Table 8
Dust shell properties determined from modelling of the reconstructed SEDs (Fig. 5) with the DUSTY numerical code.
| ISO/SWS number | 54 601 206 | 73 402 079 | Average |
| Date | 1997/05/15 | 1997/11/19 | |
| JD | 2 450 584 | 2 450 772 | |
|
|
|||
| φa | 0.56 (min.) | 0.04 (max.) | |
| TMira (K)b | 2100 | 2600 | 2350 |
| Tdust (K) |
|
|
|
| amax (μm) |
|
|
|
| τ V |
|
|
|
| A K |
|
|
|
| r1/rc |
|
|
|
| Ṁ (10-6M⊙/yr) |
|
|
|
| ve (km s-1) |
|
|
|
| Fbol (10-12 W/m2) | 21.8 | 40.9 | 31.35 |
| L (L⊙) | 5100 | 9600 | 7350c |
Notes. JD – Julian day of the observation; φ – phase of the pulsation cycle (φ = 0 for maximum brightness, φ = 0.5 for minimum brightness); TMira – temperature of the Mira component; Tdust – dust temperature on the inner boundary of the dust shell (dust sublimation temperature); amax – maximum dust grain diameter; τV – optical depth; AK – extinction at K; r1/rc – radius of the shell inner boundary (dust sublimation radius) r1 expressed in units of the stellar radius rc; Ṁ – mass loss rate assuming radiatively driven winds; ve – terminal escape velocity of the stellar wind; Fbol – bolometric flux; L – luminosity.
Phases φ = 0.56 and φ = 0.04 are considered to be close enough to the values of 0.5 and 0.0 to be declared as phases of the minimum and maximum brightness.
Minimum, maximum, and average stellar temperatures of the Mira component as determined in Sect. 3.2.
Average luminosity of the Mira component is not derived from our SED modelling but is determined from the period-luminosity relation of Whitelock et al. (1994).
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