Open AccessPhotometric, spectroscopic and polarimetric variability of the weak‐emission T Tauri star HD 288313
Author(s) -
Mekkaden M. V.,
Muneer S.,
Raveendran A. V.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.11841.x
Subject(s) - physics , astrophysics , t tauri star , brightness , starspot , amplitude , light curve , polarization (electrochemistry) , stellar rotation , rotation period , stars , astronomy , linear polarization , optics , laser , chemistry
Photometric observations over three seasons show HD 288313 to be a light variable with a 2.2636‐d period. The observed V amplitudes lie in the range of 0.06–0.15 mag. The star showed appreciable changes in the brightness at maximum and minimum of the light curve from season to season. The ( b − y ) colour did not show any significant variation during the photometric cycle. The light variation appears to be caused by the rotational modulation of stellar flux by cool starspots distributed asymmetrically across the stellar longitudes. The Hα line strength in HD 288313 varied drastically from completely filled‐in emission to almost full absorption, that is typical of a normal star of similar spectral type. The Hα equivalent width is found to show a clear rotational modulation only occasionally. Most of the time, chromospheric active regions are distributed well across the stellar longitudes, thereby suppressing obvious rotational modulations. Broad‐band linear polarization measurements show HD 288313 to be a short period, low‐amplitude polarization variable. The polarization variation is, apparently, rotationally modulated. Dust grain scattering in a non‐spherical circumstellar envelope of a star with inhomogeneities in the surface brightness distribution seems to be the mechanism operating in producing the observed polarization.