 |
Figure 1:
Atmospheric structures of BO Mic
reconstructed by Doppler imaging and related methods.
All maps show the same features for the given rotation phases.
Photospheric spot coverage is rendered as black, dark and light orange areas,
representing 100%, 67% and 33% spot coverage, respectively.
Equatorial arrows mark approximate longitudes of prominences observed in Ca K
and H .
The blue circle indicates the
chromospheric emission region of the flare.
Grid lines mark latitudes and longitudes in
steps. |
| Open with DEXTER | |
In the text
 |
Figure 2:
BO Mic's photospheric emission as measured by XMM-Newton's optical monitor (black)
and computed from our Doppler image
(blue).
The left and right sections of the black curve render the
first (lower phase scale) and second (upper scale)
observed semi-rotation, respectively.
The emission is integrated from 6000 to 6500 Å, i.e. centered
between Johnson-V and R.
The estimated
error is  0.003 mag. |
| Open with DEXTER | |
In the text
 |
Figure 3:
BO Mic's coronal and chromospheric emission.
Purple crosses show flux and  -errors of the soft X-ray emission (0.2-5.0 keV)
as registered by XMM-Newton's EPIC-pn detector.
The black and red curves give the
Ca K and H
equivalent width, respectively.
Arrows mark the phases of sub-observer passage for the prominences
shown in Figs. 1 and 5.
The horizontal lines "A-G'' indicate bin intervals for the data points
of Fig. 4.
Phase annotations are the same as in Fig. 2. |
| Open with DEXTER | |
In the text
 |
Figure 4:
Evolution of emission measure and temperature for the hot plasma component
during the flaring, with
errors as determind by the
X-ray spectral fit.
EM0.5 is used as a proxy for the plasma density.
The solid line shows a linear fit to points B-D, corresponding to the decay
of the first flare event. Further energy release is evidenced by the
deviation of points E-G from the decay path.
The time bins of points "A-G'' are given in Fig. 3. |
| Open with DEXTER | |
In the text
 |
Figure 5:
Evolution of the Ca K emission:
Ca K line core profiles, processed by unsharp masking
are rendered as a function of wavelength (units of  )
and rotation phase.
Absorption dips in the profile appear blue while
emission bumps are shown red.
Plusses indicate sine-fits according to Eq. (1). They are used to
localize absorbing prominences,
their longitudes are given to the right.
The fit to the flare-induced chromospheric emission is marked by diamonds.
See text for discussion. |
| Open with DEXTER | |
In the text
![\begin{figure}
{
\includegraphics[width=14cm,clip]{SpMic2006_6400_Maps_RM00dark05step03_LiproFits_phasannot.ps} }
\end{figure}](/articles/aa/full/2008/04/aa8838-07/img46.gif)
In the text