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Eyepiece Views: May, 2002
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THE AMERICAN ASSOCIATION OF VARIABLE STAR OBSERVERS
25 Birch Street, Cambridge, MA 02138 USA
Tel. 617-354-0484 Fax 617-354-0665
http://www.aavso.org
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E Y E P I E C E V I E W S
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May, 2002 Vol 2 No 3
Table of Contents
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1. Introduction
2a. Special Observing Requests by Janet A. Mattei: RXTE Campaign on
0006-12 WW Cet
2b. Special Observing Requests by Janet A. Mattei: 1813+49 Am Her to
be observed by FUSE satellite
3. Comments and Observing Requests on LPVs - Janet A. Mattei
4. Comments on CV's by Mike Simonsen
5. An Eyepiece View from Stamford Observatory - by Mike Simonsen SXN
6. Chart Updates
7. AAVSO Long-Term Light Curves
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1. ALOHA !
Warm weather is not the only thing arriving in the northern hemisphere.
The 91st Spring Meeting of the AAVSO will take place on the Big Island of
Hawaii the first week in July. We expect to welcome many observers from the
Pan Pacific region as well as from other parts of the world. Since colder
and longer nights are approaching in the southern hemisphere, we hope this
meeting will be a short opportunity to re-live warmer nights for our
observers down under.
Throughout the upcoming months there are several special observing
campaigns underway. You will find reminders about the RXTE campaign in this
issue and a new one we just received today. (See 2a and 2b Special Observing
Requests by Janet A. Mattei)
You will receive the next issue of EYEPIECE Views right after our spring
meeting. We hope to see many of our valuable observers in Hawaii and until
then, we wish you the best dark, clear skies.
Thanks and good observing!
Gamze Menali, AAVSO Technical Assistant (MGQ)
Aaron Price, AAVSO Technical Assistant (PAH)
Mike Simonsen, AAVSO Observer (SXN)
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2A. SPECIAL OBSERVING REQUESTS BY JAM: RXTE CAMPAIGN ON 0006-12 WW CET
Astronomer Dr. Darren Baskill of Leicester University, Leicester, UK,
will be observing the dwarf nova WW Ceti with the Rossi X-ray Timing
Explorer (RXTE) from May 10 through August 9, 2002 for a duration of 3,000
seconds each day. He has requested the assistance of AAVSO observers to
monitor WW Cet during his X-ray campaign so that the visual and X-ray data
may be correlated.
For more information consult AAVSO Alert Notice #295 at the URL below:
http://www.aavso.org/alerts/alert295/alert295text.stm
Observers are urged to monitor the variable closely, particularly during
intervals when RXTE is observing WW Cet. During such time, observations
should be made every 5 minutes. Observers should start observing WW Cet 15
minutes before and should continue 15 minutes after scheduled RXTE runs.
When RXTE is not actively observing the dwarf nova, observations should be
made every hour.
WW Cet charts are available through our web site at the following address:
http://www.aavso.org/charts/CET/WW_CET
Please use these charts to observe this variable, and report your
observations of 0006-12 WW Cet to AAVSO Headquarters. Please make sure
to indicate which comparison stars you used and report the time of
your observations to 4 decimals of the JD.
Good coverage from our observers is extremely important to the success
of this observing program. Please observe WW Cet as frequently as possible.
More information about this project will become available as time
progresses. Watch the AAVSO home page (http://www.aavso.org) for updates
and reminders!
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2B. SPECIAL OBSERVING REQUESTS BY JAM: 1813+49 AM HER TO BE OBSERVED
BY FUSE SATELLITE
NASA's Far Ultraviolet Spectroscopic Explorer (FUSE) satellite will
observe AM Her on May 11 and 12th in order to better understand the effects
of magnetic fields on the UV spectrum and to more accurately measure the
temperature and abundances of metals in the photosphere when the system is
in a low mass transfer rate (quiescent) state. The astronomer colleagues
Drs. Martin Barstow, Boris Gaensicke, and Knox Long would greatly
appreciate good optical coverage of this system, during and after the FUSE
observations. Please monitor AM Her closely.
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3. COMMENTS AND OBSERVING REQUESTS ON LPVs -- J. A, Mattei
Below are some comments on and requests for observations of long
period variables that are observable at this time. Observers are
urged to use AAVSO Bulletin 65, Predicted Maxima and Minima Dates for
Long Period Variables for 2002, to plan their observing, and also
particularly to see if more observations can be obtained for those
stars indicated in the Bulletin as needing more observations. One
caution: often the stars that need more observations do not have
adequate comparison star sequence i.e lacking faint comparison stars,
thus they are quite challenging to observe and so should be observed
only by experienced observers.
