Helioseismology

Helioseismology is the study of the structure and dynamics of the Sun through its oscillations. These are principally caused by sound waves that are continuously driven and damped by convection near the Sun's surface. It is similar to geoseismology, or asteroseismology, which are respectively the studies of the Earth or stars through their oscillations. While the Sun's oscillations were first detected in the early 1960s, it was only in the mid-1970s that it was realized that the oscillations propagated throughout the Sun and could allow scientists to study the Sun's deep interior. The term was coined by Douglas Gough in the 90s. The modern field is separated into global helioseismology, which studies the Sun's resonant modes directly,[1] and local helioseismology, which studies the propagation of the component waves near the Sun's surface.[2]

Helioseismology has contributed to a number of scientific breakthroughs. The most notable was to show that the anomaly in the predicted neutrino flux from the Sun could not be caused by flaws in stellar models and must instead be a problem of particle physics. The so-called solar neutrino problem was ultimately resolved by neutrino oscillations.[3][4][5] The experimental discovery of neutrino oscillations was recognized by the 2015 Nobel Prize for Physics.[6] Helioseismology also allowed accurate measurements of the quadrupole (and higher-order) moments of the Sun's gravitational potential,[7][8][9] which are consistent with General Relativity. The first helioseismic calculations of the Sun's internal rotation profile showed a rough separation into a rigidly-rotating core and differentially-rotating envelope. The boundary layer is now known as the tachocline[10] and is thought to be a key component for the solar dynamo.[11] Although it roughly coincides with the base of the solar convection zone — also inferred through helioseismology — it is conceptually distinct, being a boundary layer in which there is a meridional flow connected with the convection zone and driven by the interplay between baroclinicity and Maxwell stresses.[12]

Helioseismology benefits most from continuous monitoring of the Sun, which began first with uninterrupted observations from near the South Pole over the austral summer.[13][14] In addition, observations over multiple solar cycles have allowed helioseismologists to study changes in the Sun's structure over decades. These studies are made possible by global telescope networks like the Global Oscillations Network Group (GONG) and the Birmingham Solar Oscillations Network (BiSON), which have been operating for over several decades.

  1. ^ Gough, D.O.; Kosovichev, A.G.; Toomre, J.; et al. (1996), "The seismic structure of the Sun", Science, 272 (5266): 1296–1300, Bibcode:1996Sci...272.1296G, doi:10.1126/science.272.5266.1296, PMID 8662458, S2CID 15996636
  2. ^ Gizon, L.; Birch, A. C. (2005), "Local Helioseismology", Living Reviews in Solar Physics, 2 (1): 6, Bibcode:2005LRSP....2....6G, doi:10.12942/lrsp-2005-6
  3. ^ Fukuda, Y.; Super-Kamiokande Collaboration (1998), "Evidence for oscillation of atmospheric neutrinos", Phys. Rev. Lett., 81 (8): 1562–1567, arXiv:hep-ex/9807003, Bibcode:1998PhRvL..81.1562F, doi:10.1103/PhysRevLett.81.1562
  4. ^ Bahcall, J. N.; Concha, Gonzalez-Garcia M.; Pe, na-Garay C. (2001), "Global analysis of solar neutrino oscillations including SNO CC measurement", Journal of High Energy Physics, 2001 (8): 014, arXiv:hep-ph/0106258, Bibcode:2001JHEP...08..014B, doi:10.1088/1126-6708/2001/08/014, S2CID 6595480
  5. ^ Bahcall, J. N. (2001), "High-energy physics: Neutrinos reveal split personalities", Nature, 412 (6842): 29–31, Bibcode:2001Natur.412...29B, doi:10.1038/35083665, PMID 11452285, S2CID 205018839
  6. ^ Webb, Jonathan (6 October 2015). "Neutrino 'flip' wins physics Nobel Prize". BBC News.
  7. ^ Duvall, T.L. Jr; Dziembowski, W.A.; Goode, P.R.; Gough, D.O.; Harvey, J.W.; Leibacher, J.W. (1984), "The internal rotation of the Sun", Nature, 310 (5972): 22–25, Bibcode:1984Natur.310...22D, doi:10.1038/310022a0, S2CID 4310140
  8. ^ Pijpers, F.P. (1998), "Helioseismic determination of the solar gravitational quadrupole moment", Mon. Not. R. Astron. Soc., 297 (3): L76–L80, arXiv:astro-ph/9804258, Bibcode:1998MNRAS.297L..76P, doi:10.1046/j.1365-8711.1998.01801.x, S2CID 14179539
  9. ^ Antia, H.M.; Chitre, S.M.; Gough, D.O. (2008), "Temporal variations in the Sun's rotational kinetic energy", Astron. Astrophys., 477 (2): 657–663, arXiv:0711.0799, Bibcode:2008A&A...477..657A, doi:10.1051/0004-6361:20078209
  10. ^ Spiegel, E. A.; Zahn, J.-P. (1992), "The solar tachocline", Astronomy and Astrophysics, 265: 106, Bibcode:1992A&A...265..106S
  11. ^ Fan, Y. (2009), "Magnetic Fields in the Solar Convection Zone", Living Reviews in Solar Physics, 6 (1): 4, Bibcode:2009LRSP....6....4F, doi:10.12942/lrsp-2009-4
  12. ^ Gough, D.O.; McIntyre, M.E. (1998), "Inevitability of a magnetic field in the Sun's interior", Nature, 394 (6695): 755, Bibcode:1998Natur.394..755G, doi:10.1038/29472, S2CID 1365619
  13. ^ Grec, G.; Fossat, E.; Pomerantz, M. (1980), "Solar oscillations: full disk observations from the geographic South Pole", Nature, 288 (5791): 541–544, Bibcode:1980Natur.288..541G, doi:10.1038/288541a0, S2CID 4345313
  14. ^ Duvall, Jr. T. L.; Harvey, J. W. (1983), "Observations of solar oscillations of low and intermediate degree", Nature, 302 (5903): 24, Bibcode:1983Natur.302...24D, doi:10.1038/302024a0, S2CID 4274994