The Birmingham Solar Oscillations Network (BiSON) provides high-quality high-cadence observations from as far back in time as 1978. Here we present the frequencies for the Sun-as-a-star global modes of oscillation.
2014 - Low-frequency, low-degree solar p-mode properties.
The solar low-degree low-frequency modes of oscillation are of particular interest as their frequencies can be measured with very high precision and hence provide good constraints on seismic models. Here we detect and characterize these valuable measures of the solar interior from a 22 yr Birmingham Solar Oscillations Network data set. We report mode frequencies, line widths, heights, amplitudes, and rotational splitting, all with robust uncertainties. The new values of frequency, rotational splitting, amplitude, and line width we provide will help place new constraints on hydrostatic and rotational structure, plus diagnostics of near-surface convection. Further to this, by assuming simple power laws, we extrapolate mode properties to lower frequencies. We demonstrate that the low-l low-frequency p modes have a low signal-to-noise ratio and that this cannot be overcome simply by continued observation. It will be necessary to observe the Sun in novel ways to ‘beat’ the intrinsic granulation noise.
When making use of these data, please cite both 10.1007/s11207-015-0810-0 and 10.1093/mnras/stu080 in any publications. Suggested BibTeX entries are below.
@Article{s11207-015-0810-0,
author = "Hale, S. J. and Howe, R. and Chaplin, W. J. and Davies, G. R. and Elsworth, Y. P.",
title = "{{Performance of the Birmingham Solar-Oscillations Network (BiSON)}}",
journal = {\solphys},
year = {2016},
month = jan,
day = {1},
volume = {291},
number = {1},
pages = {1--28},
issn = {1573-093X},
doi = "10.1007/s11207-015-0810-0",
url = "https://doi.org/10.1007/s11207-015-0810-0"
}@article{10.1093/mnras/stu080,
author = {Davies, G. R. and Broomhall, A. M. and Chaplin, W. J. and Elsworth, Y. and Hale, S. J.},
title = "{Low-frequency, low-degree solar p-mode properties from 22 years of Birmingham Solar Oscillations Network data}",
journal = {Monthly Notices of the Royal Astronomical Society},
volume = {439},
number = {2},
pages = {2025-2032},
year = {2014},
month = {02},
issn = {0035-8711},
doi = {10.1093/mnras/stu080},
url = {https://doi.org/10.1093/mnras/stu080},
eprint = {http://oup.prod.sis.lan/mnras/article-pdf/439/2/2025/18472646/stu080.pdf},
}MD5: c89ac7efff269e4ab548803e08001980
n l Freq Error
6 0 972.615 0.002
7 0 1117.993 0.004
7 1 1185.604 0.003
8 0 1263.198 0.005
8 1 1329.635 0.003
8 2 1394.689 0.005
9 0 1407.472 0.006
9 1 1472.839 0.006
9 2 1535.853 0.005
10 0 1548.336 0.007
9 3 1591.536 0.014
10 1 1612.724 0.006
10 2 1674.538 0.008
11 0 1686.594 0.012
10 3 1729.088 0.022
11 1 1749.285 0.007
11 2 1810.308 0.009
12 0 1822.202 0.012
11 3 1865.280 0.016
12 1 1885.089 0.009
12 2 1945.824 0.013
13 0 1957.452 0.012 2009 - Definitive Sun-as-a-star p-mode frequencies.
We present a list of ‘best possible estimates’ of low-degree p-mode frequencies from 8640 days of observations made by the Birmingham Solar-Oscillations Network (BiSON). This is the longest stretch of helioseismic data ever used for this purpose, giving exquisite precision in the estimated frequencies. Every effort has been made in the analysis to ensure that the frequency estimates are also accurate. In addition to presenting the raw best-fitting frequencies from our ‘peak-bagging’ analysis, we also provide tables of corrected frequencies pertinent to the quiet-Sun and an intermediate level of solar activity.
When making use of these data, please cite both 10.1007/s11207-015-0810-0 and 10.1111/j.1745-3933.2009.00672.x in any publications. Suggested BibTeX entries are below.
