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\IBVShead{4268}{16 November 1995}

\centerline{\ft NEW OUTBURST OF V1118 Ori}
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\begintext

     Since 1983, when V1118 Ori became known as a new EXor  (Herbig, 
1990, refer to  this  species  as  EXors,  after  the  example  first 
recognized, EX Lupi or Subfuor, Parsamian and  Gasparian,  1987)  and 
entered into an active stage of fuor-like  outbursts,  two  outbursts 
have  been  observed.  As  of  now  we  have  information  concerning 
outbursts during the period  1983-84  (Chanal,  1983,  Parsamian  and 
Gasparian, 1987) and 1988-90, when another outburst of the  star  was 
observed (Parsamian et al., 1993). 

      Table  1  shows the  stellar  magnitudes  during minimum light 
(Parsamian et al., 1992).
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\centerline{Table 1}
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\begin{center}
\begin{tabular}{cccc}
\hline
U          &  B(pg)     &       V     &        R   \\
\hline
\\
$\geq$ 18.8 &  17.6-18.2 &  16.3-17.3  &     15.2-15.8 \\
\hline
\end{tabular}
\end{center} 
\vskip 4mm

     We report here the results of new observations taken over the 
region of the Orion association, and carried out at  Instituto  de 
Astrofisica,  Optica  y  Electronica  (INAOE,  Tonantzintla),   at  
Instituto  de  Astrofisica  de  Canarias  and  in  Sevilla \footnote{
Private telescope}. 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,  in 
Sevilla with 20cm Schmidt-Cassegrain telescope with  CCD  camera  and 
infrared observations were 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). 

A new outburst of the star was observed  in  V  beginning  in  
January 1993, when the V magnitude reached 14.7. According to further 
spectral observations of V1118 Ori taken 
with the 2.1\,m telescope at the  Guillermo  Haro  observatory  in  Cananea 
(Mexico), the star was already undergoing  an  outburst 
phase on 30 Nov. 1992   (E.P.). The spectrum was characteristic of an emission  line  star  (T 
Tau  type  ),  as  was  indeed  observed  during  the  1989  outburst 
(Gasparian et al., 1990). 
In Figure 1 the light curve of the star V1118 Ori is given.
 
 Brightness  fluctuations,  which  were  observed 
during the previous outburst, were also observed during  this  period. 
 The amplitude of 
the outburst in V  could  be  larger  than  2  mag,  given  that  our 
observations were performed subsequent to the period   of  maximum  outburst 
activity. In that case, the duration of the outburst  might be longer than 2.5 yrs. Errors in the measurements are $\pm  0.1$ mag.
\vfill \eject

\centerline{2}
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\centerline{\epsffile{4268-f1.ps}}
\centerline{Figure 1. The light curve of V1118 Ori}
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     Infrared magnitudes of the star during the  outburst:
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\begin{tabular}{cccc}
 Julian Date      &             J    &        H     &       K \\
2449426.9420 &  8.52$\pm$0.05  &  8.04$\pm$0.04 &   7.94$\pm$0.03 \\
\end{tabular}
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The authors are grateful to Dr. Mark Kidger for performing the infrared 
observations and to C. Escamilla for help with the observations  in 
INAOE.

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\beginauthors
 Jos\'e  Garc\'{\i}a GARC\'{I}A
 Amor, 10. 8$^0$A
 410006 Sevilla 
 Espa\~na
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\authorsrightcol
 Antonio MAMPASO
 Instituto de Astrofisica de Canarias
 38200-La Laguna, Tenerife
 Espa\~na
\vskip 2mm
 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
  
Chanal, M., 1983, {\it IAUC}, No.\,3763

Gasparian, K.G., Melkonian, A.S., Ohanian, G.B., Parsamian, E.S.,   
 1990, Flare Stars in Star Clusters, Associations and Solar 
 Vicinity, IAU Symposiun, No.\,137, ed. L.V. Mirzoyan et al., Byurakan, 253

Herbig G. H., 1990, Low Mass Star Formation and Pre-Main Sequence Objects, 
ed. Bo Reipurth, M\"unchen, 233
 
Parsamian, E.S. and Gasparian, K.G., 1987, {\it Astrofizika}, {\bf 27}, 447

Parsamian, E.S., Ibragimov, M.A.,  Ohanian,  G.B.  and  Gasparian, 
 K.G., 1992, {\it Sov. Astron. Letters}, {\bf 18}, 248 

Parsamian, E.S., Ibragimov, M.A.,  Ohanian,  G.B.  and  Gasparian, 
 K.G., 1993, {\it Astrofizika}, {\bf 36}, 23

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