1911-04 UZ Hya 9.1-14.1
This long period variable has just passed minimum and needs observations as
it brightens slowly to maximum, predicted for around the end of August.
0918-68 RW Car <9.3-15.0>
This southern Mira variable is slowly fading to minimum, predicted for the
end of June. Our southern observers with large-aperture telescopes are
strongly urged to monitor this star so we may obtain positive observations
as it fades to minimum.
0925-51 Y Vel <9.5-13.8>
This southern Mira variable is in need of observations badly as it brightens
towards maximum, predicted for mid-June. There is a 'd' scale AAVSO standard
chart with a fairly good comparison star sequence for the brighter end of the
star's range.
0940-23 RR Hya <9.3-14.4>
Another southern long period variable in need of observations as it is rising
to maximum, predicted for the later part of July. There are 'b' and 'd' AAVSO
standard charts with a good sequence.
0949-53 Z Vel <9.0-14.3> Another southern Mira variable, presently
fading to minimum predicted for early June, that is in desperate need
of observations from our southern observers with large-aperture
telescopes. Please go for this star!
0955-63 RV Car <11.3-16.2>
Yet another southern Mira variable in need of observations at all phases,
particularly as it is fading to and is around minimum, predicted for mid-June.
There is an AAVSO 'd' scale standard chart. Unfortunately, it does not have
faint comparison star magnitudes, so we ask our southern observers to do the
best they can to observe this star while it is faint.
1010-58A Z Car <10.7-15.2>
Another southern variable that we bring to the attention of our southern
observers for more observations as the star brightens slowly to its maximum,
predicted for mid-September. There is an AAVSO 'd' scale chart that does not
have faint comparison star magnitudes, so we ask our observers to do the best
they can.
1032-70 RZ Car <10.0-15.4>
This southern variable has quite a lot of scatter in its light curve. The
scatter may be due to the use of comparison star sequences from different
sources. Another plea to our southern observers to monitor this star as it
slowly brightens to maximum, predicted for the beginning of June. The
comparison star sequence for the brighter end on the 'd' AAVSO chart is fairly
good.
1136+39 RU UMa 8.3-15.1
This northern Mira variable needs more observations as it brightens towards
its maximum, predicted for the end of June. There are 'b', 'd', and 'e' scale
AAVSO preliminary charts that have a fairly good comparison star sequence
towards the brighter end of the light curve.
1144-41 X Cen <8.0-13.4>
Yet another southern variable in urgent need of observations as the star
slowly brightens to maximum, predicted for the beginning of July. There is a
'd' scale AAVSO standard chart for this star that has a fairly good comparison
star sequence towards the brighter end.
1209-05 T Vir <9.6-14.2>
The maxima and minima levels and the amplitude of this Mira variable have
been slowly fading and declining since 1997. In particular, the last two
cycles have had decreasing amplitude. The amplitude of the last cycle, which
was not very well covered, was only three magnitudes, whereas in general the
mean amplitude of the star is almost 5 magnitudes. T Vir is slowly
brightening
to maximum, predicted for early August. There are 'b' and 'd' scale AAVSO
standard charts. Observers are strongly urged to monitor this star closely in
order to determine its behavior.
1233+66 RV Dra <9.2-13.7>
This circumpolar Mira variable has an interesting light curve with varying
maxima and, particularly, minima levels. The cycle before the current one
had a maximum that was 1.5 magnitudes fainter than the mean maximum
brightness.
This star is slowly fading to minimum, predicted for mid-June. Observers with
large-aperture telescopes are strongly urged to monitor this star while it is
faint so we may obtain a good record of its minimum brightness.
1302-12 RV Vir <10.8-14.9>
Another Mira variable with varying levels of maxima, minima, and amplitude.
We didn't have many observations during the last cycle because the star was
in its observing gap. The cycle before that was also not well monitored, but
appeared to have a small amplitude, much smaller than the previous cycle.
Observers are strongly urged to monitor this star closely during the current
cycle as it slowly brightens to maximum, predicted for mid-June.
1322-02 V Vir <8.9-14.3>
This long period variable has not been well monitored for the most recent
couple of cycles. Its predicted maximum is for early May. Observers are
strongly urged to keep a close eye on V Vir, particularly while it is still
bright and as it slowly fades to minimum. There are 'd' and 'e' standard
AAVSO
charts with a fairly good sequence.
