By Jørgen Christensen-Dalsgaard (auth.), Jørgen Christensen-Dalsgaard, Søren Frandsen (eds.)
Helio- and asteroseismology learn the internal of the sunlight and different stars, through observations of oscillations on their surfaces. The final 10 years within the research of the sun inside, to a has witnessed a really fast evolution element the place we will now think of investigating the actual kingdom of subject, or the main points of rotation and different large-scale movement, within the solar. The stellar reviews are in a few respects on the element of the sunlight reports 10 years in the past, yet seem poised to take off. therefore the time used to be deemed ripe for lAO Symposium No 123, to evaluate the current prestige of this paintings, and plan for its destiny improvement. except the seismic information, few observations can be found to supply information regarding stellar interiors. specified stories, by way of spectral research, could be made up of stellar floor houses, together with atmospheric temperature and chemical composition. even if, the stellar radiative spectrum is nearly completely mounted through the mass, luminosity, radius and floor rotation of the megastar, and comprises basically no different information regarding the internal. an immense try out of stellar evolution conception is equipped via observations of stel lar clusters, whose individuals can kind of be assumed to have a similar age and chemical composition. the site of such stars in a HR diagram, the place luminosity is plotted opposed to the powerful temperature, can approximately be understood when it comes to stellar evolution calculations.
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Additional info for Advances in Helio- and Asteroseismology: Proceedings of the 123th Symposium of the International Astronomical Union, Held in Aarhus, Denmark, July 7–11, 1986
31 HELIOSEISMIC OBSERVATIONS AT STANFORD, 1977-1986 Figure 1 shows each year's results four times, at phases ± n x 160 minutes. 024 minutes would result in sloping lines across the plot with phase shifts less than 80 minutes per year. 010 minute signal determined for both Stanford (1976-1980) and Crimean observations (1974-1984) (Kotov, 1985). The agreement in later years is not as strong as for the years through 1979. The data for 1980 and 1981 had very low amplitudes during the best weather, and 1982 and 1983 had increased noise due to spectrograph seeing.
_St ... , .. 0 100 tt,I UI ~ I/, Hz l Figure 3. ) and 1984 (~). , Figure 2) with evident concentration of power within relatively narrow frequency band. A careful consideration of these PS showed that only 20% of peaks from both spectra coincide with the accuracy +5 microHz; frequencies of the rest of the peaks differ oy more than 30 microHz. ~ ~II •• ii Figure 4. , 1980) and atmospheric pressure fluctuations (x). A. B. SEVERNY ET AL. isk" velocity measurements than for the differential method, we compared the PS of atmospheric pressure with the results of Grec et ale (1980), see Figure 4.
Tsap Crimean Astrophysical Observatory Nauchny, Crimea 334413 USSR ABSTRACT. The Earth atmospheric pressure fluctuations in the 5-min range of periods are analysed and their influence on observations of solar 5-min oscillations are briefly discussed. 010 min. , 1976). , 1984) which was independently detected in Doppler velocity measurements by Brookes et al. (1976), Scherrer et a1. (1979), Grec et ale (1980) and recently in the solar diameter measurements by Hill et ale (1985). A detailed analysis of the available data indicates that the 160-min oscillations may correspond to spherical harmonic 1=3 (Kosovichev and Severny, 1986).
Advances in Helio- and Asteroseismology: Proceedings of the 123th Symposium of the International Astronomical Union, Held in Aarhus, Denmark, July 7–11, 1986 by Jørgen Christensen-Dalsgaard (auth.), Jørgen Christensen-Dalsgaard, Søren Frandsen (eds.)