Regular frequency patterns in the classical δ Scuti star HD 144277 observed by the MOST satellite

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Volume 533 (September 2011)

A&A, 533 (2011) A133

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Table 2

Results of a nonadiabatic study to match predicted mode instability with the observed frequencies.

Opacity	X	Z	Mass [M_⊙]	log T_eff	log L/L_⊙	Frequency range [d^-1]	Frequency [d^-1]
						with η > 0	of η_max

OPAL	0.76	0.0134	–	–	–	–	–
OPAL	0.74	0.0134	1.576	3.874	0.757	16.8–55.3	23.3
OPAL	0.72	0.0134	1.604	3.894	0.844	24.6–54.4	37.8
OPAL	0.70	0.0134	1.623	3.911	0.915	38.2–61.0	52.5
OPAL	0.68	0.0134	1.615	3.921	0.951	42.5–68.0	56.3
OPAL	0.65	0.0134	1.599	3.928	0.979	45.3–72.9	60.1
OPAL	0.74	0.0160	–	–	–	–	–
OPAL	0.74	0.0140	1.683	3.897	0.868	30.4–54.8	41.8
OPAL	0.74	0.0120	1.646	3.902	0.880	34.3–55.7	45.2
OPAL	0.74	0.0100	1.698	3.927	0.991	–	60.0
OPAL	0.74	0.0008	1.718	3.945	1.069	–	67.4
OPAL	0.70	0.0160	–	–	–	–	–
OPAL	0.70	0.0140	1.604	3.903	0.878	30.5–57.3	45.2
OPAL	0.70	0.0120	1.647	3.925	0.974	47.6–68.3	60.1
OPAL	0.70	0.0100	1.662	3.941	1.039	56.8–74.4	67.4
OPAL	0.70	0.0008	1.670	3.956	1.102	69.3–75.4	71.2
OP	0.74	0.0134	1.631	3.889	0.827	21.7–54.8	35.4
OP	0.74	0.010	1.741	3.936	1.034	–	63.8
OP	0.70	0.010	1.695	3.947	1.071	60.8–75.1	67.4
OP	0.70	0.011	1.694	3.941	1.045	56.3–73.4	67.4

				observed		59.9–71.1	67.6

Notes. All models fit the four frequency groups following hypothesis 2 and were obtained with the A09 element mixture adopting V_rot = 15.0 km s^-1.

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