1324-22 R Hya <4.5-9.5>
This is one of the very few long period variables that has had a drastic
period decrease in the last couple of centuries. It is the AAVSO Variable
Star of the Month for May 2002 (http://www.aavso.org/vstar/vsotm/), and I
bring it to the attention of our observers to learn more about this
fascinating (and very easy to observe) Mira variable. It is slowly
brightening to maximum, predicted for the end of July.
1331-55 RV Cen <7.7-10.3>
This fascinating southern Mira variable is a carbon star with an N spectrum,
and thus is very red. It has extremely varying maximum and minimum levels and
amplitude. The amplitude of the recent cycles has been very much decreased,
with the star varying between about 7.8 and 9.6. We bring RV Cen to the
attention of our southern observers to keep a close eye on it so its behavior
may be well monitored.
1232+73 T UMi <9.2-14.0> This circumpolar Mira variable has had a
drastic period decrease in recent decades that we wrote about in the
Journal of the AAVSO (Mattei and Foster, 1995, JAAVSO, Vol. 23, 106;
read it online via
http://www.aavso.org/journal/starindex.stm#ursaminor). From the
recent cycles, there is a hint that both and the amplitude may be
increasing. If this is the case, it is particularly interesting in
respect to the period evolution and the evolution of the star in
general. Please keep a very close eye so we may have complete coverage
of T UMi to determine its behavior.
1342-36 RT Cen <9.0-12.7>
Another very interesting southern Mira variable with varying maxima and,
particularly, minima levels, as well as varying amplitude and period. The
amplitude of the recent cycles has been quite decreased, varying only from
9.6 to 12. We bring it to the attention of our southern observers, and
request them please to keep a close eye on it so we may determine its
long-term behavior.
1343-27 W Hya 5.7 - 10.0
This star, with a good photoelectric sequence on a 'b' scale AAVSO
chart, needs observations at all phases. Currently, it is slowly
brightening to maximum, predicted for mid-August.
1353-04 SY Vir 9.0-15.0
The light curve of this Mira variable has a significant number of discrepant
observations. There is a good photoelectric sequence on 'b' and 'd' AAVSO
preliminary charts. Observers are urged to be particularly careful in making
estimates of this star, slowly brightening to maximum predicted for the end
of May.
1405-28 RU Hya <8.4-14.0>
Another long period variable with varying maxima and minima brightnesses.
The minimum in March 2001 was very faint, and the maximum that followed it was
also faint. This star needs more observations to determine its behavior.
Observers are strongly urged to monitor it using the standard 'd' scale AAVSO
chart.
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4. CVs and UNUSUAL OBJECTS FOR SPRING
By Mike Simonsen (SXN)
With the Big Dipper riding high in the north this time of year, now is a
good time to discuss some interesting targets in Ursa Major.
0803+62 SU UMa (UGSU) This is the prototypical dwarf nova of its class.
Normal outbursts have maxima around 13.0, but this dwarf nova also exhibits
superoutbursts that can last up to two weeks and are much brighter. Stars in
this class exhibit superhumps during superoutbursts, a small periodic
fluctuation of several tenths of a magnitude. The unique aspect of
superhumps is that the period of fluctuation is 2-3% longer than the orbital
period of the system. By observing superhumps, you can derive the orbital
period of the system.
(Please see CCD Views Special Issue: May 5, 2002 for the special observing
requests of the star.)
For a star that is fairly well covered by observers, this can be a difficult
field to navigate. The 14th magnitude comps on the charts are probably much
fainter then the chart indicates. This can be disconcerting when trying to
make positive estimates in the faint range.
0829+53 SW UMa (UGSU) Although outbursts are rare, this CV can get as bright
as 9.7 when it decides to show off! If you observe this UG in outburst
notify AAVSO immediately, and then go back to the telescope and observe it
some more! It may be a long time before you see it again.
0831+48 EI UMa (NL) This is another star targeted by XMM satellite in
the coming weeks. This nova-like variable does not exhibit large amplitude
fluctuations from my experience, but it does seem to be different every time
I observe it. Usually hovering around 14th magnitude, I have seen it as
bright as 13.7 on occasion.
