Bibcode
Kóspál, Á.; Ábrahám, P.; Prusti, T.; Siebenmorgen, R.; Acosta-Pulido, J.; Moór, A.
Referencia bibliográfica
Astrophysics of Variable Stars, Pecs, Hungary, 5-10 September 2005, Sterken, C. and Aerts, C. (eds). ASP Conference Series, Vol. 349, p. 269. San Francisco: Astronomical Society of the Pacific, 2006.
Advertised on:
4
2006
Número de citas
3
Número de citas referidas
3
Descripción
OO Ser is a deeply embedded young star which brightened by 5 mag between
1994 and 1995, and gradually faded afterwards. In many respects its
eruption resembled the well-known FU Orionis-type (FUor) outbursts.
Since very few such events have ever been documented at infrared
wavelengths, we monitored OO Ser with the Infrared Space Observatory in
the 3.6-100 mum wavelength range, starting already 4 months after peak
brightness and covering a period of 20 months. Eight years later, in
2004 we again observed OO Ser at 2.2 and 12 mum from the ground. The
collected data provide a very unique opportunity to study the eruption
of a young star at infrared wavelengths. In this contribution we
present part of the data set, namely the 2.2 and 12 mum observations,
from which one can reach the following conclusions: (1) the star had
already returned to its pre-outburst phase by 2004, thus the timescale
of its outburst was significantly shorter than that of classical FUors;
(2) the fading at 12 mum was slightly faster than at 2.2-mum, somewhat
contradicting to model predictions; and (3) FU Ori-type outburst models
can only work for OO Ser if the viscosity parameter in the circumstellar
disk, alpha, is set to an order of magnitude higher value than in other
FUors.