[vsnet 860] Mira-type stars: Multiharmonic analysis of the AAVSO v.38

["Prof. Ivan ANDRONOV" <ila@auriga.ta3.sk>]

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{\Large\bf MULTIHARMONIC ANALYSIS OF MIRA--TYPE STARS}
\footnote{IAU Symposium 180 "Planetary Nebulae"  Poster I-8}\\[1mm]
L.S. Kudashkina, I.L. Andronov\\[1mm]
Department of Astronomy, Odessa State University,
T.G.Shevchenko Park, Odessa 270014 Ukraine\\[2mm]
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{\bf Abstract}. The shapes of light curves of Mira-type variable stars
are analyzed by using the multi--harmonic fit (Andronov 1994). The light
curves of 63 stars best covered by the AAVSO observations and published
by Mattei (1978) were used. Some correlations between the
characteristics of the mean light curves were found.\\[2mm]

The following parameters were analyzed: the number of harmonics $m$ of a
statistically significant amplitude $r_j$ of the $j^{th}$ harmonic,
their phases $\phi_j$ in respect to the maximum, the period $P,$
asymmetry $f,$ amplitude $\Delta m,$ the maximal slope of the incline
$m_i=dm/dt,$ $t_i=m_i^{-1},$ its ratio to that obtained for a pure
sinusoid of the same period and amplitude $m_{is}=m_iP/(2\pi\Delta m),$
similar parameters for decline $t_d,$ $m_d,$ $m_{ds},$ ratio of the
amplitudes $r_j/r_1$ and phase differences $\phi_j-\phi_1$ and some
combinations of them.

The correlation table $25\times25$ was computed for these parameters.
For 63 pairs the correlation coefficient $\rho$ exceeds $3\sigma.$ Some
of them are listed in the table below. However, some diagrams show
different clusters, e.g. at the $\Delta m\,|\,t_i$ diagram two sequences
are present which are crossing at the point $\Delta m\approx5^m,$
$t_i\approx16^d$.

One or two points come out of several diagrams. These are W And ($\Delta
m=11.08^m,$ $P=399.2^d$) and $\chi$ Cyg ($\Delta m=8.99^m,$
$P=421.5^d$), which have very large amplitudes. However, these stars
keep within total picture for other parameters. The star X Oph come out
of the diagram $P\,|\,t_i.$ The light curve of this star is symmetric,
the amplitude is very small 1.34$^m$; $t_i=78^d.$ There are other stars
located far from the "main sequence" at some diagrams.

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\noindent\begin{tabular}{ccc|ccc|ccc}
\hline
Pair&$\rho$&$\rho/\sigma_{\rho}$&
Pair&$\rho$&$\rho/\sigma_{\rho}$&
Pair&$\rho$&$\rho/\sigma_{\rho}$\\
\hline
$P\,|\, m   $&$0.67$&$6.9$&$f \,|\, m_{is}  $&$0.63$&$6.3 $&$m_i \,|\, \phi_1  $&$0.51$&$4.1$\\
$P\,|\, m_i $&$0.43$&$3.7$&$f \,|\, r_1    $&$0.53$&$4.8 $&$m_i \,|\, r_2    $&$0.54$&$4.4$\\
$P\,|\, t_i $&$0.39$&$3.3$&$f \,|\, \phi_1  $&$0.91$&$15.4$&$m_i \,|\, r_3    $&$0.66$&$4.7$\\
$P\,|\, m_{is}$&$0.50$&$4.4$&$f \,|\, \phi_2\!-\!\phi_1 $&$0.60$&$5.2 $&$t_i \,|\, r_1$&$0.67$&$7.0$\\
$P\,|\, m_d $&$0.68$&$7.1$&$f \,|\, \phi_3\!-\!\phi_1 $&$0.77$&$6.4 $&$t_i \,|\, \phi_1  $&$0.47$&$3.7$\\
$P\,|\, t_d $&$0.58$&$5.5$&$\Delta m \,|\, m_i $&$0.61$&$6.0 $&$t_i \,|\, r_2    $&$0.45$&$3.5$\\
$P\,|\, r_2  $&$0.41$&$3.1$&$\Delta m \,|\, t_i $&$0.60$&$5.6 $&$t_i \,|\, r_3    $&$0.45$&$2.8$\\
$P\,|\, r_2/r_1$&$0.40$&$3.0$&$\Delta m \,|\, r_1  $&$0.98$&$38.3$&$m_{is} \,|\, r_2   $&$0.68$&$6.4$\\
$m\,|\, \Delta m $&$0.38$&$3.2$&$\Delta m \,|\, \phi_1$&$0.49$&$3.8 $&$m_{is} \,|\, r_2/r_1 $&$0.61$&$5.3$\\
$m\,|\, m_{is}$&$0.72$&$8.1$&$\Delta m \,|\, r_2  $&$0.70$&$6.8 $&$m_d \,|\, r_3    $&$0.76$&$6.4$\\
$m\,|\, r_3/r_1$&$0.51$&$3.2$&$\Delta m \,|\, r_3  $&$0.79$&$7.0 $&$t_d \,|\, r_1    $&$0.57$&$5.3$\\
$f\,|\, \Delta m$&$0.50$&$4.4$&$m_i \,|\, r_1   $&$0.67$&$6.9 $&$\phi_1 \,|\, \phi_3\!-\!\phi_1$&$0.81$&$7.3$\\
\hline
\end{tabular}
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{\bf References}\\[2mm]
Andronov, I.L., 1994, Odessa Astron. Publ., 7, 49.\\
Mattei, J.A., 1978, AAVSO Rep., 38.
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