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The On/Off nature of star-planet interactions in the HD 179949 and υ And systems

Published online by Cambridge University Press:  01 October 2007

Evgenya Shkolnik ,
David A. Bohlender ,
Gordon A. H. Walker  and
Andrew Collier Cameron
Evgenya Shkolnik
Affiliation:
NASA Astrobiology Institute / University of Hawaii2680 Woodlawn Drive, Honolulu, HI 96822 email: shkolnik@ifa.hawaii.edu
David A. Bohlender
Affiliation:
Herzberg Institute for Astrophysics, National Research Council of Canada Victoria BC, Canada V9E 2E7
Gordon A. H. Walker
Affiliation:
1234 Hewlett Place, Victoria, BC, V8S 4P7
Andrew Collier Cameron
Affiliation:
School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, Scotland KY16 9SS
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Abstract

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Evidence suggesting an observable magnetic interaction between a star and its hot Jupiter (Porb < 7 days, a < 0.1 AU, Mpsini > 0.2 MJ) appears as a cyclic variation of stellar activity synchronized to the planet's orbit. HD 179949 has been observed almost every year since 2001. Synchronicity of the Ca II H & K emission with the orbit is clearly seen in four out of six epochs, while rotational modulation with Prot=7 days is apparent in the other two seasons. We observe a similar phenomenon on υ And, which displays rotational modulation (Prot=12 days) in September 2005, while in 2002 and 2003 variations appear to correlate with the planet's orbital period. This on/off nature of star-planet interaction (SPI) in the two systems is likely a function of the changing stellar magnetic field structure throughout its activity cycle. The tentative correlation between this activity in the 13 stars we have observed to date and the ratio of Mpsini to the planet's rotation period, a quantity proportional to the hot Jupiter's magnetic moment, first presented in Shkolnik et al. (2005) remains viable. This work furthers the characterization of SPI, improving its potential as a probe of extrasolar planetary magnetic fields.

Keywords

late-type starschromospheric activityplanetary systemsHD 179949υ And
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 151 - 158
Copyright
Copyright © International Astronomical Union 2008

References

Arge, C. N., Mullan, D. J. & Dolginov, A. Z., 1995, ApJ, 443, 795CrossRefGoogle Scholar
Bakos, G. Á., Knutson, H., Pont, F., Moutou, C., Charbonneau, D., Shporer, A., Bouchy, F., Everett, M., Hergenrother, C., Latham, D. W., Mayor, M., Mazeh, T., Noyes, R. W., Queloz, D., Pál, A., & Udry, S., 2006, ApJ, 650, 1160CrossRefGoogle Scholar
Cranmer, S. & Saar, S., 2007, arXiv:astro-ph/0702530v1Google Scholar
Cuntz, M., Saar, S.H., & Musielak, Z.E., 2000, ApJ, 533, L151CrossRefGoogle Scholar
Donati, J.-F., Semel, M., Carter, B. D., Rees, D. E., & Collier Cameron, A. 1997, MNRAS, 291, 658CrossRefGoogle Scholar
Donati, J.-F. 2007, MNRAS, in preparationGoogle Scholar
Griessmeier, J.-M.Stadelmann, A., Penz, T., Lammer, H., Selsis, F., Ribas, I., Guinan, E. F., Motschmann, U., Biernat, H. K., & Weiss, W. W., 2004, A&A, 425, 753Google Scholar
Gu, P.-G., Shkolnik, E., Li, S.-L., & Liu, X-W, 2005, AN, 326, 909Google Scholar
Ip, W.-H., Kopp, A., & Hu, J.-H., 2004, ApJ, 602, L53CrossRefGoogle Scholar
Khodachenko, M. L., Lammer, H., Lichtenegger, H. I. M., Langmayr, D., Erkaev, N. V., Griemeier, J.-M., Leitner, M., Penz, T., Biernat, H. K., Motschmann, U., & Rucker, H. O., 2007, P&SS, 55, 631Google Scholar
McIvor, T., Jardine, M., & Holzwarth, V., 2006, MNRAS, 367, 1CrossRefGoogle Scholar
Olson, P. & Christensen, U. R., 2006, E&PSL. 250, 561Google Scholar
Pont, F., Bouchy, F., Melo, C., Santos, N. C., Mayor, M., Queloz, D., & Udry, S., 2005, A&A, 438, 1123Google Scholar
Preusse, S., Kopp, A., Büchner, J., & Motschmann, U. 2006, A&A, 460, 317Google Scholar
Saar, S. H., Cuntz, M., & Shkolnik, E., 2004, in IAU Symp. 219, Stars as Suns: Activity, Evolution, Planets, eds. Dupree, A.K. and Benz, A.O., p.355CrossRefGoogle Scholar
Sánchez-Lavega, A., 2004, ApJ, 609, 87CrossRefGoogle Scholar
Shkolnik, E., Walker, G. A. H., & Bohlender, D. A., 2003, ApJ, 597, 1092CrossRefGoogle Scholar
Shkolnik, E., Walker, G. A. H., Bohlender, D. A., Gu, P.-G., & Kürster, M., 2005, ApJ, 622, 1075CrossRefGoogle Scholar
Shkolnik, E., Bohlender, D. A., Walker, G. A. H., & Collier Cameron, A., 2008, ApJ, 676, 628CrossRefGoogle Scholar
Stevens, I. R. 2005, MNRAS, 356, 1053CrossRefGoogle Scholar
Vidal-Madjar, A., Lecavelier des Étangs, A., Désert, J.-M., Ballester, G., Ferlet, R., Hébrard, G., & Mayor, M., 2003, Nature, 422, 143CrossRefGoogle Scholar
Vidal-Madjar, A., Désert, J.-M., Lecavelier des Etangs, A., Hébrard, G., Ballester, G. E., Ehrenreich, D., Ferlet, R., McConnell, J. C., Mayor, M., & Parkinson, C. D., 2004, ApJ, 604, L69CrossRefGoogle Scholar
Wolf, M. & Harmanec, P., 2004, IBVS, 5575, 1Google Scholar