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AM CVn Systems as Optical, X-Ray and GWR Sources

Published online by Cambridge University Press:  22 February 2018

L. Yungelson ,
G. Nelemans  and
S. F. Portegies Zwart
L. Yungelson
Affiliation:
Institute of Astronomy, RAS, Moscow, Russia
G. Nelemans
Affiliation:
Institute of Astronomy, U. Cambridge, UK
S. F. Portegies Zwart
Affiliation:
U. Amsterdam, the Netherlands

Abstract

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We discuss the model for the Galactic sample of the AM CVn systems with Porb, ≤ 1500 s that can be detected in the optical and/or X-ray bands and may be resolved by the gravitational waves detector LISA. At 3 ≲ P ≲ 10 min all detectable systems are X-ray sources. At P ≳ 10 min most systems are only detectable in the V-band. About 30% of the X-ray sources is also detectable in the V-band. About 10,000 AM CVn systems might be resolved by LISA: this is comparable to the number of detached double white dwarfs that can be resolved. Several hundreds of AM CVn LISA sources might be also detectable in the V- and/or X-ray bands.

Resumen

Resumen

Discutimos el modelo para la muestra Galáctica de sistemas AM CVn cоn Рorb ≤ 1500 s detectables en la banda óptica y/o en rayos-X y de resolverse por el detector de ondas gravitacionales LISA. En el caso de 3 ≲ P ≲ 10 min todos los sistemas que se detectan son fuentes de rayos-X. En el caso de la P ≳ 10 min mayoría de los sistemas se detectan sólo en la banda V. Alrededor de 10,000 sistemas AM CVn pueden ser resueltos por LISA; esto es comparable con el número de enanas blancas dobles separadas que puedcn ser resueltas. Es posible que varios cientos de fuentes AM CVn de LISA puedan ser también detectadas en las bandas V y/o de rayos-X.

Keywords

BinariesClose — Gravitational Waves — White Dwarfs
Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 117 - 119
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Evans, C. R., Iben, I. J., & Smarr, L. 1987, ApJ, 323, 129 Google Scholar
Hansen, B. M. S. 1999, ApJ, 520, 680 CrossRefGoogle Scholar
Hellings, R. W. 2003, Class.Quant.Grav., 20, 1019 Google Scholar
Hils, D. & Bender, P. L. 2000, ApJ, 537, 334 Google Scholar
Marsh, T. R. & Steeghs, D. 2002, MNRAS, 331, L7 Google Scholar
Nelemans, G., Portegies Zwart, S. F., Verbunt, F., & Yungelson, L. R. 2001, A&A, 368, 939 Google Scholar
Nelemans, G., Yungelson, L. R., & Portegies Zwart, S. F. 2001, A&A, 375, 890 Google Scholar
Nelemans, G. 2003, MNRAS, in pressGoogle Scholar
Paczyński, B. 1967, Acta Astron., 17, 287 Google Scholar
Portegies Zwart, S. F. & Verbunt, F. 1996, A&A, 309, 179 Google Scholar
Predehl, P. & Schmitt, J. H. M. M. 1995, A&A, 293, 889 Google Scholar
Pringle, J. E. 1977, MNRAS, 178, 195 Google Scholar
Sandage, A. 1972, ApJ, 178, 1 CrossRefGoogle Scholar
Solheim, J.-E. 2003, in NATO ASIB Proc. 105: White Dwarfs, 299 Google Scholar
Tsugawa, M. & Osaki, Y. 1997, PASJ, 49, 75 Google Scholar
Wade, R. A. 1984, MNRAS, 208, 381 Google Scholar