THE 1994-1995 APHELIC APPARITION OF MARS

By: Daniel M. Troiani, Donald C. Parker, and Carlos E. Hernandez

ABSTRACT
The 1994-1995 apparition of Mars was aphelic, in that the planet's
apparent size reached only 13.85 arc seconds at opposition.  This made
the apparition the poorest (in apparent size) since 1980.  What this
apparition had going for it was Mars being high in the sky for northern
observers.  Furthermore, since the Martian north pole was tilted
earthward observers were able to watch the spring-summer regression of
the North Polar Cap and the concomitant increase in meteorological
activity. These phenomena formed the main thrust of the observational
programs of the Association of Lunar and Planetary Observers'
International Mars Patrol (IMP). Despite Mars unfavorable presentation,
improved instrumentation and observational techniques permitted quality
work to be done. For the hard-core Mars observer this apparition turned
out to be very exciting!


INTRODUCTION

The ALPO Mars Section received 2,364 observations from 66
observers in ten countries as part of the IMP    not bad for an aphelic
apparition that had Mars at over 100 million kilometers from Earth at
its closest approach.  Observations covered the period from Ls 261  (T.
Stryk) to 127 (H. Ishado), corresponding to Martian northern winter
through early summer (Fig. 1). Observers submitted 1297 drawings, 41
photographs, and 444 CCD images. In addition, we received over 400
measurements of the North Polar Cap (NPC) areocentric latitudes
obtained between 22  and 122  Ls from bifilar micrometer, CCD and video
red-light images. The NPC displayed numerous rifts and web-like
features. Some interesting relationships between Martian meteorology
and NPC behavior appear to be emerging, with numerous atmospheric
features such as limb clouds and hazes, topographic clouds, equatorial
band clouds and the Syrtis Blue Cloud increasing in prominence as
theNPC progressed.


CAN AMATEUR OBSERVATIONS STILL BE WORTHWHILE?

The answer is definitely YES!! The Mars Section has assisted a number
of professional planetary scientists during the present apparition by
responding to requests for ALPO Mars data. One request comes from Fred
Espenak of the NASA/Goddard Space Flight Center-Planetary Systems
Branch. He observed Mars in March of 1995 in the 10 micron
spectroscopic range with NASA's 3 meter telescope (IRTF) on Mauna Kea.
He was measuring the distribution of ozone in Mars' atmosphere using
the Goddard's IR Heterodyne Spectrometer. In his analysis of this data
he needed to know the transparency of the Martian atmosphere at the
time of his observation. Our data showed him what clouds or haze
activities were present before, during and after his observing run on
Mauna Kea.

Jim Bell and Jeff Moersch of NASA Planetary Astronomy program at
Cornell University hosted the Mars Telescopic Observations (MTO)
workshop which was sponsored by the Lunar and Planetary Institute. The
theme of this workshop was to explore the role that current and
continuing Earth-based observations play in increasing our
understanding of Mars. In addition, it brought togetherastronomers who
work at different wavelengths (both professionals and amateurs) and
don't often have the opportunity to share their ideas with one
another.  All of the Mars recorders were invited to present papers on
the work of our section. Don Parker gave a talk on the NPC regressions,
past and present and on the continuing IMP meteorological survey that
Jeff Beish and he have been conducting for many years. Dan Joyce
substituted for Dan Troiani, who was unable to attend, and presented
the ALPO Mars Section results from both the 1992-93 and the 1994-995
Martian apparitions, including numerous drawings, photographs, and
videos. All of the ALPO papers were well received and generated a great
deal of interest from the professional astronomers present. Abstracts
of the MTO Workshop papers have been published in a professional
abstract volume [Bell and Moersch 1995]. The work of the IMP (your
observations and hard work) has made an impact upon theprofessional
planetary scientists' community. Even in this day of space telescopes
and planned space missions, planetary scientists are still interested
in using amateur's data on Mars.  In fact, a significant portion of the
MTO workshop was devoted to planning ground-based support programs for
the upcoming space probes to Mars, and amateur visible light monitoring
was included in these plans. We will keep the readers and our observers
informed of these programs, including an E-mail alert network, as they
crystallize.

 
THE MARTIAN ARCTIC

The North Polar Hood (NPH) was conspicuous and visible from June, 1994,
through late October, 1994 (290 - 010  Ls), after which time the hood
became fragmented. This agrees well with Ebisawas finding that
polarization of the north polar region weakened around 9  Ls  [Ebisawa
1995]. Whitby, Warell, Niechoy, and Parker reportedthe NPC largely free
of the hood around 358  Ls, but at times high thin arctic clouds were
visible in blue light through November (25  Ls) by Will, Stryk, and
Schmude. There was an arctic cold front that pushed clouds south of the
NPC on the morning limb on Oct.  7, 1994 and again on November 3 (359
and 012  Ls respectively).  Lowells Band, the dark collar around the
NPC, first appeared around mid-October, as reported by Warell, and
persisted throughout the apparition.


