2009MNRAS.400L..80S

Query : 2009MNRAS.400L..80S

2009MNRAS.400L..80S - Mon. Not. R. Astron. Soc., 400, L80-L84 (2009/November-3)

The relation between Δν and νmax for solar-like oscillations.

STELLO D., CHAPLIN W.J., BASU S., ELSWORTH Y. and BEDDING T.R.

Abstract (from CDS):

Establishing relations between global stellar parameters and asteroseismic quantities can help improve our understanding of stellar astrophysics and facilitate the interpretation of observations. We present an observed relation between the large frequency separation, Δν, and the frequency of maximum power, νmax. We find that Δν ∝ ν0.77max, allowing prediction of Δν to about 15 per cent given νmax. Our result is further supported by established scaling relations for Δν and νmax and by extended stellar model calculations, which confirm that Δν can be estimated using this relation for basically any star showing solar-like oscillations in the investigated range (0.5 < M/M☉ < 4.0).

Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): stars: fundamental parameters - stars: interiors - stars: oscillations

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 631 0
2 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1354 1
3 * iot Hor PM* 02 42 33.4666679022 -50 48 01.055138166   5.97 5.40     F8V 446 1
4 HD 49933 PM* 06 50 49.8309774552 -00 32 27.167495244   6.147 5.771 7.04   F3V 407 2
5 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1925 0
6 HD 70514 * 08 18 18.8068680864 -65 36 47.491954416   6.210 5.056     K1III 30 0
7 * bet Vol PM* 08 25 44.1950662149 -66 08 12.796451416   4.896 3.759     K2III 96 0
8 * ksi Hya ** 11 33 00.1149306166 -31 51 27.447975478 5.17 4.47 3.54 2.84 2.36 G7IIIb 269 0
9 * bet Vir PM* 11 50 41.7185158616 +01 45 53.001539131 4.26 4.15 3.60 3.13 2.85 F9V 973 0
10 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 733 0
11 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 1092 2
12 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1352 1
13 * eps Oph PM* 16 18 19.2902245358 -04 41 33.047349888 4.95 4.21 3.23 2.54 2.05 G9.5IIIbFe-0.5 246 0
14 * kap Oph LP? 16 57 40.0975028128 +09 22 30.104472450 5.52 4.36 3.20 2.36 1.82 K2III 314 0
15 * mu. Ara PM* 17 44 08.7031414872 -51 50 02.591603160   5.85 5.15     G3IV-V 578 2
16 * mu.01 Her ** 17 46 27.5472960785 +27 43 14.560978925 4.56 4.17 3.42 2.89 2.51 G5IV 719 0
17 * ksi Dra PM* 17 53 31.7295427958 +56 52 21.510944948 6.14 4.93 3.75 2.92 2.33 K2III 285 0
18 * eta Ser PM* 18 21 18.6004923875 -02 53 55.780691633 4.84 4.19 3.25 2.55 2.05 K0III-IV 390 0
19 HD 175726 PM* 18 56 37.1723923656 +04 15 54.462836664   7.28 6.71     G0V 124 0
20 HD 181420 PM* 19 20 27.0720449304 -01 18 35.132869692   6.98 6.55     F6V 95 0
21 HD 181906 PM* 19 22 21.3624224688 +00 22 58.628902908   8.11 7.65     F5V 67 0
22 * gam Pav PM* 21 26 26.6049826473 -65 21 58.313057521 4.57 4.70 4.22 3.75 3.45 F9VFe-1.4CH-0.7 439 0
23 * nu. Ind ** 22 24 36.8853892493 -72 15 19.488237466   5.94 5.29     G9VFe-3.1CH-1.5 290 0

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