Mode lifetimes of stellar oscillations - Implications for asteroseismology

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Volume 500 / No 2 (June III 2009)

A&A, 500 2 (2009) L21-L24

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Table 1:

Mode lifetimes and fundamental stellar parameters for 12 solar-like stars, sub-giants and giants.
Name	$M/M_{\odot}$	$L/L_{\odot}$	$T_{\rm eff}$	$\Delta \nu$	$\tau$
$\xi$ Hydrae	3.07^a	$61.1 \pm 6.2^a$	$5000 \pm 100$ K^a	$7.11 \pm 6.14$ $\mu$ Hz^a	2 days^b
$\nu$ Indi	0.847 $\pm$ 0.043^c	6.21 $\pm$ 0.23^c	5291 $\pm$ 34K^c	24.25 $\pm$ 0.25 $\mu$ Hz^c	$\rm 16.2_{-7.5}^{+44.6}$ days^d
$\alpha$ Cen A	1.105 $\pm$ 0.007^e	1.522 $\pm$ 0.03^e	5810 $\pm$ 50 K^e	106.2^f	$3.9 \pm 1.4$ days^g
$\alpha$ Cen B	0.934 $\pm$ 0.006^e	0.503 $\pm$ 0.02^e	5260 $\pm$ 50 K^e	161.38 $\pm$ 0.06 $\mu$ Hz^h	$\rm 3.3_{-0.9}^{+1.8}$ days^h
$\beta$ Hydri	1.07 $\pm$ 0.03ⁱ	3.51 $\pm$ 0.09ⁱ	5872 $\pm$ 44 Kⁱ	57.24 $\pm$ 0.16 $\mu$ Hz^j	$\rm 2.3_{-0.5}^{+0.6}$ days^j
HD 49 933	1.2^k	0.53 $\pm$ 0.01^k	6780 $\pm$ 130 K^k	85.9 $\pm$ 0.15 $\mu$ Hz^k	$\rm 2.3_{-0.3}^{+0.5}$ days^k
Procyon	1.48^l	6.9^l	6500 K^l	55.90 $\pm$ 0.08 $\mu$ Hz^l	$\rm 1.5_{-0.8}^{+1.9}$ days^m
$\tau$ Ceti	0.783 $\pm$ 0.012ⁿ	0.488 $\pm$ 0.01ⁿ	5264 K^o	169 $\pm$ 0.2 $\mu$ Hzⁿ	1.7 $\pm$ 0.5 daysⁿ
$\varepsilon$ Oph	2.4 $\pm$ 0.4^p	59^p	4887 $\pm$ 100 K^p	5.3 $\pm$ 0.1 $\mu$ Hz^q	$\rm 2.7_{-0.8}^{+0.6}$ days^q
Arcturus	0.8 $\pm$ 0.3^r	200 $\pm$ 10^r	4290 $\pm$ 30 K^r	0.8 $\mu$ Hz^r	24.1 days^r
$\beta$ Ursae Minoris	1.3 $\pm$ 0.3^s	475 $\pm$ 30^s	4040 $\pm$ 100 K^s	0.7 $\pm$ 0.1 $\mu$ Hz^s	18 $\pm$ 9 days^s
Sun	1	1	5780 K	134 $\mu$ Hz	3.2 $\pm$ 0.2 days^t

References: ^a Frandsen et al. (2002); ^b Stello et al. (2006); ^c Bedding et al. (2006); ^d Carrier et al. (2007); ^e Miglio & Montalbán (2005); ^f Bedding et al. (2004); ^g Fletcher et al. (2006); ^h Kjeldsen et al. (2005); ⁱ North et al. (2007); ^j Bedding et al. (2007); ^k Appourchaux et al. (2008); ^l Leccia et al. (2007); ^m Arentoft et al. (2008); ⁿ Teixeira et al. (2009); ^o Pijpers (2003); ^p de Ridder et al. (2006); ^q Barban et al. (2007); ^r Tarrant et al. (2007); ^s Tarrant et al. (2008); ^t Chaplin et al. (2005).

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