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Theory of spots on chemically peculiar stars

Published online by Cambridge University Press:  10 September 2015

D. Shulyak
Institute for Astrophysics, Georg-August-University, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
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Surface inhomogeneities are found in many stars. In active sun-like stars and cool giants temperature spots similar to that found in the Sun are recovered from the inversion of spectroscopic data. M-dwarfs also show highly inhomogeneous surface structures in polarized light and photometric variability that are believed to be connected with cool regions on their surface, too. Supergiants have highly inhomogeneous atmospheres because large convective cells, and therefore bright and dark regions, have sizes comparable to the size of stars themselves. Hot luminous stars can have dense clamps in their atmospheres caused by an interaction of fast stellar wind, rotation, and the magnetic fields. Finally, a special class of main-sequence B-F stars, called chemically peculiar stars, have spots of abundance origin. Spots in these stars can look bright or dark depending on wavelength of observation. Modern interferometry is capable of reaching a very high angular resolution that will make it possible to study starspots in very detail. In this review we will focus on starspots in general and abundance spots in chemically peculiar stars in particular, as well as possible application of interferometry to study them.

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© EAS, EDP Sciences, 2015

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Alecian, G., & Stift, M.J., 2007, A&A, 475, 659
Babcock, H.W., 1960, ApJ, 132, 521CrossRef
Berdyugina, S.V., 2005, Liv. Rev. Solar Phys., 2, 8
Berdyugina, S.V., 1998, A&A, 338, 97
Bruntt, H., Kervella, P., Mérand, A., et al., 2010, A&A, 512, A55
Bruntt, H., North, J.R., Cunha, M., et al., 2008, MNRAS, 386, 2039CrossRef
Catalano, S., Biazzo, K., Frasca, A., & Marilli, E., 2002, A&A, 394, 1009
Deutsch, A.J., 1958, Electromagnetic Phenomena in Cosmical Physics, 6, 209
Donati, J.-F., Morin, J., Petit, P., et al., 2008a, MNRAS, 390, 545CrossRef
Donati, J.-F., Moutou, C., Farès, R., et al., 2008b, MNRAS, 385, 1179CrossRef
Donati, J.-F., Semel, M., & Praderie, F., 1989, A&A, 225, 467
Goncharskii, A.V., Stepanov, V.V., Kokhlova, V.L., & Yagola, A.G., 1977, Soviet. Astron. Lett., 3, 147
Gray, D.F., 1996, Stellar Surface Structure, 176, 227
Irwin, J., Berta, Z.K., Burke, C.J., et al., 2011, ApJ, 727, 56CrossRef
Jankov, S., Domiciano de Souza, A., Jr., Stehle, C., et al., 2003, Proc. SPIE, 4838, 587CrossRef
Johns-Krull, C.M., & Valenti, J.A., 2000, Stellar Clusters and Associations: Convection, Rotation, and Dynamos, 198, 371
Johns-Krull, C.M., & Valenti, J.A., 1996, ApJ, 459, L95CrossRef
Kochukhov, O., Shulyak, D., & Ryabchikova, T., 2009, A&A, 499, 851
Kochukhov, O., Adelman, S.J., Gulliver, A.F., & Piskunov, N., 2007, Nature Physics, 3, 526CrossRef
Korhonen, H., 2014, IAU Symposium, 302, 350
Korhonen, H., 2013 [arXiv:1310.3678]
Elkin, V.G., Mathys, G., Kurtz, D.W., Hubrig, S., & Freyhammer, L.M., 2010, MNRAS, 402, 1883CrossRef
Lanza, A.F., Catalano, S., Cutispoto, G., Pagano, I., & Rodono, M., 1998, A&A, 332, 541
Leblanc, F., Monin, D., Hui-Bon-Hoa, A., & Hauschildt, P.H., 2009, A&A, 495, 937
Lueftinger, T., Kuschnig, R., Piskunov, N.E., & Weiss, W.W., 2003, A&A, 406, 1033
Morin, J., Donati, J.-F., Petit, P., et al., 2010, MNRAS, 407, 2269CrossRef
Michaud, G., 1970, ApJ, 160, 641CrossRef
Nesvacil, N., Lüftinger, T., Shulyak, D., et al., 2012, A&A, 537, A151
Piskunov, N., & Kochukhov, O., 2002, A&A, 381, 736
Perraut, K., Borgniet, S., Cunha, M., et al., 2013, A&A, 559, A21
Perraut, K., Brandão, I., Mourard, D., et al., 2011, A&A, 526, A89
Piskunov, N.E., Tuominen, I., & Vilhu, O., 1990, A&A, 230, 363
Reiners, A., 2012, Liv. Rev. Solar Phys., 9, 1
Reiners, A., & Basri, G., 2007, ApJ, 656, 1121CrossRef
Rice, J.B., & Strassmeier, K.G., 2000, A&AS, 147, 151PubMed
Rousselet-Perraut, K., Stehlé, C., Lanz, T., et al., 2004, A&A, 422, 193
Ryabchikova, T., & Leblanc, F., 2011, Ap&SS, 335, 77
Samadi, R., Belkacem, K., & Ludwig, H.-G., 2013, A&A, 559, A39
Semel, M., 1989, A&A, 225, 456
Shulyak, D., Paladini, C., Causi, G.L., Perraut, K., & Kochukhov, O., 2014, MNRAS, 443, 1629CrossRef
Shulyak, D., Reiners, A., Seemann, U., Kochukhov, O., & Piskunov, N., 2014, A&A, 563, A35
Shulyak, D., Ryabchikova, T., & Kochukhov, O., 2013, A&A, 551, A14
Shulyak, D., Krtička, J., Mikulášek, Z., Kochukhov, O., & Lüftinger, T., 2010, A&A, 524, A66
Shulyak, D., Ryabchikova, T., Mashonkina, L., & Kochukhov, O., 2009, A&A, 499, 879
Solanki, S.K., 2003, A&ARv, 11, 153PubMed
Strassmeier, K.G., 2009, A&ARv, 17, 251
Strassmeier, K.G., 1999, A&A, 347, 225
Vogt, S.S., Penrod, G.D., & Hatzes, A.P., 1987, ApJ, 321, 496CrossRef
Wittkowski, M., Schöller, M., Hubrig, S., Posselt, B., & von der Lühe, O., 2002, Astron. Nachr., 323, 2413.0.CO;2-D>CrossRef

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Theory of spots on chemically peculiar stars
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