Effect of wave motions in the active region of the solar surface on convection
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| 1Kostyk, RI 1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine |
| Kinemat. fiz. nebesnyh tel (Online) 2018, 34(2):46-54 |
| https://doi.org/10.15407/kfnt2018.02.046 |
| Start Page: Solar Physics |
| Language: Russian |
Abstract: The results of observations of the active region (faculae) near the center of the solar disk, which were obtained on the German Vacuum Tower Telescope VTT (Tenerife, Spain) are discussed. We have determined that the decrease in the contrast (brightness) of the faculae with an increase in the magnetic field from 1300 G to 1600 G is due to the fact that in this range of magnetic field strengths the V_V phase shift of the waves is close to zero (ΦVV ≈ 0), i.е. the wave becomes stationary and does not transfer energy from the photosphere to the chromosphere. Sound waves that propagate from the chromosphere towards the photosphere significantly affect the temperature characteristics of turbulent vortices at the level of formation of the continuous spectrum, in particular, the contrast of the granules under the influence of these waves can increase by 25 %. |
| Keywords: faculae, granulation, oscillations, the Sun |
References:
1.M. Collados, A. Lagg, A. J. J. Diaz Garci, et al., “Tenerife infrared polarimeter II,” in Proc. The Physics of Chromospheric Plasmas, Coimbra, Portugal, Oct. 9–13, 2006, Ed. by P. Heinzel, I. Dorotovi., and R. J. Rutten (Astronomical Society of the Pacific, San Francisco, CA, 2007), in Ser.: ASP Conference Series, Vol. 368, 611–616 (2007).
2.O. Gingerich, R. W. Noyes, W. Kalkofen, et al., “The Harvard–Smithsonian reference atmosphere,” Sol. Phys. 18, 347–365 (1971).
https://doi.org/10.1007/BF00149057
3.H. Holweger, and L. Testerman, “Five-minute oscillations of solar equivalent widths,” Sol. Phys. 43, 271–284 (1975).
https://doi.org/10.1007/BF00152351
4.E. Khomenko, R. I. Kostik, and N. G. Shchukina, “Five-minute oscillations above granules and intergranular lanes,” Astron. Astrophys. 369, 660–671 (2001).
https://doi.org/10.1051/0004-6361:20010129
5.R. I. Kostik, and E. Khomenko, “Observations of a bright plume in solar granulations,” Astron. Astrophys. 476, 341–347 (2007).
https://doi.org/10.1051/0004-6361:20077163
6.R. Kostik and E. Khomenko, “Properties of convective motions in facular regions,” Astron. Astrophys. 545, A22 (2012).
https://doi.org/10.1051/0004-6361/201219534
7.R. Kostik and E. Khomenko, “The possible origin of facular brightness in the solar atmosphere regions,” Astron. Astrophys. 589, A6 (2016).
https://doi.org/10.1051/0004-6361/201527419
8.R. Kostik, E. Khomenko, and N. Shchukina, “Solar granulation from photosphere to low chromosphere observed in Ba II 4554 Å line,” Astron. Astrophys. 506, 1405–1415 (2009).
https://doi.org/10.1051/0004-6361/200912441
9.R. I. Kostyk and E. V. Khomenko, “The effect of acoustic waves on spectral-line profiles in the solar atmosphere: Observations and theory,” Astron. Rep. 46, 925–931 (2002).
https://doi.org/10.1134/1.1522081
10.J. L. Linsky and H. E. Avrett, “The Solar H and K lines,” Publ. Astron. Soc. Pac. 82 (485) 169L–248L (1970).
https://doi.org/10.1086/128904
11.B. Ruiz Cobo and J. C. del Toro Iniesta, “Inversion of Stokes profiles,” Astrophys. J. 398, 375–385 (1992).
https://doi.org/10.1086/171862
12.E. H. Schroeter, D. Soltau, and E. Wiehr, “The German solar telescopes at the observatorio del Teide,” Vistas Astron. 28, 519–525 (1985).
https://doi.org/10.1016/0083-6656(85)90073-X
13.N. G. Shchukina, V. L. Olshevsky, and E. V. Khomenko, “The solar Ba II 4554 Å line as a Doppler diagnostic: NLTE analysis in 3D hydrodynamical model,” Astron. Astrophys. 506, 1393–1404 (2009).
https://doi.org/10.1051/0004-6361/200912048
14.R. Stebbins and P. R. Goode, “Waves in the solar photosphere,” Sol. Phys. 110, 237–253 (1987).
https://doi.org/10.1007/BF00206421
15.A. Tritschler, W. Schmidt, K. Langhans, and T. Kentischer, “High-resolution solar spectroscopy with TESOS — Upgrade from a double to a triple system,” Sol. Phys. 211, 17–29 (2002).
https://doi.org/10.1023/A:1022459132089