[vsnet-chat 3517] Re: EO Eri ( NSV1710 ) - A Mira Variable

["Peter F Williams" <pfwilliams@onaustralia.com.au>]

Hi Stan and vsnet chatters,

This paper on EO Eri is really a flow-on from the earlier one on NSV4189. 
EO Eri was actually the first star I suggested Eugene Brings photograph
amongst the red NSV stars.  I needed to work out its period for inclusion
in a Table of stars we had observed along with NSV4189, and the paper just
followed.

My interest in this one came directly from IACU5031 back in 1990 June when
attention was directed to it. My first observation was in November of that
year using a preliminary chart which Mati Morel prepared at my request. 
This chart later appeared as VSS RASNZ Chart 1054 and the first observation
by another VSS member was in 1993 February (Albert Jones - who else? :) ). 
The vsnet and AAVSO sites seem to have essentially no data on this star
(but perhaps I did not look hard enough??).  There appears to be a 7 year
gap between Wenzel's data and the commencement of ours.

I was certainly not knocking Wenzel - merely reporting what I found from
the observations and thereby drawing attention to the current behaviour in
case something dramatic had happened.  Perhaps the light curve has changed?
 I do not know if an earlier light curve has been published so can only go
on the text which appeared in the IBVS3504.  This would be interesting to
see if available.

Yes, 10 years is a short time but at least we now know someone has been
looking at a potentially interesting star and what to expect in coming
years.

Re V803 Cen in outburst, my observations earlier tonight (Friday Aug 04):

CENV803	20000804.4347	135	WPX
CENV803	20000804.4770	132	WPX

Regards,

Peter Williams

----------
From: Stan Walker <astroman@voyager.co.nz>
To: pfwilliams@onaustralia.com.au; vsnet-chat
<vsnet-chat@kusastro.kyoto-u.ac.jp>
Subject: [vsnet-chat 3516] Re: EO Eri ( NSV1710 ) - A Mira Variable
Date: Friday, August 04, 2000 7:00

Peter,

I've just seen this note buried amongst screeds of others. Don't knock
Wenzel too much. All of these Miras with periods of 400+ days seem to be
unstable insofar as the period and shape of the light curve goes. R Cen is
perhaps the most stable. But BH Crucis is sometimes a double humped Mira,
sometimes single humped, and sometimes has a bump on the ascent/descent
like
Cepheids around 10 days. All of this shows up in the pe measures although
not always clearly in the visual ones. So give it time - 10 years is a very
short baseline. I'd be interested in seeing what you've concluded - don't
the VSS measures go back before 1990?

Regards,
Stan

PS Thanks for the data on V803 Cen - it's now in outburst.

S

----- Original Message -----
From: Peter F Williams <pfwilliams@onaustralia.com.au>
To: vsnet-chat <vsnet-chat@kusastro.kyoto-u.ac.jp>
Sent: Monday, July 31, 2000 11:20 PM
Subject: [vsnet-chat 3512] EO Eri ( NSV1710 ) - A Mira Variable

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