Hostname: page-component-78c5997874-g7gxr Total loading time: 0 Render date: 2024-11-13T11:55:21.629Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of stellar winds from the Sun to red giants

Published online by Cambridge University Press:  01 September 2008

Takeru K. Suzuki
Takeru K. Suzuki*
Affiliation:
School of Arts and Sciences, University of Tokyo, Komaba, Meguro, Tokyo, Japan153-8902 email: stakeru@ea.c.u-tokyo.ac.jp
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

By performing global 1D MHD simulations, we investigate the heating and acceleration of solar and stellar winds in open magnetic field regions. Our simulation covers from photosphere to 20-60 stellar radii, and takes into account radiative cooling and thermal conduction. We do not adopt ad hoc heating function; heating is automatically calculated from the solutions of Riemann problem at the cell boundaries. In the solar wind case we impose transverse photospheric motions with velocity ~1 km/s and period between 20 seconds and 30 minutes, which generate outgoing Alfvén waves. We have found that the dissipation of Alfvén waves through compressive wave generation by decay instability is quite effective owing to the density stratification, which leads to the sufficient heating and acceleration of the coronal plasma. Next, we study the evolution of stellar winds from main sequence to red giant phases. When the stellar radius becomes ~10 times of the Sun, the steady hot corona with temperature 106 K, suddenly disappears. Instead, many hot and warm (105 – 106 K) bubbles are formed in cool (T < 2 × 104 K) chromospheric winds because of the thermal instability of the radiative cooling function; the red giant wind is not a steady stream but structured outflow.

Keywords

wavesMHDSun: photosphereSun: chromosphereSun: Coronasolar windstars: chromospheresstars: coronaestars: magnetic fieldsstars: mass lossstars: late-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 589 - 599
Copyright
Copyright © International Astronomical Union 2009

