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 - 2024
#notes
1 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 592 0
2 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1255 1
3 * iot Hor PM* 02 42 33.4666679022 -50 48 01.055138166   5.97 5.40     F8V 394 1
4 HD 49933 PM* 06 50 49.8309774552 -00 32 27.167495244   6.147 5.771 7.04   F3V 379 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 1864 0
6 HD 70514 * 08 18 18.8068680864 -65 36 47.491954416   6.210 5.056     K1III 24 0
7 * bet Vol PM* 08 25 44.1950662149 -66 08 12.796451416   4.896 3.759     K2III 89 0
8 * ksi Hya ** 11 33 00.1149306166 -31 51 27.447975478 5.17 4.47 3.54 2.84 2.36 G7IIIb 257 0
9 * bet Vir PM* 11 50 41.7185158616 +01 45 53.001539131 4.26 4.15 3.60 3.13 2.85 F9V 929 0
10 * eta Boo SB* 13 54 41.07892 +18 23 51.7946 3.440 3.250 2.680 2.24 1.95 G0IV 704 0
11 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 1024 2
12 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1280 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-0.5 235 0
14 * kap Oph LP? 16 57 40.0975028128 +09 22 30.104472450 5.52 4.36 3.20 2.36 1.82 K2III 305 0
15 * mu. Ara PM* 17 44 08.7031414872 -51 50 02.591603160   5.85 5.15     G3IV-V 531 2
16 * mu.01 Her ** 17 46 27.5472960785 +27 43 14.560978925 4.56 4.17 3.42 2.89 2.51 G5IV 691 0
17 * ksi Dra PM* 17 53 31.7295427958 +56 52 21.510944948 6.14 4.93 3.75 2.92 2.33 K2III 272 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 377 0
19 HD 175726 PM* 18 56 37.1723923656 +04 15 54.462836664   7.28 6.71     G0V 112 0
20 HD 181420 PM* 19 20 27.0720449304 -01 18 35.132869692   6.98 6.55     F6V 88 0
21 HD 181906 PM* 19 22 21.3624224688 +00 22 58.628902908   8.11 7.65     F5V 63 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-0.7 411 0
23 * nu. Ind ** 22 24 36.8853892493 -72 15 19.488237466   5.94 5.29     G9VFe-3.1CH-1.5 276 0

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