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The influence of eclipses in the stellar radio emission

Published online by Cambridge University Press:  12 September 2017

Caius Lucius Selhorst  and
Adriana Valio
Caius Lucius Selhorst
Affiliation:
NAT - Núcleo de Astrofísica Teórica - Universidade Cruzeiro do SulSão Paulo, SP, Brazil email: caiuslucius@gmail.com IP&D - Universidade do Vale do Paraíba - UNIVAPSão José dos Campos, SP, Brazil
Adriana Valio
Affiliation:
CRAAM - Universidade Presbiteriana Mackenzie, São Paulo, SP, Brazil
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Abstract

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Here we simulate the shape of a planetary transit observed at radio wavelengths. The simulations use a light curve of the K4 star HAT-P-11 and its hot Jupiter companion as proxy. From the HAT-P-11 optical light curve, a prominent spot was identified (1.10 RP and 0.6 IC). On the radio regime, the limb brighting of 30% was simulated by a quadratic function, and the active region was assumed to have the same size of the optical spot. Considering that the planet size is 6.35% of the the stellar radius, for the quiet star regions the transit depth is smaller than 0.5%, however, this value can increase to ~2% when covering an active region with 5.0 times the quiet star brightness temperature.

Keywords

Eclipses - Stars: activity - Radio Continnum: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 305 - 307
Copyright
Copyright © International Astronomical Union 2017 

References

Alonso, R., Brown, T. M., & Torres, G., et al., 2004, ApJL, 613, L153 Google Scholar
Béky, B., Holman, M. J., Kipping, D. M., & Noyes, R. W., 2014, ApJ, 788, 1 CrossRefGoogle Scholar
Hallinan, G., Sirothia, S. K., Antonova, A., et al., 2013, ApJ, 762, 34 Google Scholar
Poppenhaeger, K., Schmitt, J. H. M. M., & Wolk, S. J., 2013, ApJ, 773, 62 Google Scholar
Selhorst, C. L., Barbosa, C. L., & Valio, A., 2013, ApJL, 777, L34 CrossRefGoogle Scholar
Selhorst, C. L., Silva, A. V. R., Costa, J. E. R., & Shibasaki, K., 2003, A&A, 401, 1143 Google Scholar
Selhorst, C. L., Silva-Valio, A. V. R., & Costa, J. E. R., 2008, A&A, 488, 1079 Google Scholar
Silva, A. V. R., 2003, ApJL, 585, L147 Google Scholar
Silva, A. V. R., Laganá, T. F., Gimenez Castro, C. G., et al., 2005, SoPh, 227, 265 Google Scholar
Silva-Valio, A., Lanza, A. F., Alonso, R., & Barge, P., 2010, A&A, 510, A25 Google Scholar