 |
Figure 1:
The dotted line denotes the OH 312.80 nm line calculated with the
MARCS model atmosphere using a solar oxygen abundance of
log
 ,
a microturbulence of
 km s-1 and 60% additional continuous opacity over
the standard value computed by the spectrum synthesis program. According to
Balachandran & Bell (1998) this fits the observations very well, and is
here used as a substitute to the observed profile in this crowded
spectral region. The dashed line corresponds
to a 3D line calculation with log
and without any
extra opacity. The solid line represents the 3D results with the same
abundance but with 50% extra continuous opacity, which yields
the same overall line strength as the here shown 1D profile. No micro- and macroturbulence
enter the 3D calculations but the Doppler shifts caused by the convective motions
make the line broader than the 1D case which is here shown without macroturbulence.
|
| Open with DEXTER | |
In the text
 |
Figure 2:
The dotted line denotes the Be I 313.10 nm line calculated with the
MARCS model atmosphere using a solar beryllium abundance of
log
 ,
a microturbulence of
km s-1 and 60% additional continuous opacity, which
is required to fit the observations according to
Balachandran & Bell (1998). The dashed line corresponds
to a 3D line calculation with log
and without any
extra opacity. The solid line represents the 3D results with the same
abundance but with 50% extra continuous opacity, which yields the same
line strength as the here shown 1D profile.
|
| Open with DEXTER | |
In the text