The gravitational wave radiation of pulsating white dwarfs revisited: The case of BPM 37093 and PG 1159-035

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作者：
García-Berro, E. [1 ,2 ]
Lorén-Aguilar, P. [1 ,3 ]
Córsico, A.H. [4 ,5 ]
Althaus, L.G. [1 ,6 ]
Lobo, J.A. [2 ,3 ]
Isern, J. [2 ,3 ]
机构：
[1] Departament de Física Aplicada, Universitat Politècnica de Catalunya, Av. del Canal Olímpic, s/n, 08860, Castelldefels, Barcelona, Spain
[2] Institut d'Estudis Espacials de Catalunya, Ed. Nexus, c/Gran Capità 2, 08034, Barcelona, Spain
[3] Institut de Ciències de l'Espai, C.S.I.C., Facultat de Ciències, Torre C-5, 08193 Bellaterra, Spain
[4] Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (B1900FWA) La Plata, Argentina
[5] Instituto de Astrofísica La Plata, CONICET-UNLP, Argentina
[6] Carrera del Investigador Científico y Tecnológico, CONICET, Argentina
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Astronomy and Astrophysics | 1600年 / 446卷 / 01期
关键词：
We compute the emission of gravitational radiation from pulsating white dwarfs. This is done by using an up-to-date stellar evolutionary code coupled with a state-of-the-art pulsational code. The emission of gravitational waves is computed for a standard 0.6 Mo white dwarf with a liquid carbon-oxygen core and a hydrogen-rich envelope; for a massive DA white dwarf with a partially crystallized core for which various l = 2 modes have been observed (BPM 37093) and for PG 1159-035; the prototype of the GW Vir class of variable stars; for which several quadrupole modes have been observed as well. We find that these stars do not radiate sizeable amounts of gravitational waves through their observed pulsation g-modes; in line with previous studies. We also explore the possibility of detecting gravitational waves radiated by the f-mode and the p-modes. We find that in this case the gravitational wave signal is very large and; hence; the modes decay very rapidly. We also discuss the possible implications of our calculations for the detection of gravitational waves from pulsating white dwarfs within the framework of future space-borne interferometers like LISA. © ESO 2006;
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页码：259 / 266
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