Abstract
The results of spectropolarimetric and filter observations of a faculae region located near the solar disc center in the Fe I 1564.3, Fe I 1565.8, Ba II 455.4, and Ca II H 396.8 nm lines are discussed. The observation data are obtained using the German vacuum tower telescope of Observatorio del Teide (Tenerife, Spain). Observations of the faculae region are made simultaneously in the three spectral regions: spectropolarimetric observations of the I, Q, U, and V Stokes parameters of two neutral iron lines Fe I 1564.8 and Fe I 1565.2 nm with a time resolution of 6 min 50 s; filter observations in 37 sections of the profile of the ionized barium Ba II 455.4 nm line with a time resolution of 25.6 s; and filter observations only in the center of the ionized calcium Ca II H 396.8 nm line with a time resolution of 4.9 s. The following observation data are studied: (1) the power of the magnetic field at the altitude of the formation of a continuous spectrum near the Fe I 1564.8 and Fe I 1565.2 nm lines (h ≈ −100 km); (2) wave velocities at fourteen altitude levels in the atmosphere of the Sun, at which radiation in the Ba II 455.4 nm spectral line is formed (h ≈ 0−650 km), and calculated phase shifts Φ(V,V) between fluctuations of velocity V in the photosphere at the height of radiation formation in the center of this line (h ≈ 650 km) and velocity fluctuations at the other thirteen altitude levels; and (3) the faculae contrast at the altitude of formation of the Ca II H 396.8 nm line center (h ≈ 1600 km). The following two trends are shown: (1) The power of velocity fluctuations greatly varies depending on the frequency of oscillations with a change in the altitude in the atmosphere of the Sun. At the altitudes ranging from 0 to 300 km, the maximum oscillation power occurs at a frequency of 3.5 mHz. Another maximum occurs near a frequency of 4.5 mHz at the altitude level of h = 650 km, and the maximum oscillation power at a frequency of approximately 1.5 mHz is quite noticeable at an altitude of h = 1600 km. (2) The contrast in the center of the Ca II H 396.8 nm line (h = 650 km) does not monotonically increase with an increase in the intensity of the photospheric magnetic field, as might be expected from general considerations. At large magnetic fields (B > 140 mT), this dependence becomes inverse.
REFERENCES
V. Abbasvand, M. Sobotka, P. Heinzel, et al., “Chromospheric heating by acoustic waves compared to radiative cooling. II. Revised grid of models,” Astrophys. J. 890, 22–28 (2020).
C. Beck, E. Khomenko, R. Rezaei, and M. Collados, “The energy of waves in the photosphere and lower chromosphere I. Velocity statistics,” Astron. Astrophys. 507, 453–467 (2009).
T. E. Berger, L. H. M. Rouppe van der Voort, M. G. Löfdahl, et al., “Solar magnetic elements at 0.1 arcsec resolution. General appearance and magnetic structure,” Astron. Astrophys. 428, 613–628 (2004).
P. S. Cally and E. Khomenko, “Fast-to-Alfvén mode conversion mediated by the Hall current. I. Cold plasma model,” Astrophys. J. 814, 106–116 (2015).
M. Carlsson, R. F. Stein, Å. Nordlund, and G. B. Scharmer, “Observational manifestations of solar magnetoconvection: Center-to-limb variation,” Astrophys. J. 610, L137–L140 (2004).
M. Collados, A. Lagg, J. J. Díaz García, et al., “Tenerife infrared polarimeter II. The physics of chromospheric plasmas,” in The Physics of Chromospheric Plasmas, Ed. by P. Heinzel, I. Dorotovič, and R. J. Rutten (Astronomical Society of the Pacific, San Francisco, Calif., 2007), in Ser.: ASP Conference Series, Vol. 368, pp. 611–616.
O. Gingerich, R. W. Noyes, W. Kalkofen, and Y. Cuny, “The Harvard–Smithsonian reference atmosphere,” Sol. Phys. 18, 347–365 (1971).
P. A. Gonzalez-Morales, E. Khomenko, N. Vitas, and M. Collados, “Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun. I. Dissipation and generation of waves,” Astron. Astrophys. 642, A220–A237 (2020).
J. Hirzberger and E. Wiehr, “Solar limb faculae,” Astron. Astrophys. 438, 1059–1065 (2005).
C. U. Keller, M. Schüssler, A. Vögler, and V. Zakharov, “On the origin of solar faculae,” Astrophys. J. Lett. 607, 59–62 (2004).
E. Khomenko, “Simulations of waves in sunspots,” in Solar-Stellar Dynamos as Revealed by Helio- and Asteroseismology: GONG 2008/SOHO 21, Ed. by M. Dikpati, T. Arentoft, I. González Hernández, C. Lindsey, and F. Hill (Astronomical Society of the Pacific, San Francisco, Calif., 2009), in Ser: ASP Conference Series, Vol. 416, pp. 31–40.
E. Khomenko and P. S. Cally, “Numerical simulations of conversion to Alfvén waves in sunspots,” Astrophys. J. 746, 68–77 (2012).
P. Kobel, S. K. Solanki, and J. M. Borrero, “The continuum intensity as a function of magnetic field. I. Active region and quiet Sun magnetic elements,” Astron. Astrophys. 531, A112–A123 (2011).
R. I. Kostik and E. Khomenko, “Observations of a bright plume in solar granulations,” Astron. Astrophys. 476, 341–347 (2007).
