Abstract
We developed a code for imaging the surfaces of spotted stars by a set of circular spots with a uniform temperature distribution. The flux from the spotted surface is computed by partitioning the spots into elementary areas. The code takes into account the passing of spots behind the visible stellar limb, limb darkening, and overlapping of spots. Modeling of light curves includes the use of recent results of the theory of stellar atmospheres needed to take into account the temperature dependence of flux intensity and limb darkening coefficients. The search for spot parameters is based on the analysis of several light curves obtained in different photometric bands. We test our technique by applying it to HII 1883.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
S. S. Vogt and G. D. Penrod, Publ. Astronom. Soc. Pacific 95, 565 (1983).
E. Budding, Astrophys. and Space Sci. 48, 207 (1977).
J. D. Dorren, Astrophys. J. 320, 756, (1987).
Z. Eker, Astrophys. J. 420 373, (1994).
K. G. Strassmeier, Astrophys. and Space Sci. 140, 223 (1988).
R. Harmon and L. Crews, Astronom. J. 120, 3274 (2000).
A. I. Kolbin, V. V. Shimansky, and N. A. Sakhibullin, Astronomy Reports 57, 548 (2013).
W. Van Hamme, Astronom. J. 5, 2096 (1993).
R. Kurucz, SAO CD-ROMs (1994).
A. Azusienis and V. Straizys, Sov. Astron. 13 316 (1969).
H. L. Johnson, Astrophys. J. 141, 923 (1965).
M. S. Bessell, Publ. Astronom. Soc. Pacific 95, 480 (1983).
S. S. Vogt, Astrophys. J. 250, 327 (1981).
Ph. E. Gill, W. Murray, and M. H. Wright, Practical Optimization (Academic press, London, 1984).
P. Alphenaar and F. van Leeuwen, Inform. Bull. Var. Stars 1957 (1981).
J. J. Meys, P. Alphenaar, and F. van Leeuwen, Inform. Bull. Var. Stars 2115 (1982).
F. van Leeuwen and P. Alphenaar, ESO Messenger 28, 15 (1982).
J. R. Stauffer, L. Hartmann, D. R. Soderblom, and N. Burnham, Astrophys. J. 280, 202 (1984).
J. R. Stauffer, J. D. Dorren, and J. L. Africano, Astronom. J. 91, 1443 (1986).
G.W. Marcy, D. K. Duncan, and B. D. Cohen, Astrophys. J. 288, 259 (1985).
L. W. Hartmann and R. W. Noyes, Annual Rev. Astronom. Astrophys. 25, 271 (1987).
D. Clarke, Astronom. and Astrophys. 421, 273 (2004).
M. S. Bessell and E. W. Weis, Publ. Astronom. Soc. Pacific 99, 642 (1987).
M. S. Bessell, Publ. Astronom. Soc. Pacific 91, 589 (1979).
G. V. Schultz and W. Wiemer, Astronom. and Astrophys. 43, 133 (1975).
A. M. Boesgaard and E. D. Friel, Astrophys. J. 351, 467 (1990).
A. Alonso, S. Arribas, and C. Martinez-Roger, Astronom. and Astrophys. 313, 873 (1996).
D. An, D. M. Terndrup, M. H. Pinsonneault, et al., Astronom. J. 655, 233 (2007).
L. Girardi, A. Bressan, G. Bertelli, and C. Chiosi, Astronom. and Astrophys. Suppl. 141, 371 (2000).
M. A. O’Dell, M. A. Hendry, and A. Collier Cameron, Monthly Notices Royal Astronom. Soc. 268, 181 (1994).
T. G. Barnes, D.S. Evans, T.J. Moffet, Monthly Notices Royal Astronom. Soc. 183, 285 (1978).
M. S. O’Brien and H. E. Bond, Astrophys. J. 563, 971 (2001).
J. R. Stauffer and L. W. Hartmann, Astrophys. J. 318, 337 (1987).
I. S. Savanov and K. G. Strassmeier, Astronomische Nachrichten 329, 364 (2008).
Author information
Authors and Affiliations
Corresponding author
Additional information
Original Russian Text © A.I. Kolbin, V.V. Shimansky, 2014, published in Astrofizicheskij Byulleten, 2014, Vol. 69, No. 2, pp. 190–202.
Rights and permissions
About this article
Cite this article
Kolbin, A.I., Shimansky, V.V. Spotted star light curve numerical modeling technique and its application to HII 1883 surface imaging. Astrophys. Bull. 69, 179–190 (2014). https://doi.org/10.1134/S1990341314020059
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1134/S1990341314020059