Hostname: page-component-8448b6f56d-xtgtn Total loading time: 0 Render date: 2024-04-25T05:17:25.114Z Has data issue: false hasContentIssue false
  • English
  • Français

Four years of starspot evolution on an active F-type ultra-fast rotator KIC 6791060

Published online by Cambridge University Press:  27 November 2018

Subhajeet Karmakar Open the ORCID record for Subhajeet Karmakar [Opens in a new window] ,
Jeewan C. Pandey ,
Igor S. Savanov ,
Ashish Raj ,
E. S. Dmitrienko ,
Yurij Pakhomov  and
D. K. Sahu
Subhajeet Karmakar
Affiliation:
Aryabhatta Research Institute of observational sciencES (ARIES), Manora Peak, Nainital 263002, India
Jeewan C. Pandey
Affiliation:
Aryabhatta Research Institute of observational sciencES (ARIES), Manora Peak, Nainital 263002, India
Igor S. Savanov
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, ul. Pyatniskaya 48, Moscow 119017, Russia
Ashish Raj
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
E. S. Dmitrienko
Affiliation:
Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow 119234, Russia
Yurij Pakhomov
Affiliation:
Institute of Astronomy, Russian Academy of Sciences, ul. Pyatniskaya 48, Moscow 119017, Russia
D. K. Sahu
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
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.

Using the data obtained from Kepler satellite, we have analyzed an F-type ultra-fast rotator KIC 6791060. We derive a rotational period of 0.34365±0.00004 d. Multiple periodicity with a period separation of ~0.00016 d was detected, which appears to be a result of the relative velocity between the multiple spot-groups in different stellar latitudes due to the surface differential rotation. Modeling of the surface inhomogeneities using the light curve of 3899 epochs shows the evidence of single active longitude region. The active longitude is found to drift along the longitude at a rate similar to the detected period separation of the F-type star. The surface coverage of cool spots is found to be in the range of ~0.07–0.44%. The low value of the spottedness can be interpreted probably due to the thinner convection zone on the F-type star.

Keywords

stars: individual (KIC 6791060)–stars: activity–stars: imaging - stars: spots–stars: rotation–stars: evolution–stars: atmospheres–stars: late-type–techniques: photometric–techniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 229 - 232
Copyright
Copyright © International Astronomical Union 2018 

Footnotes

†

speaker; email: subhajeet09@gmail.com

References

Balona, L. A., 2015, MNRAS, 447, 2714Google Scholar
Feigelson, E. D., Lawson, W. A., 2004, ApJ, 614, 267Google Scholar
Høg, E. et al., 2000, A&A, 355, L27Google Scholar
Karmakar, S. et al., 2016, MNRAS, 459, 3112Google Scholar
Kurucz, R. L., 1992, in IAU Symposium, Vol. 149, The Stellar Populations of Galaxies, Barbuy B., Renzini A., eds., p. 225Google Scholar
Luo, A.-L. et al., 2016, VizieR Online Data Catalog, 5149Google Scholar
Press, W. H., Rybicki, G. B., 1989, ApJ, 338, 277Google Scholar
Savanov, I. S. et al., 2016, Acta Astron., 66, 381Google Scholar
Savanov, I. S. & Strassmeier, K. G., 2008, Astronomische Nachrichten, 329, 364Google Scholar
Scargle, J. D., 1982, ApJ, 263, 835Google Scholar