V367 - EB type with long 18.6d period
Fig.1. #364 V367 CYG measurements in 1998-1999. Data overlapped as
superposition with period 18.59773 days.
Couple humps near main minimum observable.
Smooth white curve is 13th moving average.
("Movpoints 8" refer to calculation of sigma not visual moving average
curve. And month color codes are switched off here).
Fig.1. #364 V367 CYG measurements in 1998-1999. Data overlapped as
superposition with period 18.59773 days.
Couple humps near main minimum obsersvable.
Smooth white curve is now (about, I remember) 7th moving average.
Now you can see extra variation. I'm not sure if its real or
just artifact due to daily observations syncro with 18+3/5 period.
Fig.1. #144 V1031 ORI measurements in 1/1999-3/2000. Data overlapped as
superposition with period 3.4057 days.
Only 4 previous measurements are known.Last time perhaps in 1991 by
Hipparcos satellite. This by-passing has amazed me!
This is bright +6..+6.5 star for binoculars just under Kappa Orion !
Perhaps one reason is that it is out of ephemeris. Eclipsing
happen now about 8 hours earlier than predicted
(Look BBSAG Bulletin to appear for exact timing of minima)
Beta Lyrae
Data values (julian) ASCII-file
Fig.1. #184 BETA Lyrae measurements in 1996 - 1998. Data overlapped
with period of 12.937 days.
Look at strange hump in middle of minima.
Look also the unsymmetricity the curve.
(Smooth upper curve is moving average of lower observations.)
Now as Computer screen pictures:
Beta Lyrae observed light curve in 1996-1998
NEW ! Beta Lyrae light curve in Nov 1998-Sep 1999.
Some differences observable around main minimum but more points needed
to confirm.
Period seems to have lengthened somebit from 12.937 d to 12.9407 d
(rough estimation).
This is expected because fast lengthening of period from 12.89 d->to 12.94d has been observed since last century.
RZ Cassiopeiae - minima curves
Data values (julian) ASCII-file
Fig.1. RZ Cassiopeiae has quite sharp minimum at 1.1952 days period.
Fig.2. Enlarged picture of minimum. About 18 minimum observations
1997-1998 overlapped.
In moving average curve there seems to be flat bottom that
lasts about 20 minutes.
Fig.3. RZ Cassiopeiae at minimum in 3 May 1997.
Red dots are middle points. Minimum is average of
those middle points. Here Minimum at 00:14,0+-6min
Local Geocentric time or
50571.423 JD Heliocentric time.
(some RZ-curves taken away , these pages are already heavy!)
Fig.3. RZ Cassiopeiae at minimum in 5 Apr 1998
at 01:42,1 +-2min Local Geocentric time or
50908.4853+-1.4E-3 JD Heliocentric time.
You can see asymmetricity of those curves. They are not all measurement
errors. Recently astronomers have found that RZ Cas is delta Scutii
type variable. They are variables with very short periods 0.05..0.20 days.
Here is one scientific reference I found:
-----------------------------------------------------------
581 Detection of the Scuti Oscillation in RZ Cassiopeiae
Osamu OHSHIMA, Shin-ya NARUSAWA, Hidehiko AKAZAWA, Mitsugu FUJII,
Tetsuya KAWABATA, Nobuo OHKURA
15 April 1998
( http://www.konkoly.hu/pub/ibvs/4501/4501cont.txt)
-----------------------------------------------------------
Recent about 14 ecplipsings got from Dec 22 1999 whit periodogram plot.
There seem to be flat bottom of 30-45 minutes
Remark that sigma, standard deviation of my visual observations
from moving average of phase plot is only 0.083 mag !
Fig.1. Delta Cep is prototype of cepheids, pulsating stars that
are used as standard candles when astronomers measures distances to
other galaxies. Upper Curve is #9/#7 Sieved Average of Lower.
(It drops min and max from each Average moving window. Less sensitive to
errors.)
I've made #85 observations in 1997-1998.
My purpose was to measure accuracy of my visual measurements of magnitude.
But this curve of mine observations doesn't look like that smooth curve
showed on standard books of astronomy.
So I'm wondering. What's wrong ? Are the extra humps and pumps real ?
Has Delta Cep changed its pulsating?
It looks like that it is pulsating
also at extra overtone periods.. I'm bit confused.
I used Beta Cephei as my compare star and I got to know that it is
variable too, but its amplitude is only 0.04..0.1 mag and its period
is 0.1904881 days not over 1 day like those bumps suggest.
I've been told now that humps/pumps are maybe artifact. I've quite
few observations. More is needed.
Compare with SPA VSS's light curve of Delta Cep on their homepage:
http://www.u-net.com/ph/spa/sections/vs/vss1998/dcep97.jpg"
Data values (julian) ASCII-file
Fig.1. Algol has drops to minimium at 2.867315 days interval.
It is in fact triple stars. 3rd star orbits these two at 1.6 yrs
period.
Fig.2. Close look at minimum
Epoch of minimum is about 245115.368+-0.01
Data values (julian) ASCII-file
Fig.1. W UMA has been hard target to me but hundreds observations and
computer makes regular curves. Here You can note also strange
bumps around maxima. Upper curve is 7th moving average.
W UMA is ahead of Big Dipper in the sky.
Fig.2. Now Upper curve is 13th moving average.
Secondary minimum can clearly be distinguished though difference is only
0.05-0.10 mag.
Period is about 0.333631+-0.000005 days.
In descending part of phase plot curve there is larger restless scatter.
Once there was few hours deep bump.Real or erroenous measurement ?
Elliptic stars are hard to visual observer, but periodogram found
3.52 d period which is quite close real one
Strange that descending part of minimum is deeper and faster
than ascending part. Minimum is clearly unsymmetric.
It is known that U CEP often pullouts gas shells/rings around it causing
great differences in light curve
Here in light curve some "traits" are above moving average in bottom
Here you can see also marks of secondary minimum in middle of primaries
The Observer, who also made curves above and computer programs for those, is
Mr. Kari A. Tikkanen
OULU
FINLAND
EUROPE
email : ktikkane@mailREMOVETHISS.student.oulu.fi