SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 353, 583-597 (2000)

Previous Section Next Section Title Page Table of Contents

3. Emission from the present mass loss gas

The central emission, present in both lines, presumably arises from the envelope formed during the present mass loss epoch. We have determined the peak positions by fitting two-dimensional Gaussians to the data in the -27.5[FORMULA]2[FORMULA] range. The result is [FORMULA](2000) = 19h40m57[FORMULA]00, [FORMULA](2000) = 32o37´05[FORMULA]6 and [FORMULA](2000) = 19h40m57[FORMULA]00, [FORMULA](2000) = 32o37´05[FORMULA]9 for the J=[FORMULA] and J=[FORMULA] data, respectively. These positions agree, within the uncertainty of [FORMULA]0[FORMULA]5, well with each other and with the Hipparcos position of TT Cyg.

The central J=[FORMULA] and 2[FORMULA]1 brightness distributions are well fitted by circular Gaussians with deconvolved radii at half maxima of 1[FORMULA]1 (corresponding to 8[FORMULA]1015 cm at the adopted distance) and 0[FORMULA]8 (6[FORMULA]1015 cm) and peak brightnesses of 0.085 and 0.36 Jy beam-1, respectively. That is, the emission is at least partly resolved, and the smaller size in the J=[FORMULA] line is consistent with the higher energy requirements for exciting this line. The source fluxes, i.e., the source brightnesses integrated over the source, in the -27.5[FORMULA]2[FORMULA] interval are 0.8 and 5.2 Jy[FORMULA] in the J=[FORMULA] and J=[FORMULA] lines, respectively. This suggests, at least partly, optically thin emission, or, as expected, that the J=[FORMULA] line emission comes from a warmer region than the J=[FORMULA] line. The centre position spectra are shown in Fig. 3. The J=[FORMULA] spectrum suggests partly resolved optically thin emission, but the J=[FORMULA] spectrum indicates a higher optical depth. The systemic and gas expansion velocities are estimated to be -27.3[FORMULA] and 3.8[FORMULA], respectively. The source fluxes correspond to J=[FORMULA] and J=[FORMULA] line intensities of 0.03 and 0.12 K, respectively, in the IRAM 30 m telescope (in the [FORMULA]-scale and assuming Gaussian sources with the estimated sizes). This is consistent with the observed intensities, [FORMULA]0.05: and [FORMULA]0.1 K in the J=[FORMULA] and J=[FORMULA] lines, respectively (Olofsson et al. 1993).

[FIGURE] Fig. 3. CO(J=[FORMULA] and J=[FORMULA]) spectra obtained towards the position of TT Cyg (upper and lower panel, respectively). The feature at [FORMULA]-15[FORMULA] in the J=[FORMULA] spectrum is due to emission from the shell

We have estimated the present mass loss of TT Cyg using these data, and a radiative transfer model that determines the excitation of the CO molecules, in a circumstellar envelope that expands with constant velocity, using the Monte Carlo method. The energy balance equation for the circumstellar gas is solved self-consistently taking into account the CO line cooling (see Schöier, PhD thesis in preparation, for details). Adopting the (uncertain) Hipparcos distance of 510 pc, a luminosity of 2300[FORMULA] obtained from this distance and a derived apparent bolometric magnitude, and a gas expansion velocity of 4[FORMULA], and assuming a stellar temperature of 2700 K, and a CO number abundance with respect to H2, [FORMULA], of 10-3, we estimate a mass loss loss rate of [FORMULA]3[FORMULA]10[FORMULA]. The J=[FORMULA] emission is optically thin, but the J=[FORMULA] is, at least partly, optically thick. An outer radius of the CO envelope of 3[FORMULA]1016 cm was used in order to fit the observed radial brightness distributions. This is half of that obtained from the CO photodissociation model of Mamon et al. (1988) for the derived mass loss rate, but it must be regarded as within the uncertainties of this model when applied to low mass loss rate objects. Thus, the present mass loss of TT Cyg lies at the very low end of the mass loss rate distribution obtained by Olofsson et al. (1993) for a sample of ([FORMULA]100) optically bright carbon stars. The same applies to the gas expansion velocity, which is only about one third of the median gas expansion velocity of this sample.

Previous Section Next Section Title Page Table of Contents

© European Southern Observatory (ESO) 2000

Online publication: December 17, 1999
helpdesk.link@springer.de