Abstract
According to the data of complex 2D observations on the VTT telescope of the solar facula, a 3D model of the solar atmosphere in the facular region was obtained by solving the inverse radiative transfer problem in the Ba II 4554 A line. The magnetic field was estimated using the Stokes V profiles of the Fe I 15648 A line. The influence of magnetic field on photospheric convection was investigated: spatial variations in temperature and velocities at different heights were considered. It is shown that the mutual transformation of the mechanical and thermal energy of the solar plasma into magnetic energy occurs in the layers of the middle photosphere. The integral effect of a small-scale magnetic dynamo leads to lowering the temperature and slowing down the motion of the predominant downward flows in the layers of the middle photosphere in the facular regions with a strong field (greater than 1 kG), while there is an increase in temperature and acceleration of the motion of the predominant upward flows in the layers of the middle photosphere in the facular regions with a weak field (less than 1 kG). It is shown that the magnetic field of the facula stabilizes photospheric convection, and the small-scale magnetic dynamo causes a double temperature inversion in the photospheric layers of the facula.
Similar content being viewed by others
REFERENCES
O. A. Baran and M. I. Stodilka, “Convection structure in the solar photosphere at granulation and mesogranulation scales,” Kinematics Phys. Celestial Bodies 31, 65–72 (2015).
R. I. Kostyk, “Magnetic field effect on the fine structure of convective motions in the solar atmosphere,” Kinematics Phys. Celestial Bodies 28, 155–161 (2012).
R. I. Kostyk, “What are solar faculae?” Kinematics Phys. Celestial Bodies 29, 32–36 (2013).
V. L. Ol’shevskii, N. G. Shchukina, and I. E. Vasil’eva, “NLTR-formation of the Ba II 455.4 nm resonance line in the solar atmosphere,” Kinematics Phys. Celestial Bodies 24, 145–158.
M. N. Pasechnik, “Spectral study of Ellerman bombs. Photosphere,” Kinematics Phys. Celestial Bodies 34, 68–81 (2018).
A. I. Prysiazhnyi, M. I. Stodilka, and N. G. Shchukina, “Robust method for determination of magnetic field strength in the solar photosphere,” Kinematics Phys. Celestial Bodies 34, 277–289 (2018).
M. I. Stodilka and A. I. Prysiazhnyi, “Diagnostics of the solar atmosphere by the Non-LTE inversion method: Line of Ba II 455.403 nm,” Kinematics Phys. Celestial Bodies 32, 23–29 (2016).
M. I. Stodilka, “The Tychonoff stabilizers in inverse problems of spectral studies,” Kinematics Phys. Celestial Bodies 19, 229–235 (2003).
J. M. Borrero, S. Jafarzadeh, M. Schussler, and S. K. Solanki, “Solar magnetoconvection and small-scale dynamo. Recent developments in observation and simulation,” Space Sci. Rev. 210, 275–316 (2017).
D. Buehler, A. Lagg, S. K. Solanki, and M. van Noort, “Properties of solar plage from a spatially coupled inversion of Hinode SP data,” Astron. Astrophys. 576, A27 (2015).
G. A. Chapman and N. R. Sheeley, Jr., “The Photospheric Network,” Sol. Phys 5, 442–461 (1968).
A. Cristaldi and I. Ermolli, ID atmosphere models from inversion of Fe I 630nm observation with an application to solar irradiance studies,” Astrophys. J. 841, 115 (2017).
H. Hotta, M. Rempel, and T. Yokoyama, “Efficient small-scale dynamo in the solar convection zone,” Astrophys. J. 803, 42 (2015).
C. U. Keller, M. Schiissler, A. Vogler, and V. Zakharov, “On the origin of solar faculae,” Astrophys. J. Lett. 607, L59–L62 (2004).
R. Kostik and E. V. Khomenko, “Properties of convective motions in facular regions,” Astron. Astrophys. 545, A22 (2012).
R. Kostik and E. Khomenko, “Properties of oscillatory motions in a facular region,” Astron. Astrophys. 559, A107 (2013).
C. M. Norris, B. Beeck, Y. C. Unruh, et al., “Spectral variability of photospheric radiation due to faculae. I. The Sun and Sun-like stars,” Astron. Astrophys. 605, A45 (2017).
O. V. Okunev and F. Kneer, “Numerical modeling of solar faculae close to the limb,” Astron. Astrophys. 439, 323–334 (2005).
K. Petrovay and G. Szakaly, “The origin of intranetwork fields: A small-scale solar dynamo,” Astron. Astrophys. 274, 543–554 (1993).
R. J. Rutten, “Extreme limb observations of Ba II 4554 and Mg 1 4571,” Sol. Phys. 51, 3–24 (1977).
R. J. Rutten, “Empirical NLTE Analyses of Solar Spectral Lines. II — The formation of the Ba II 4554 resonance line,” Sol. Phys. 56, 237–262 (1978).
R. J. Rutten and R. W. Milkey, “Partial redistribution in the solar photospheric Ba II spectrum,” Astrophys. J. 231, 277–283 (1979).
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).
H. Socas-Navarro, “Semiempirical models of solar magnetic structures,” Astrophys. J. Suppl. Ser. 169, 439–457 (2007).
O. Steiner, “Radiative properties of magnetic elements. II. Center to limb variation of the appearance of photospheric faculae,” Astron. Astrophys. 430, 691–700 (2005).
J. E. Vernazza, E. H. Avrett, and R. Loeser, “Structure of the solar chromosphere. III. Models of the EUV brightness components of the quiet Sun,” Astrophys. J. Suppl. Ser. 45, 635–725 (1981).
Funding
This work was partly supported by the Ministry of Education and Science of Ukraine at the Ivan Franko National University of Lviv as part of research work on the project AO-91F.
Author information
Authors and Affiliations
Corresponding authors
Additional information
Translated by S. Avodkova
About this article
Cite this article
Stodilka, M.I., Prysiazhnyi, A.I. & Kostyk, R.I. Features of Convection in the Atmospheric Layers of the Solar Facula. Kinemat. Phys. Celest. Bodies 35, 261–270 (2019). https://doi.org/10.3103/S0884591319060059
Received:
Revised:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.3103/S0884591319060059