Darkening of the Sun prior to surface appearance of sunspot flux tubes and magneto-thermal pulsation of the Sun

Details Darkening of the Sun prior to surface appearance of sunspot flux tubes and magneto-thermal pulsation of the Sun Darkening of the Sun prior to surface appearance of sunspot flux tubes and magneto-thermal pulsation of the Sun

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994an....315..371y&link_type=abstract

Astronomische Nachrichten (ISSN 0004-6337), vol. 315, no. 5, p. 371-390

Astronomy and Astrophysics

Astronomy

5

Heat Transfer, Irradiance, Magnetic Flux, Solar Convection (Astronomy), Stellar Luminosity, Sunspots, Thermomagnetic Effects, Solar Maximum Mission, Solar Oscillations, Stellar Magnetic Fields, Time Lag

Scientific paper

We found an evidence that the luminosity of the Sun systematically decreased about 20 days before sunspot surface appearance by analyzing time-lag correlation of time derivatives of running mean time profiles of the data ofthe Active Cavity Radiometer Irradiance Monitor (ACRIM) I experiment on board of Solar Maximum Mission (SMM) and of the data of the daily sunspot number. This indicates that sunspot flux tube cooling and heat transfer blocking by the flux tubes start to take place in the interior of the solar convection zone well before the sunspot surface appearance. From this finding and our previous finding that the luminosity of the Sun systematically increased and the blocked heat appeared on the surface about 50 days after the sunspot surface appearance, a new view of sunspot formation and dynamics and a new view of the luminosity modulation emerged. (1) Sunspots of a solar cycle are formed from clusters of flux tubes which can be seen in the running time mean profile of the sunspot number as a peak with duration on the order of 100 to 200 days. (2) Heat flow is blocked by the cluster of sunspot flux tubes inside the convection zone to decrease the luminosity about 20 days before the surface emergence of the sunspot cluster. (3) The blocked heat appears on the surface about 50 days after the surface emergence of the cluster of sunspot flux tubes to heat up the surface. This appears as a thermal pulse in the running mean time profile of the ACRIM data in between the peaks of the sunspot running mean time profile. This process of heating the surface makes the temperature gradient less steep and weakens the bouyancy of sunspot flux tubes below the surface. (4) The radiative cooling of the surface layer by the excess heat release steepens the temperature gradient so that the bouyancy of the sub-surface magnetic flux tubes becomes stronger to cause the next surge of emergence of a cluster of sunspots and other magnetic activities, which creates a peak in the time profile of the sunspot number. We call this peak a magnetic pulse of the Sun and the coupled process of alternating pulsed appearance of heat and sunspots the magnetio-thermal pulsation of the Sun.

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