The rate of cooling of the pulsating white dwarf star G117-B15A: a new asteroseismological inference of the axion mass

被引：77

作者：

Corsico, A. H. ^{[1
,2
]}

Althaus, L. G. ^{[1
,2
]}

Miller Bertolami, M. M. ^{[1
,2
]}

Romero, A. D. ^{[1
,2
]}

Garcia-Berro, E. ^{[3
,4
]}

Isern, J. ^{[4
,5
]}

Kepler, S. O. ^{[6
]}

机构：

[1] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina

[2] Consejo Nacl Invest Cient & Tecn CONICET, Buenos Aires, DF, Argentina

[3] Univ Politecn Cataluna, Dept Fis Aplicada, Castelldefels 08860, Spain

[4] IEEC, Inst Space Studies Catalonia, Barcelona 08034, Spain

[5] Fac Ciencies, CSIC, Inst Ciencies Espai, Bellaterra 08193, Spain

[6] Univ Fed Rio Grande do Sul, Dept Astron, BR-91501970 Porto Alegre, RS, Brazil

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 424卷 / 04期

关键词：

asteroseismology; elementary particles; stars: individual: ZZ Ceti stars; stars: interiors; stars: oscillations; white dwarfs; ZZ-CETI STARS; EVOLUTIONARY TIME-SCALE; INSTABILITY STRIP; CP INVARIANCE; KEPLER FIELD; DENSE STARS; MODELS; CONSTRAINTS; BREMSSTRAHLUNG; DISCOVERY;

D O I：

10.1111/j.1365-2966.2012.21401.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We employ a state-of-the-art asteroseismological model of G117-B15A, the archetype of the H-rich atmosphere (DA) white dwarf pulsators (also known as DAV or ZZ Ceti variables), and use the most recently measured value of the rate of period change for the dominant mode of this pulsating star to derive a new constraint on the mass of axion, the still conjectural non-baryonic particle considered as a candidate for dark matter of the Universe. Assuming that G117-B15A is truly represented by our asteroseismological model, and, in particular, that the period of the dominant mode is associated with a pulsation g mode trapped in the H envelope, we find strong indications of the existence of extra cooling in this star, compatible with emission of axions of mass macos2 beta=(17.4-2.7+2.3) meV.

引用

页码：2792 / 2799

页数：8

共 56 条

[1] NEW CHEMICAL PROFILES FOR THE ASTEROSEISMOLOGY OF ZZ CETI STARS [J].