@Article{s11207-015-0810-0,
author = "Hale, S. J. and Howe, R. and Chaplin, W. J. and Davies, G. R. and Elsworth, Y. P.",
title = "{{Performance of the Birmingham Solar-Oscillations Network (BiSON)}}",
journal = {\solphys},
year = {2016},
month = jan,
day = {1},
volume = {291},
number = {1},
pages = {1--28},
issn = {1573-093X},
doi = "10.1007/s11207-015-0810-0",
url = "https://doi.org/10.1007/s11207-015-0810-0"
}@article{10.1111/j.1745-3933.2009.00672.x,
author = {Broomhall, A.-M. and Chaplin, W. J. and Davies, G. R. and Elsworth, Y. and Fletcher, S. T. and Hale, S. J. and Miller, B. and New, R.},
title = "{Definitive Sun-as-a-star p-mode frequencies: 23 years of BiSON observations}",
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
volume = {396},
number = {1},
pages = {L100-L104},
year = {2009},
month = {06},
issn = {1745-3925},
doi = {10.1111/j.1745-3933.2009.00672.x},
url = {https://doi.org/10.1111/j.1745-3933.2009.00672.x},
eprint = {http://oup.prod.sis.lan/mnrasl/article-pdf/396/1/L100/3024124/396-1-L100.pdf},
}MD5: d329a8da84b66b4a3b2716eb2fe906f6
These are corrected frequencies pertinent to the quiet Sun.
n l Freq Error
6 0 972.613 0.002
7 1 1185.592 0.004
8 0 1263.162 0.012
8 1 1329.629 0.004
8 2 1394.680 0.011
9 0 1407.481 0.012
9 1 1472.835 0.007
9 2 1535.859 0.011
10 0 1548.333 0.007
10 1 1612.720 0.007
10 2 1674.534 0.008
10 3 1729.085 0.016
11 0 1686.597 0.011
11 1 1749.279 0.007
11 2 1810.304 0.009
11 3 1865.293 0.019
12 0 1822.196 0.011
12 1 1885.081 0.009
12 2 1945.797 0.013
12 3 2001.243 0.017
13 0 1957.421 0.012
13 1 2020.793 0.010
13 2 2082.102 0.015
13 3 2137.788 0.019
14 0 2093.518 0.013
14 1 2156.784 0.014
14 2 2217.656 0.018
14 3 2273.516 0.026
15 0 2228.749 0.014
15 1 2291.993 0.015
15 2 2352.222 0.017
15 3 2407.643 0.025
16 0 2362.788 0.016
16 1 2425.595 0.015
16 2 2485.873 0.019
16 3 2541.671 0.023
17 0 2496.180 0.017
17 1 2559.162 0.015
17 2 2619.668 0.018
17 3 2676.149 0.023
18 0 2629.668 0.015
18 1 2693.347 0.014
18 2 2754.439 0.017
18 3 2811.318 0.021
19 0 2764.142 0.015
19 1 2828.150 0.014
19 2 2889.578 0.018
19 3 2946.935 0.021
20 0 2899.022 0.013
20 1 2963.322 0.014
20 2 3024.689 0.018
20 3 3082.273 0.025
21 0 3033.754 0.014
21 1 3098.140 0.015
21 2 3159.821 0.020
21 3 3217.683 0.028
22 0 3168.618 0.017
22 1 3233.139 0.018
22 2 3295.063 0.025
22 3 3353.335 0.041
23 0 3303.520 0.021
23 1 3368.469 0.023
23 2 3430.748 0.034
23 3 3489.409 0.053
24 0 3438.992 0.030
24 1 3504.129 0.030
24 2 3566.949 0.044
24 3 3626.078 0.075
25 0 3574.893 0.048
25 1 3640.475 0.038
25 2 3703.044 0.067
25 3 3762.530 0.105
26 0 3710.717 0.088
26 1 3777.067 0.052
26 2 3839.717 0.144
27 0 3846.993 0.177
27 1 3913.570 0.068
27 2 3976.930 0.298
28 0 3984.214 0.323