0846+58 BZ UMa (UGSU:) This possible UGSU doesn't seem to have normal
outbursts and superoutburts. The last few outbursts have reached 11th
magnitude, and no intermediate outbursts have been observed. This one could
be ripe for another bright outburst soon. It will probably be a visual
observer that notifies the astronomical community when the next outburst
begins.
0940+52 ER UMa (UGSU(ER)) This one goes on the "hyper-active list". It is
more unusual to observe this star at minimum than in some state of activity.
The prototype of a sub-group of UGSU stars, this type of system has frequent
outbursts and superoutbursts and exhibits superhumps at all phases of
outburst, not just during superoutbursts.
0959+68 CH UMa (UGSS) The most recent outburst of this star reached 11.5. At
minimum it fluctuates around 14.8-15.0. It is therefore possible that a
visual observer, lucky enough to catch the very beginning of an outburst,
could track a major portion of a rise to maximum.
This is also one of my "star-party stars". While everyone is oohing and
aahing over M81 and M82, I nudge the scope south a bit and make an
observation of CH UMa.
1010+72 CI UMa (UGSU) Not too long ago I was able to scratch this off my
'never been seen list'. It rises to around 13.8 at maximum. It is the
northernmost star in a little kite shaped asterism formed by a triangle of
comp stars. Just a little further away from M82 than CH UMa, and to the
north.
A quick hop from here takes you to the field of DH and CP Dra, which have
the awesome spiral galaxy NGC3147 in the same field of view.
1014+53 KS UMa (UGSU) Formerly known as SBS1017+533. When I first started
observing this CV I assumed it was one of those obscure, rarely outbursting,
faint CVs because of its exotic name. I couldn't have been more wrong. Over
this past winter I have observed several outbursts of this system and a
superoutburst in the 12th magnitude range. There are excellent new charts
with a CCD(V) sequence for this active star that make it a pleasure to
observe.
1037+58 IY UMa (UGSU+E) A much anticipated outburst of this CV, formerly
known as TmzV85, occurred on May 7. Due to the fact it is an eclipsing UGSU,
this one is of particular interest to astronomers studying the orbital
periods of dwarf novae. Eclipses are quite dramatic, and can be followed
visually. It's easy to find, and a good sequence and charts make this a
worthwhile stop in your nightly CV monitoring program.
1051+50 CY UMa (UGSU) This UGSU can get as bright as 12th magnitude in
outburst, or a touch brighter. It's located in a fairly recognizable
asterism with several good comp stars around it. Be careful not to mistake
it for the 131 comp star, a careless mistake I have made before.
1058+38 MARK 421 (BLLAC) BL Lac objects are active galactic nuclei that have
rather featureless spectra but exhibit rapid fluctuations in brightness.
Current models explaining the characteristics of AGN all include a
supermassive black hole surrounded by an accretion disc and clouds of
ionized gases moving at high velocities.
The fact that amateurs can make valuable visual observations of these
objects is almost as amazing as the fact that we can see them at all.
Markarian 421 is believed to be 400 million light years away.
This one is easy to find because it resides very close to a 6th magnitude
star. This same star can make observing Markarian 421 a challenge when
faint.
1112+48 KV UMa (XT) Formerly called XTEJ1118+480, this is a black hole
binary system in our galaxy, that behaves much like a quasar. These objects
have come to be known as microquasars. They exhibit the same kinds of
behaviors as very distant quasars, so they are very interesting to
astronomers.
Amateur observations of these systems are important because visible light
flare-ups have preceded activity at other wavelengths.
The last optical outburst was in the 12th magnitude range and lasted for
months. No one knows when the next outburst may happen.
1147+49 BC UMa (UGSU) This is another infrequent burster. I recall one
superoutburst and one normal outburst in the past three years. It does get
into the 11th magnitude range at super-maximum, so it will be hard to miss.
Next issue, I will explain what all these bizarre names and prefixes stand
for. Like, XTEJ, Markarian, SBS, RXSJ, TmzV, etc.
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5. AN EYEPIECE VIEW FROM STAMFORD OBSERVATORY
By Mike Simonsen SXN
Not many large telescopes in permanent observatories actually have
eyepieces attached to the business end of the scope. Most have CCD cameras
or other instrument packages attached, and viewing is done remotely at a
computer monitor.
At Stamford Observatory the 22" Gregory Maksutov has a whole turret of
eyepieces for the observer to select from. For two nights in November last
year, I had the privilege of observing with the big scope at Stamford, the
old fashioned way, through the eyepiece.
