Long-term evolution of FU Orionis objects at infrared wavelengths*
Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, 1525 Budapest, Hungary e-mail: firstname.lastname@example.org
2 Department of Astronomy, Eötvös Loránd University, PO Box 32, 1518 Budapest, Hungary
3 ESTEC/SCI-SAF, Postbus 299, 2200 AG Noordwijk, The Netherlands
Accepted: 26 July 2004
We investigate the brightness evolution of seven FU Orionis systems in the m wavelength range using data from the Infrared Space Observatory (ISO). The ISO measurements were supplemented by 2MASS and MSX observations performed in the same years as the ISO mission (1995-98). The spectral energy distributions (SEDs) based on these data points were compared with earlier ones derived from the IRAS photometry as well as from ground-based observations carried out around the epoch 1983. In three cases (Z CMa, Parsamian 21, V1331 Cyg) no difference between the two epochs was seen within the measurement uncertainties. V1057 Cyg, V1515 Cyg and V1735 Cyg have become fainter at near-infrared wavelengths while V346 Nor has become slightly brighter. V1057 Cyg exhibits a similar flux change in the mid-infrared. At m most of the sources remained constant; only V346 Nor seems to fade. Our data on the long-term evolution of V1057 Cyg agree with the model predictions of Kenyon & Hartmann ([CITE]) and Turner et al. ([CITE]) at near- and mid-infrared wavelengths, but disagree at m. We discuss if this observational result at far-infrared wavelengths could be understood in the framework of the existing models.
Key words: stars: pre-main sequence / stars: circumstellar matter / stars: individual: V1057 Cyg / infrared: stars
© ESO, 2004