samples of relatively rare events.
Using two families of transient noise that appeared unexpectedly during LIGO's
second observing run (O2), we demonstrate the impact that the similarity
indices could have had on finding these new glitch types in the Gravity Spy
program
False positive probabilties for all Kepler Objects of Interest: 1284 newly validated planets and 428 likely false positives
We present astrophysical false positive probability calculations for every
Kepler Object of Interest (KOI)---the first large-scale demonstration of a
fully automated transiting planet validation procedure. Out of 7056 KOIs, we
determine that 1935 have probabilities <1% to be astrophysical false positives,
and thus may be considered validated planets. 1284 of these have not yet been
validated or confirmed by other methods. In addition, we identify 428 KOIs
likely to be false positives that have not yet been identified as such, though
some of these may be a result of unidentified transit timing variations. A side
product of these calculations is full stellar property posterior samplings for
every host star, modeled as single, binary, and triple systems. These
calculations use 'vespa', a publicly available Python package able to be easily
applied to any transiting exoplanet candidate.Comment: 20 pages, 8 figures. Published in ApJ. Instructions to reproduce
results can be found at https://github.com/timothydmorton/koi-fp
Determination of Uncertainties for Analytically Derived Material Properties to Be Used in Monte Carlo Based Orion Heatshield Sizing
Ablative materials are often used for spacecraft heatshields to protect underlying structures from the extreme environments associated with atmospheric reentry. NASA's Orion EM-1 capsule has been designed to use a molded Avcoat material system. In order to determine the required heatshield thickness, a Monte Carlo approach to the sizing process was proposed. To perform the Monte Carlo simulation, statistical uncertainties on all material property input parameters were required. Obtaining these values for measured properties is straightforward, however input parameters that are derived analytically have historically used uncertainties based on engineering judgment. A MATLAB program was created to use laboratory generated thermogravimetric analysis (TGA) data to calculate uncertainties on the Arrhenius parameters for molded Avcoat. Uncertainties associated with the normalized ablation rate and pyrolysis gas enthalpy were also generated using a wrapper script and the ACE code. These uncertainties could then be tied directly to measured values of individual elemental constituents. The resulting uncertainty values will allow for a probabilistic sizing approach on molded Avcoat with a higher level of confidence in the input parameters
KIC 4247791: A SB4 system with two eclipsing binaries (2EBs)
KIC 4247791 is an eclipsing binary observed by the Kepler satellite mission.
We wish to determine the nature of its components and in particular the origin
of a shallow dip in its Kepler light curve that previous investigations have
been unable to explain in a unique way. We analyze newly obtained
high-resolution spectra of the star using synthetic spectra based on atmosphere
models, derive the radial velocities of the stellar components from
cross-correlation with a synthetic template, and calculate the orbital
solution. We use the JKTEBOP program to model the Kepler light curve of KIC
4247791. We find KIC 4247791 to be a SB4 star. The radial velocity variations
of its four components can be explained by two separate eclipsing binaries. In
contradiction to previous photometric findings, we show that the observed
composite spectrum as well as the derived masses of all four of its components
correspond to spectral type F. The observed small dip in the light curve is not
caused by a transit-like phenomenon but by the eclipses of the second binary
system. We find evidence that KIC 4247791 might belong to the very rare
hierarchical SB4 systems with two eclipsing binaries.Comment: 6 pages, 8 figures, 2 table
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