R. Kostik and E. Khomenko, “Properties of convective motions in facular regions,” Astron. Astrophys. 545, A22–A30 (2012).
R. Kostik and E. Khomenko, “Properties of oscillatory motions in a facular region,” Astron. Astrophys. 559, A107–A116 (2013).
R. Kostik and E. Khomenko, “The possible origin of facular brightness in the solar atmosphere,” Astron. Astrophys. 589, A6–A12 (2016).
R. Kostyk, “What are solar faculae?,” Kinematic Phys. Celestial Bodies 29, 32–36 (2013).
R. I. Kostyk, “What mechanisms allow 5-minute oscillations in active regions of the solar surface to penetrate from the photosphere into the chromosphere?,” Kinematic Phys. Celestial Bodies 31, 188–192 (2015).
R. I. Kostyk, “Effect of wave motions in the active region of the solar surface on convection,” Kinematic Phys. Celestial Bodies 34, 82–87 (2018).
J. L. Linsky and H. E. Avrett, “The solar H and K lines,” Publ. Astron. Soc. Pac. 82, 169–248 (1970).
M. Montagne, R. Mueller, and J. Vigneau, “The photosphere of the Sun: statistical correlations between magnetic field, intensity and velocity,” Astron. Astrophys. 311, 304–310 (1996).
G. Narayan and G. B. Scharmer, “Small-scale convection signatures associated with a strong plage solar magnetic field,” Astron. Astrophys. 524, A3–A18 (2010).
S. P. Rajaguru, C. R. Sangeetha, and D. Tripathi, “Magnetic fields and the supply of low-frequency acoustic wave energy to the solar chromospheres,” Astrophys. J. 871, 155–169 (2019).
R. Rezaei, J. H. M. J. Bruls, W. Schmidt, C. Beck, W. Kalkofen, and R. Schlichenmaier, “Reversal-free Ca II H profiles: A challenge for solar chromosphere modeling in quiet inter-network,” Astron. Astrophys. 484, 503–509 (2008).
B. Ruiz Cobo and J. C. del Toro Iniesta, “Inversion of Stokes profiles,” Astrophys. J. 398, 375–385 (1992).
E. H. Schroeter, D. Soltau, and E. Wiehr, “The German solar telescopes at the Observatorio del Teide,” Vistas Astron. 28, 519–525 (1985).
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).
S. Shelyag, E. Khomenko, Á. de Vicente, and D. Przybylski, “Heating of the partially ionized solar chromosphere by waves in magnetic structures,” Astrophys. J., Lett. 819, L11–L16 (2016).
M. Sobotka, P. Heinzel, M. Svanda, et al., “Chromospheric heating by acoustic waves compared to radiative cooling,” Astrophys. J. 826, 49–56 (2016).
Solanki S. K. “Small scale solar magnetic fields. An overview,” Space Sci. Rev. 63, 188 (1993).
A. K. Srivastava, J. L. Ballester, P. S. Cally, et al., “Chromospheric heating by magnetohydrodynamic waves and instabilities,” J. Geophys. Res.: Space Phys. 126, e2020JA029097 (2021). arXiv 2104.02010
M. Stangalini, D. del Moro, F. Berrilli, and S. M. Jeeries, “MHD wave transmission in the Sun’s atmosphere,” Astron. Astrophys. 534, A65–A71 (2011).
R. Stebbins and P. R. Goode, “Waves in the solar photosphere,” Sol. Phys. 110, 237–253 (1987).
M. I. Stodilka and R. I. Kostyk, “Solar faculae: Microturbulence as an indicator of inclined magnetic fields,” Kinematic Phys. Celestial Bodies 36, 153–160 (2020).
M. I. Stodilka, A. I. Prysiazhnyi, and R. I. Kostyk, “Features of convection in the atmosphere layers of the solar facula,” Kinematic Phys. Celestial Bodies 35, 261–270 (2019).
A. M. Title, K. P. Topka, T. D. Tarbell, et al., “On the differences between plage and quiet Sun in the solar photosphere,” Astrophys. J. 393, 782–794 (1992).
K. P. Topka, T. D. Tarbell, and A. M. Title, “Properties of the smallest solar magnetic elements. II. Observations versus hot wall models of faculae,” Astrophys. J. 484, 479–486 (1997).
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).
ACKNOWLEDGMENTS
I am sincerely grateful to Prof. Manuel Callados and Prof. Elena Khomenko, the members of the Canary Islands Institute of Astrophysics, for their assistance in obtaining observation data from the vacuum tower telescope (Observatory del Teide, Tenerife Island, Spain) and for providing us with the SIR software package and also to the reviewer for his useful comments.
Funding
This study was supported by ongoing institutional funding. No additional grants to carry out or direct this particular research were obtained.
Author information
Authors and Affiliations
Corresponding author
Ethics declarations
The author of this work declares that she has no conflicts of interest.
Additional information
Publisher’s Note.
Allerton Press remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
About this article
Cite this article
Kostik, R.I. Solar Faculae and Flocculent Flows: Spectropolarimetric and Filter Observations in the Fe I, Ba II, and Ca II Lines. Kinemat. Phys. Celest. Bodies 40, 40–46 (2024). https://doi.org/10.3103/S0884591324010069
Received:
Revised:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.3103/S0884591324010069