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\IBVShead{4269}{16 November 1995}

\centerline{\ft NEW OUTBURST OF V1143 Ori}
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\begintext

     Since 1982 four outbursts in the EXor V1143 Ori were observed 
(Sugano, 1983, Natsv\-lishvili, 1984, Verdenet, 1985,  Parsamian  and 
Gasparian, 1987, Parsamian et al., 1991, 1992). 

      In Table  1  the  stellar  magnitudes  in  the minimum light 
are given (Parsamian et al., 1991).

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\centerline{Table 1}
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\begin{center}
\begin{tabular}{cccc}
\hline
 U        &   B(pg)     &        V       &    R \\
\hline
\\
17.6-18.6 &   17.5-18.2 &      16.3-17.1 &    15.0-16.0\\
\hline
\end{tabular}
\end{center}
\vskip 3mm

     We report here  the  results  of  new  observations  of  an 
outburst during 1993-95. The observations (in V) were carried out at 
Instituto de Astrofisica, Optica y Electronica (INAOE,  Tonantzintla) 
with the 26$^{\prime\prime}$ Schmidt telescope on Kodak 103aD plates  when 
the star 
was already  its maximum light. Infrared  observation  was  performed 
during service time at the 1.5m Carlos S\'anchez  Telescope  (Tenerife, 
Spain). A two mirror focal plane chopper was used  and  a  liquid  N2 
cool InSb detector, together with standard J, H and K filters. A  set 
of standard stars was used for atmospheric extinction correction  and 
flux calibration (Arribas and Martinez, 1987). 

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\centerline{Figure 1. The light curve of V1143 Ori.}
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\centerline{2}
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     In Figure 1 the light curve of V1143 Ori is given.  
The first two observations were made on 15 Jan. 1993 without filter, when 
the star's  visual magnitude already was 13.5.   The 
amplitude in V could  be  larger  than  3  mag.  According  to  further 
spectral observations of V1143 Ori taken 
with the 2.1\,m telescope at the  Guillermo  Haro  observatory  in  Cananea 
(Mexico), the star was in its minimum light or very near 
to it on 27 Nov. 1992 (E.P.). The spectrum of the star was typical of an M type,
with Balmer emission lines and TiO bands, as it was observed earlier, at minimum
during the ``active'' stage (Peimbert et al.,  1991).  Therefore,  the 
star  undergoes  an  outburst  phase  after   21 Nov. 1992.   Our   first 
observations were made on 15 Jan. 1993, therefore the interval of  increase 
to the maximum was less than  two  months  if  we  suppose  that  the 
increase of brightness began in  December  1992.  In  the  first  two 
outbursts the duration of increase was about three months (Parsamian et 
al., 1991).  Our observations show that until  16 March 1993  the  star 
was in outburst, then there are not observations till 10 Nov., when 
star already was in its  minimum light.


Infrared magnitudes of the star after outburst :
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\begin{tabular}{cccc}
 Julian  Date        &          J      &       H      &       K \\
 
2449426.9191 & 12.51$\pm$0.17 &   11.79$\pm$0.12 &   11.41$\pm$0.12\\
\end{tabular}

\vskip .4cm

The authors are grateful to Dr. Mark Kidger for  performing the infrared 
observations and to C. Escamilla for help with the observations.



\vskip 1cm
\beginauthors
 Antonio MAMPASO
 Instituto de Astrofisica
 de Canarias 38200-La Laguna
 Tenerife,  Espa\~na 
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\authorsrightcol
 Elma S. PARSAMIAN 
 Byurakan Astrophysical Observatory 
 Armenia
 Instituto de Astronomia, UNAM
 M\'exico
\endauthors

\references

Arribas S. and Martinez Roger, 1987, {\it A\&AS}, {\bf 70}, 303  

Natsvlishvili, R.Sh., 1984, {\it IBVS}, No.\,2565

Parsamian E.S. and Gasparian L.G., 1987, {\it Astrofizika}, {\bf 27}, 447

Parsamian  E.S., Gasparian L.G., Ohanian G.B. and Chavira E.,
 1991,  {\it Astrofizika}, {\bf 34}, 175

Parsamian Elma S., Gasparian L.G. and Ohanian  Greta  B.,  1992, 
{\it Astron. and Astrophys. Transactions}, {\bf 2}, 209

Peimbert M., Parsamian  E.S.,  Gasparian  K.G.,  Melkonian  A.S. 
 and Ohanian G.B., 1991, {\it Astrofizika}, {\bf 35}, 181 

Sugano I., 1983, {\it IAUC}, No.\,3763

Verdenet M., 1985, {\it IAUC}, No.\,4035

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