The influence of magnetic field on the propagation of 5-min oscillations in the solar atmosphere: the phase shifts
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| 1Kostyk, RI, 1Shchukina, NG, 2Kobanov, NI, 2Pulyaev, VA 1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine 2Institute of Solar-Terrestrial Physics of the Siberian Branch of the RAS, Irkutsk, Russia |
| Kinemat. fiz. nebesnyh tel (Online) 2014, 30(1):61-69 |
| Start Page: Solar Physics |
| Language: Russian |
Abstract: Using some results of spectral (in Ba ІІ 455.4 nm line) and spectropolarimetric (in Fe I 1564.3—1565.8 nm lines) observations of the active region (isolated faculae in the solar disk center) with the German Vacuum Tower Telescope (VTT) at the Canaries Institute of Astrophysics, we investigated some properties of the propagation of five-minute oscillations from the base of the photosphere (h = 0 km) to the bottom of the chromosphere (h = 650 km). At the height of the continuum formation (h = 0 km) the nature of wave propagation in active and quiet regions are not much different: from 80 % to 90 % of the investigated areas are occupied by waves moving up and down. In the lower chromosphere (h = 650 km), the differences in the behavior of the waves are fundamental. In a quiet area, the waves become standing for 90 % of the cases. In contrast to this, in the presence of moderate and strong magnetic fields (B = 30—180 nT), for 47 % of the cases, the waves are running up, giving the principal possibility to heat the active region. Our investigation revealed the presence of the waves in the active region, ΦT,V phase shift of which is between –90° and 0°. The waves with such ΦT,V phase shifts can not propagate in a quiet atmosphere. |
| Keywords: atmosphere, magnetic field, Sun |
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