FR Cnc revisited: photometry, polarimetry and spectroscopy



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Golovin, A. and Gálvez Ortiz, M. C. and Hernán Obispo, M. and Andreev, M. and Barnes, J. R. and Montes Gutiérrez, David and Pavlenko, E. and Pandey, J. C. and Martínez Arnaiz, R. and Medhi, B. J. and Parihar, P. S. and Henden, A. and Sergeev, A. and Zaitsev, S. V. and Karpov, N. (2012) FR Cnc revisited: photometry, polarimetry and spectroscopy. Monthly notices of the Royal Astronomical Society, 421 (1). pp. 132-148. ISSN 0035-8711

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This paper is part of a multiwavelength study aimed at using complementary photometric, polarimetric and spectroscopic data to achieve an understanding of the activity process in late-type stars. Here, we present the study of FR Cnc, a young, active and spotted star.
We performed analysis of All Sky Automated Survey 3 (ASAS-3) data for the years 2002–08 and amended the value of the rotational period to be 0.826518 d. The amplitude of photometric variations decreased abruptly in the year 2005, while the mean brightness remained the same, which was interpreted as a quick redistribution of spots. BVR_C and I_C broad-band photometric calibration was performed for 166 stars in FR Cnc vicinity.
The photometry at Terskol Observatory shows two brightening episodes, one of which occurred at the same phase as the flare of 2006 November 23. Polarimetric BVR observations indicate the probable presence of a supplementary source of polarization. We monitored FR Cnc spectroscopically during the years 2004–08. We concluded that the radial velocity changes cannot be explained by the binary nature of FR Cnc. We determined the spectral type of FR Cnc as K7V. Calculated galactic space-velocity components (U, V, W) indicate that FR Cnc belongs to the young disc population and might also belong to the IC 2391 moving group. Based on Li Iλ6707.8 measurement, we estimated the age of FR Cnc to be between 10 and 120 Myr. Doppler tomography was applied to create a starspot image of FR Cnc. We optimized the goodness of fit to the deconvolved profiles for axial inclination, equivalent width and v sin i, finding v sin  i=46.2 km s^−1 and i= 55°. We also generated a syntheticV-band light curve based on Doppler imaging that makes simultaneous use of spectroscopic and photometric data. This synthetic light curve displays the same morphology and amplitude as the observed one.
The starspot distribution of FR Cnc is also of interest since it is one of the latest spectral types to have been imaged. No polar spot was detected on FR Cnc.

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© 2012 The Authors.
© Monthly Notices of the Royal Astronomical Society.
© 2012 RAS.
MCG acknowledges the financial support from the European Commission in the form of Marie Curie Intra European Fellowship (PIEF-GA-2008-220679) and the partial support by the Spanish MICINN under the Consolider-Ingenio 2010 Programme grant CSD2006-00070: First Science with the GTC ( MCG and JRB have also received support from RoPACS during this research, a Marie Curie Initial Training Network funded by the European Commission's Seventh Framework Programme. This work was partly supported by the Spanish Ministerio de Ciencia e Innovación (MICINN), Programa Nacional de Astronomía y Astrofísica under grants AYA2008-00695 and AYA2008-06423-C03-03, and the Comunidad de Madrid under PRICIT project S2009/ESP-1496 (AstroMadrid). AG is thankful to Universidad Complutense de Madrid for hospitality and for all the efforts and the help during his visit to Spain in 2008 July and 2009 February.

Uncontrolled Keywords:Multiwavelength optical observations; Active binary-systems; Late-type stars; Main-sequence stars; Scale magnetic topologies; Band linear-polarization; Stellar kinematic groups; Radial-velocity jitter; RS canum-venaticorum; Einstein slew survey
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:37791
Deposited On:20 May 2016 15:31
Last Modified:10 Dec 2018 15:05

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