scholarly journals MESA models of the evolutionary state of the interacting binary epsilon Aurigae

2018 ◽  
Vol 476 (4) ◽  
pp. 5026-5031 ◽  
Author(s):  
Justus L Gibson ◽  
Robert E Stencel
Keyword(s):  
Evolutionary State ◽  
Epsilon Aurigae

scholarly journals On the origin and evolutionary state of RZ Cassiopeiae, KO Aquilae, and S Equulei

2008 ◽  
Vol 486 (3) ◽  
pp. 919-921 ◽  
Author(s):  
N. Mennekens ◽  
J.-P. De Greve ◽  
W. Van Rensbergen ◽  
L. R. Yungelson
Keyword(s):  
Evolutionary State

Epsilon Aurigae

1985 ◽  
pp. 177-181
Author(s):  
Robert D. Chapman
Keyword(s):  
Epsilon Aurigae

scholarly journals Clumpiness: time-domain classification of red giant evolutionary states

2020 ◽  
Vol 497 (4) ◽  
pp. 4843-4856 ◽  
Author(s):  
James S Kuszlewicz ◽  
Saskia Hekker ◽  
Keaton J Bell
Keyword(s):  
Time Series ◽  
Time Series Data ◽  
Series Data ◽  
Red Giants ◽  
Distance Information ◽  
Evolutionary State ◽  
State Classification ◽  
Red Giant ◽  
Reliable Classification

ABSTRACT Long, high-quality time-series data provided by previous space missions such as CoRoT and Kepler have made it possible to derive the evolutionary state of red giant stars, i.e. whether the stars are hydrogen-shell burning around an inert helium core or helium-core burning, from their individual oscillation modes. We utilize data from the Kepler mission to develop a tool to classify the evolutionary state for the large number of stars being observed in the current era of K2, TESS, and for the future PLATO mission. These missions provide new challenges for evolutionary state classification given the large number of stars being observed and the shorter observing duration of the data. We propose a new method, Clumpiness, based upon a supervised classification scheme that uses ‘summary statistics’ of the time series, combined with distance information from the Gaia mission to predict the evolutionary state. Applying this to red giants in the APOKASC catalogue, we obtain a classification accuracy of $\sim 91{{\ \rm per\ cent}}$ for the full 4 yr of Kepler data, for those stars that are either only hydrogen-shell burning or also helium-core burning. We also applied the method to shorter Kepler data sets, mimicking CoRoT, K2, and TESS achieving an accuracy $\gt 91{{\ \rm per\ cent}}$ even for the 27 d time series. This work paves the way towards fast, reliable classification of vast amounts of relatively short-time-span data with a few, well-engineered features.

scholarly journals Algols as Limits on Binary Evolution Scenarios

1989 ◽  
Vol 107 ◽  
pp. 155-164
Author(s):  
M.S. Hjellming
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Initial Mass ◽  
Transfer Rates ◽  
Successful Transition ◽  
Evolutionary State ◽  
Mass Ratios ◽  
Binary Evolution ◽  
Do So

AbstractEvolutionary scenarios must account for Algol binaries surviving their first phase of mass transfer. The outcome of this phase is dependent upon the rapidity of the initial mass transfer, which can be estimated by calculating the radial reponse of potential progenitors to mass loss. Limits on the donor’s evolutionary state, and its companion mass, can be placed on systems which would transfer mass on a thermal or dynamical timescale. Slower mass transfer rates are necessary for the successful transition to an Algol. Considering 1.5 and 5.0 M⊙ models, the former succeed in case A and Br systems, while the latter can do so only in case A systems. To evolve into an Algol binary, all systems seem to require initial mass ratios near one.

scholarly journals Statistical Properties of Magnetic CP Stars

2003 ◽  
Vol 210 ◽  
pp. 209-220
Author(s):  
S. Bagnulo
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Main Sequence ◽  
Statistical Properties ◽  
Chemically Peculiar ◽  
Evolutionary State ◽  
Statistical Studies ◽  
Magnetic Strength

Magnetic fields of chemically peculiar (CP) stars of the upper main sequence are characterised by a geometry organised at a large scale, permeating the entire photosphere, and with a typical strength of the order of 0.1–30 kG. Here I review the results obtained from statistical studies of the structures of the magnetic fields of CP stars, which are aimed at finding how magnetic strength and morphology are correlated with other stellar characteristics and with the star's evolutionary state.

scholarly journals Photometry of the Recent Eclipse of Epsilon Aurigae

1986 ◽  
Vol 7 ◽  
pp. 142-149
Author(s):  
Robert E. Stencel
Keyword(s):  
Light Curves ◽  
Optical Polarization ◽  
Infrared Photometry ◽  
Ultraviolet Spectrophotometry ◽  
Long Period ◽  
Epsilon Aurigae

AbstractNew observations of the long period eclipsing system Epsilon Aurigae are discussed, including optical and infrared photometry, ultraviolet spectrophotometry and optical polarization. Trends are noted in the light curves and compared to previous eclipses. Comments regarding interpretation are also provided.

scholarly journals The Ursa Major Cluster Redefined as a ‘Supergroup’

2016 ◽  
Vol 33 ◽  
Author(s):  
K. Wolfinger ◽  
V. A. Kilborn ◽  
E. V. Ryan-Weber ◽  
B. S. Koribalski
Keyword(s):  
Real Data ◽  
Virgo Cluster ◽  
Sloan Digital Sky Survey ◽  
Galaxy Groups ◽  
The Third ◽  
Evolutionary State ◽  
Sky Survey ◽  
Major Cluster ◽  
The Galaxy ◽  
Major Region

AbstractWe identify gravitationally bound structures in the Ursa Major region using positions, velocities and photometry from the Sloan Digital Sky Survey (SDSS DR7) and the Third Reference Catalogue of Bright Galaxies (RC3). A friends-of-friends algorithm is extensively tested on mock galaxy lightcones and then implemented on the real data to determine galaxy groups whose members are likely to be physically and dynamically associated with one another. We find several galaxy groups within the region that are likely bound to one another and in the process of merging. We classify 6 galaxy groups as the Ursa Major ‘supergroup’, which are likely to merge and form a poor cluster with a mass of ~ 8 × 1013 M⊙. Furthermore, the Ursa Major supergroup as a whole is likely bound to the Virgo cluster, which will eventually form an even larger system in the context of hierarchical structure formation. We investigate the evolutionary state of the galaxy groups in the Ursa Major region and conclude that these groups are in an early evolutionary state and the properties of their member galaxies are similar to those in the field.

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