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Optical and X-ray studies of chromospherically active stars : FR Cancri, HD 95559 and LO Pegasi

By SpaceRef Editor
August 22, 2005
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Astrophysics, abstract

From: Jeewan C. Pandey [view email]
Date: Wed, 1 Jun 2005 08:36:56 GMT (667kb)

Optical and X-ray studies of chromospherically active stars : FR Cancri,
HD 95559 and LO Pegasi

J. C. Pandey (ARIES, Nainital),
K. P. Singh (TIFR, Mumbai),
R. Sagar (ARIES, Nainital)

Comments: 40 pages, 11 figures, 6 tables, Accepted for the publication in AJ

We present a multiwavelength study of three chromospherically active stars,
namely FR Cnc (= BD +16\degr 1753), HD 95559 and LO Peg (=BD +22\degr 4409),
including newly obtained optical photometry, low-resolution optical
spectroscopy for FR Cnc, as well as archival IR and X-ray observations. The BVR
photometry carried out during the years 2001 – 2004 has found significant
photometric variability to be present in all three stars. For FR Cnc, a
photometric period $0.8267 \pm 0.0004 \rm {d}$ has been established. The strong
variation in the phase and amplitude of the FR Cnc light curves when folded on
this period implies the presence of evolving and migrating spots or i spot
groups on its surface. Two independent spots with migration periods of 0.97 and
0.93 years respectively are inferred. The photometry of HD 95559 suggests the
formation of a spot (group) during the interval of our observations. We infer
the existence of two independent spots or groups in the photosphere of LO Peg,
one of which has a migration period of 1.12 years. The optical spectroscopy of
FR Cnc carried out during 2002-2003, reveals the presence of strong and
variable Ca II H and K, H$_\beta$ and $H_{\alpha}$ emission features indicative
of high level of chromospheric activity. The value of 5.3 for the ratio of the
excess emission in $H_{\alpha}$ to $H_{\beta}$, $E_{H_{\alpha}}/E_{H_{\beta}}$,
suggests that the chromospheric emission may arise from an extended off-limb
region. We have also analyzed archival X-ray observations of HD 95559 and LO
Peg carried out by with the ROSAT observatory. The best fit models to their
X-ray spectra imply the presence of two coronal plasma components of differing
temperatures and with sub-solar metal abundances.

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