I had been invited by Charles Scovil, the observatory director, to come
visit him and observe at Stamford. So on Sunday, after the AAVSO fall
meeting in Cambridge, I found myself tailgating Chaz and his other guest,
Marc Beismans, across the countryside from Boston to Stamford.
We arrived at the observatory around dusk. Chaz gave Marc and me a tour
of the facility and then marched us up the stairs to the dome.
I had seen pictures of the telescope before, but I wasn't prepared for
the sight of the 22" up close when the lights were flipped on. It's
massive! The solid tube, painted silver, adorned with a number of guide
scopes, finder scopes and the eyepiece turret, looks like a giant cannon
out of some Buck Rogers fantasy. I was also surprised at the thickness and
extreme curvature of the meniscus, and the relatively small size of the
secondary.
The control panel has digital setting circles, a joystick for telescope
control, controls for rotating the dome and a switch for pumping oil into
the bearing of the huge fork mount. The telescope makes a slow, rhythmic
squeaking sound when the drive is engaged. A sound I never did get
completely comfortable with.
In spite of hazy skies and a nearly full moon, we took turns observing at
the eyepiece of the 22. We observed a fading nova, V2275 Cyg, and RX Lyr,
an LPV Chaz and Marc were working on new charts for. This is an interesting
star if for no other reason than the ghostly smoke ring, M57, resides in
the same medium power field.
One of the things I had looked forward to was making positive
observations of some of my program CVs at minimum. Observations that are
usually difficult or impossible in my 10" scope. As luck would have it SS
Aur, U Gem, KT Per and TZ Per, four of my intended targets, all went into
outburst during my visit! Just as well, since sky conditions favored
brighter objects that first night.
Skies deteriorated quickly, so we closed up the dome and went to dinner,
hoping for a change in local conditions. It rained while we were eating and
never did improve that night, so we spent the rest of the morning in the
inner sanctum of chart making for the AAVSO, Charles' office on the second
floor of the observatory.
Monday evening looked very promising as I pulled up to the observatory.
The skies had begun to clear and I could almost smell the Canadian high
pressure that is my best friend back home in Michigan.
Charles and Marc were already there and had opened the dome and readied
the scope for another night of observing. Unfortunately, Charles had other
plans for the night and asked if I would mind observing alone, since he and
Marc were busy preparing the new charts for RX Lyr.
I tried not to giggle as I found myself saying, "No, I won't mind having
this huge telescope to myself all night!"
It happened to be my birthday, and I couldn't have dreamed of a better
gift. At least that was what I thought at the time.
After a couple hours of being blissfully absorbed in observing in
Andromeda and Perseus, I suddenly began having trouble seeing faint stars.
I thought maybe it was time to take a break or that the weather had taken a
turn when I looked out the dome slot and the sky appeared orange. Or was
that red?
It quickly dawned on me as I ran out on to the observation deck that Chaz
had ordered up one of the most dramatic auroral displays I had ever
witnessed in honor of my birthday! We all stood outside under the blazing
red, orange and green lights for a long time.
In spite of the moon and occasional auroral flare-ups later that night, I
was able to log several 16th magnitude observations. The faintest positive
observation was in one of my favorite fields in Auriga, ST Aur. I was able
to see it at or near minimum at 15.7. After making an estimate of RX And in
outburst I scanned over M31, quite a sight in a 22" scope.
At times it was necessary to re-align the digital circles on a bright
star. I was impressed by the different colors of these stars blazing in the
eyepiece of the 22" Mak. Betelgeuse, Aldeberan, Vega and Altair left
lasting impressions on my mind and dark adaptation!
Closing up for the night felt strangely familiar as I capped the end of
the scope, parked it in the home position, closed the dome slot and turned
off the power. Of course, the cap for my scope looks like a Frisbee,
whereas the cap for the 22" is more the size of a garbage can lid!
I slept with a smile on my face that morning.
I hope to return some time soon (around new moon) and do it all again.
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6. CHART UPDATES
New charts were issued for the following stars since March 1. For each
chart scale reversed charts are also available:
F, G - V4334 SGR (Sakurai's Object)
E - AK CNC
F - SN 2002BS
F - SN 2002BO
F - GK PER
B,D,E - Y MON (BI Mon + IY Mon also in the field)
Also, in March a set of 239 new charts were issued for faint objects,
mainly CV's using photometry from A. Henden and sequences selected by B.
Sumner.
