Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 449, Issue 2, Pages 2194-2204Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv382
Keywords
binaries: close; binaries: eclipsing; stars: low mass; white dwarfs
Categories
Funding
- FONDECYT [3140585, 1141269]
- Science and Technology Facilities Council (STFC)
- STFC [ST/L000733/1]
- European Research Council under the European Union [320964]
- Millennium Science Initiative, Chilean ministry of Economy: Nucleus [RC130007]
- Postdoctoral Science Foundation of China [2013M530470, 2014T70010]
- Research Fund for International Young Scientists by the National Natural Science Foundation of China [11350110496]
- Science and Technology Facilities Council [ST/M000095/1, ST/M001350/1, ST/M003035/1, ST/L000733/1] Funding Source: researchfish
- STFC [ST/M003035/1, ST/M000095/1, ST/M001350/1, ST/L000733/1, ST/M002012/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1413600] Funding Source: National Science Foundation
Ask authors/readers for more resources
We report on the search for neweclipsing white dwarf plusmain-sequence (WDMS) binaries in the light curves of the Catalina surveys. We use a colour-selected list of almost 2000 candidate WDMS systems from the Sloan Digital Sky Survey, specifically designed to identify WDMS systems with cool white dwarfs and/or early M-type main-sequence stars. We identify a total of 17 eclipsing systems, 14 of which are new discoveries. We also find three candidate eclipsing systems, two main-sequence eclipsing binaries and 22 non-eclipsing close binaries. Our newly discovered systems generally have optical fluxes dominated by the main-sequence components, which have earlier spectral types than the majority of previously discovered eclipsing systems. We find a large number of ellipsoidally variable binaries with similar periods, near 4 h, and spectral types M2-3, which are very close to Roche lobe filling. We also find that the fraction of eclipsing systems is lower than found in previous studies and likely reflects a lower close binary fraction among WDMS binaries with early M-type main-sequence stars due to their enhanced angular momentum loss compared to fully convective late M-type stars, hence causing them to become cataclysmic variables quicker and disappear from the WDMS sample. Our systems bring the total number of known detached, eclipsing WDMS binaries to 71.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available