References

Axford, W. I. & McKenzie, J. F. 1997 The Solar Wind in “Cosmic Winds and the Heliosphere”, Eds. Jokipii, J. R., Sonnet, C. P., and Giampapa, M. S., University of Arizona Press, 31Google Scholar
Ayres, T. R., Simon, T., Stern, R. A., Drake, S. A., Wood, B. E., & Brown, A. 1998 ApJ, 496, 428CrossRefGoogle Scholar
Banerjee, D., Teriaca, L., Doyle, J. G., & Wilhelm, K. 1998 A&A, 339, 208Google Scholar
Canals, A., Breen, A. R., Ofman, L., Moran, P. J., & Fallows, R. A., 2002 Ann. Geophys., 20, 1265CrossRefGoogle Scholar
Cranmer, S. R. 2008, ApJ in press (arxiv0808.2250)Google Scholar
Esser, R., Fineschi, S., Dobrzycka, D., Habbal, S. R., Edgar, R. J., Raymond, J. C., & Kohl, J. L., 1999 ApJ, 510, L63CrossRefGoogle Scholar
Fisk, L. A., Schwadron, N. A., & Zurbuchen, T. H. J. Geophys. Res., 104, A4, 19765CrossRefGoogle Scholar
Fludra, A., Del Zanna, G., & Bromage, B. J. I., 1999 Spa. Sci. Rev., 87, 185CrossRefGoogle Scholar
Goldreich, P. & Sridhar, S., 1995 ApJ, 438, 763CrossRefGoogle Scholar
Goldstein, M. L., 1978, ApJ, 219, 700CrossRefGoogle Scholar
Grall, R. R., Coles, W. A., Klinglesmith, M. T., Breen, A. R., Williams, P. J. S., Markkanen, J., & Esser, R., 1996 Nature, 379, 429CrossRefGoogle Scholar
Güdel, M. 2004, ARA&A, 12, 71Google Scholar
Güdel, M. 2007, Living Rev. in Sol. Phys., 4, 3CrossRefGoogle Scholar
Habbal, S. R., Esser, R., Guhathakura, M., & Fisher, R. R., 1994 Gephys. Res. Lett., 22, 1465CrossRefGoogle Scholar
Hakamada, K. & Kojima, M. 1999, Sol. Phys., 187, 115CrossRefGoogle Scholar
Harper, G. M., Wood, B. E., Linsky, J. L., Bennett, P. D., Ayres, T. R., & Brown, A. 1995, ApJ, 452, 407CrossRefGoogle Scholar
Hartmann, L., Dupree, A. K., & Raymond, J. C. 1980, ApJ, 236, L143CrossRefGoogle Scholar
Heyvaerts, J. & Priest, E. R., 1983 A&A, 117, 220Google Scholar
Holweger, H., Gehlsen, M., & Ruland, F., 1978 A&A, 70, 537Google Scholar
Jacques, S. A. 1977, ApJ, 215, 942CrossRefGoogle Scholar
Judge, P. G. & Stencel, R. E. 1991, ApJ, 371, 357CrossRefGoogle Scholar
Kojima, M., Breen, A. R., Fujiki, K., Hayashi, K., Ohmi, T., & Tokumaru, M., 2004 J. Geophys. Res., 109, A04103Google Scholar
Kudoh, T. & Shibata, K., 1999 ApJ, 514, 493CrossRefGoogle Scholar
Lamers, H. J. G. L. M. & Cassinelli, J. P. (1999), ‘Introduction to Stellar Wind’, CambridgeCrossRefGoogle Scholar
Lamy, P., Quemerais, E., Liebaria, A., Bout, M., Howard, R., Schwenn, R., & Simnett, G., 1997 Fifth SOHO Worshop, The Corona and Solar Wind near Minimum Activity, ed Wilson, A. (ESA-SP 404; Noordwijk:ESA), 491Google Scholar
Landini, M. & Monsignori-Fossi, B. C., 1990 A&AS, 82, 229Google Scholar
Linsky, J. L. & Haisch, B. M., 1979 ApJ, 229. L27CrossRefGoogle Scholar
Moore, R. L., Suess, S. T., Musielak, Z. E., & An, A.-H., 1991 ApJ, 378, 347CrossRefGoogle Scholar
Nariyuki, Y. & Hada, T., 2006 Phys. Plasma, 13, 124501CrossRefGoogle Scholar
Ofman, L. 2004, J. Geophys. Res., 109, A07102Google Scholar
Ofman, L. & Davila, J. M. 1998, J. Geophys. Res., 103, 23677CrossRefGoogle Scholar
Oughton, S., Matthaeus, W. H., Dmitruk, P., Milano, L. J., Zank, G. P., & Mullan, D. J., 2001 ApJ 551, 565CrossRefGoogle Scholar
Renzini, A., Cacciari, C., Ulmschneider, P., & Schmitz, F., 1977 A&A, 61, 39Google Scholar
Schwadron, N. A. & McComas, D. J. 2003 ApJ, 599, 1395CrossRefGoogle Scholar
Stein, R. F., Georgobiani, D., Trampedach, R., Ludwig, H.-G., & Nortlund, Å., 2004, Sol. Phys., 220, 229CrossRefGoogle Scholar
Suzuki, T. K., 2004 MNRAS, 349, 1227CrossRefGoogle Scholar
Suzuki, T. K. 2006, ApJ, 640, L75CrossRefGoogle Scholar
Suzuki, T. K., 2007 ApJ, 659, 1592CrossRefGoogle Scholar
Suzuki, T. K. & Inutsuka, S., 2005 ApJ, 632, L49CrossRefGoogle Scholar
Suzuki, T. K. & Inutsuka, S., 2006 J. Geophys. Res., 111, A6, A06101Google Scholar
Terasawa, T., Hoshino, M., Sakai, J. I., & Hada, T., 1986, J. Geophys. Res., 91, 4171CrossRefGoogle Scholar
Teriaca, L., Poletto, G., Romoli, M., & Biesecker, D. A., 2003 ApJ, 588, 566CrossRefGoogle Scholar
Tsurutani, B. T. et al. , 2002 Geophys. Res. Lett., 29, 23-1Google Scholar
Wang, Y.-M. & Sheeley, N. R. Jr,: Solar wind speed and coronal flux-tube expansion, Astrophys. J., 355, 726–732, 1990CrossRefGoogle Scholar
Wang, Y.-M. & Sheeley, N. R. Jr: Why fast solar wind originates from slowly expanding coronal flux tubes, Astrophys. J. Lett., 372, L45 - L48, 1991CrossRefGoogle Scholar
Wilhelm, K., Marsch, E., Dwivedi, B. N., Hassler, D. M., Lemaire, P., Gabriel, A. H., & Huber, M. C. E., 1998 ApJ, 500, 1023CrossRefGoogle Scholar
Withbroe, G. L. & Noyes, R. W., 1977, ARAA, 15, 363CrossRefGoogle Scholar
Wood, B. E., Müller, H.-R., Zank, G. P., Linsky, J. L., & Redfield, S. 2005, ApJ, 628, L143CrossRefGoogle Scholar
Zangrilli, L., Poletto, G., Nicolosi, P., Noci, G., & Romoli, M., 2002 ApJ, 574, 477CrossRefGoogle Scholar