Below is a list the objects for which we have new e and/or f-scale charts:
3C 232 3C 279 VIR
3C66A AND AP LIB
AX CAP AY LAC
BF ERI BV PUP
BX PUP BY CAM
CG CAM CG DRA
CI CAM CI GEM
CT HYA DW CNC
EG LAC ES AQL
EV AQR FBS 1719
FBS 1735 FG SER
FT CAM GW LIB
GY HYA HP LIB
HS VIR HT CAM
IR COM KS UMA
KV DRA KZ GEM
LS AND LY HYA
MM HYA NS PER
NY SER NSV 895
CG CMA DK CAS
PQ AQL PQ ORI
PR HER PT PER
PV PER PV PER
QR AND QW SER
RY SER TK5 LYR
TU CRT TU TRI
TX TRI TY PSA
UY PUP V1113 CYG
V1141 AQL V1316 CYG
V1454 CYG V2400 OPH
V336 PER V368 PEG
V378 PEG V381 LAC
V391 SCT V402 AND
V452 CAS V478 HER
V630 CAS V650 ORI
V699 OPH V823 CYG
VY SCL VZ PYX
W COM WY TRI
XZ ERI DO VUL
WZ CMA TY VUL
More information on this list is available at:
/observing/charts/hs.shtml
As always, all charts are available through our online chart search engine
at: /observing/charts/
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7. AAVSO LONG-TERM LIGHT CURVES
AAVSO long-term light curves on variable stars define the behavior
pattern of variable stars and provide basic sets of observations that may
be used to correlate spectroscopic, photometric, and polarimetric
multiwavelength data, and to match theoretical stellar models.
The AAVSO Monograph format enables us to present long-term variable star
behavior, with each monograph containing 20 or more years of
computer-generated light curves on one star. Each Supplement to a Monograph
continues the light curves of the same star, bringing them more up-to-date.
For more information on published AAVSO Monographs, please visit the
following page:
http://www.aavso.org/monograph/index.stm
Here is a list of the monographs and supplements we feature on our web
page:
AAVSO Monograph 1: SS Cygni 1896 - 1985
Supplement 1: 1986-1990
Supplement 2: 1991-1995
Supplement 3: 1996-2000 (Published, soon will be on the web too)
AAVSO Monograph 2: U Geminorum 1855 - 1985
Supplement 1: 1986 - 1990
Supplement 2: 1991 - 1995
AAVSO Monograph 3: R Scuti 1963 - 1985
Supplement 1: 1986 - 1990
Supplement 2: 1991 - 1995
Supplement 3: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 4: R Coronae Borealis 1843 - 1990
Supplement 1: 1991 - 1995
Supplement 2: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 5: RY Sagittarii 1892 - 1990
Supplement 1: 1991 - 1995
Supplement 2: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 6: Z Camelopardalis 1927 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 7: RS Ophiuchi 1890 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 8: AH Herculis 1963 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 9: RX Andromedae 1963 - 1995
Supplement 1: 1996-2000 (Published, soon will be on the web too)
AAVSO Monograph 10: AM Herculis 1977 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 11: PU Vulpeculae 1979 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
AAVSO Monograph 12: TT Arietis 1974 - 1995
AAVSO Monograph 13: GK Persei 1901 - 1902 and 1963 - 1995
Supplement 1: 1996 - 2000 (Published, soon will be on the web too)
We are preparing more monographs for publication. Stay tuned
for updates and announcements on our web page.
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EYEPIECE Views is published bimonthly and when circumstances warrant
via e-mail. An archive is available at http://www.aavso.org/eyepieceviews/ .
Please send comments and suggestions to gamze@aavso.org.
To receive EYEPIECE Views via e-mail send a message to
majordomo@aavso.org with "subscribe eyepieceviews" in the body of the
e-mail. To unsubscribe, place "unsubscribe eyepieceviews" in the e-mail.
The AAVSO has many free online publications including "CCD
Views", a similar newsletter intended for ccd observers. To learn
more and subscribe visit: http://www.aavso.org/mailinglists.stm
Good observing!
Gamze Menali,AAVSO Technical Assistant (MGQ)
Aaron Price, AAVSO Technical Assistant (PAH)
Mike Simonsen, AAVSO Observer (SXN)
Copyright 2002, American Association of Variable Star Observers
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THE AMERICAN ASSOCIATION OF VARIABLE STAR OBSERVERS
25 Birch Street, Cambridge, MA 02138 USA
Tel. 617-354-0484 Fax 617-354-0665
http://www.aavso.org
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