期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 405, 期 3, 页码 1770-1776出版社
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2010.16548.x
关键词
stars: AGB and post-AGB; binaries: close; stars: oscillations
资金
- US Department of Energy through the University of California, Lawrence Livermore National Laboratory [W-7405-Eng-48]
- National Science Foundation through the Center for Particle Astrophysics of the University of California [AST-8809616]
- Mount Stromlo and Siding Spring Observatory, part of the Australian National University
- National Aeronautics and Space Administration
- National Science Foundation
- STFC [ST/G002622/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G002622/1] Funding Source: researchfish
We have studied a sample of Large Magellanic Cloud red giant binaries that lie on sequence E in the period-luminosity plane. We show that their combined light and velocity curves unambiguously demonstrate that they are binaries showing ellipsoidal variability. By comparing the phased light and velocity curves of both sequence D and E variables, we show that the sequence D variation - the long secondary period - is not caused by ellipsoidal variability. We also demonstrate several further differences between stars on sequences D and E. These include differences in velocity amplitude, in the distribution of eccentricity and in the correlations of velocity amplitude with luminosity and period. We also show that the sequence E stars, unlike stars on sequence D, do not show any evidence of a mid-infrared excess that would indicate circumstellar dust.
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