==========================================================================
J/A+A/310/143 Variability of classical T Tauri stars (Fernandez+, 1996)
The following files can be converted to FITS (extension .fit .fit.Z .fgz)
tables
==========================================================================
drwxr-xr-x 13 cats archive 228 Jan 29 2012 [Up]
drwxr-xr-x 2 cats archive 187 Jan 12 2023 [TAR file]
-rw-r--r-- 1 cats archive 310 Sep 10 1996 .message
-r--r--r-- 1 cats archive 3287 Jun 8 1996 ReadMe
-r--r--r-- 1 cats archive 552 Feb 8 1996 tables.gz [Uncompressed]
Beginning of ReadMe :J/A+A/310/143 Variability of classical T Tauri stars (Fernandez+, 1996)
================================================================================
Variability of classical T Tauri stars. Its relation to the accretion process
Fernandez M., Eiroa C.
<Astron. Astrophys. 310, 143 (1996)>
=1996A&A...310..143F (SIMBAD/NED BibCode)
================================================================================
ADC_Keywords: Photometry, UBVRI
Keywords: stars: formation - stars: pre-main sequence - accretion disks
stars spots
Description:
We present the analysis of a UBV(RI)c photometric monitoring program
carried out from July 1988 to August 1992 on a sample of 13 classical
T Tauri stars and 2 suspected classical T Tauri stars. We detected
optical irregular variability with an amplitude larger than 0.1mag in
the V band in 8 stars. For 5 of them most of the variability can be
attributed to hot spots, for one, to cool spots and for two of them,
there is no clear mechanism; nevertheless, other phenomena must
explain the short term (hours - days) and long term (years)
variations superimposed. For some objects an anomalous behaviour at
the shorter wavelengths (U band) is detected. From the comparison
between the amplitude of the optical variability due to hot spots and
the equivalent width of the Halpha emission a correlation between them
is suggested. Assuming that the Halpha emission is related to the
accretion process, this correlation supports the idea that we are
observing the hot spots where the material from the accretion disks
falls onto the star.
For a description of the (RI)c photometric system, see e.g.
GCPD/54