The NPC Regression

The northern spring - early summer (22  - 112  Ls) regression of the
NPC was investigated by measuring the areocentric latitudes of the caps
edge from 220 bifilar micrometer measurements, 168 CCD images, and 36
video images (Fig. 2). In all cases, red filters were employed and the
east-west extent of the cap was measured and corrected for phase and
Ds.  Areocentric latitudes were computed using the formulae derived by
Beish [Dobbins, et al. 1986]. There were no statistically significant
differencesbetween the micrometer, CCD, or video determinations,
supporting preliminary data obtained during the 1992-1993 apparition.
This is good news, since micrometric determinations are tedious and
require considerable experience. We anticipate obtaining more NPC data
in future apparitions as the number of astronomers submitting CCD and
video images grows. It must be stressed, however, that observations
must be made through red filters, since even thin arctic hazes and
clouds will make the cap appear larger than it really is. Perhaps this
is one reason that cap sizes derived from drawings are systematically
larger. It must also be stressed that images submitted for NPC
measurements be carefully calibrated; that is, flat-fielded and dark
subtracted.

Initially the NPC was significantly smaller than normal but then
exhibited a delayed regression, similar to that observed in 1992-1993.
This retardation ceased at approximately 60  Ls, after which the caps
edge retreated rapidly to a latitude of 84.8  by 100  Ls. The tiny
summer cap remnant remained at approximately this size into early
northern summer, when the planets small apparent size precluded further
measurements. A slight transient regrowth of the cap was observed
between 65  and 72  Ls, corresponding to the aphelic chill. This
phenomenon, first described by Dr.  Clyde Tombaugh, is a temporary
reforming of arctic hazes near aphelion [Capen andCapen 1970]. Overall,
the 1994-1995 spring (24 -90  Ls) NPC was slightly (2.4 ) but
significantly smaller than those of the 1980 and 1982 (P< 0.05>0.01),
suggesting a continuation of the warming trend first observed in 1980
[Parker et al. 1983]. See Fig. 3. The 1984 North Cap exhibited unusual
retardations in regression between 60  and 110  Ls, a period coinciding
with the appearances of five localized dust storms [Beish and Parker
1990a]. Inclusion of this 1984 data would make the difference between
1995 and the 1980s even greater but could introduce spurious results.
Our 1995 data agrees nicely with that obtained by Iwasaki [1995] and
with preliminary Hubble Space Telescope (HST) values.


NPC Rifts

1. The Chasma Borealis and NPC Outliers.

Upon  emergence  from beneath the polar hood, the NPC displays  a
rather  smooth and uniform border.  Later, during the rapid thaw
period, the edge of the cap will appear uneven, with  numerous  small,
white, circular detachments along its border. By Martian summer, the
NPC retreat slows and three bright projections, termed outliers, appear
which detach from the cap as its edge  retreats past 80  N. latitude.
The white remnants may persist throughout northern summer and autumn,
although this has not been the case in recent apparitions. They are
named after the areas on Mars that they occupy. Their averaged
center-of-area areocentric longitude positions according to G. de
Mottini's 1941-52 IAU Mars map are as follows:  Ierne 137 , Lemuria
(Olympia) 200 , and Cecropia  297 . Lemuria is separated from the cap
by a dark conspicuous rift, called the Chasma Borealis. The positions
of the outliers vary form one apparition to the next, as can be seen in
Table 2.

The outliers and the Chasma Borealis were well observed during the
1994-1995 apparition. In January Hiroshi Ishadoh of the OAA Mars
Section (Japan) observed a shadowy streak in the NPC that Masatsugu
Minami of the OAA believes to be the early start of the Chasma
Borealis. Parkers CCD images from late December through mid February
(39 -60  Ls) reveal a concentric dark NPC rift, producing a lifesaver
effect on the cap that corresponded in orientation and position to the
Chasma Borealis. By 17 February the classical NPC peripheral
extensions, or outliers, called Lemuria and Ierne had become completely
detached from the cap. Lemuria persisted until at least late March (78
Ls) and was possibly detected as late as mid June, at 111 Ls. Ierne was
imaged well into May (97  Ls). The third classical outlier, Cecropia,
was not detected in its established location at 280 W, but a peripheral
deposit was noted near 350 W, close to the location of one of two
unnamed bright spots observed in 1982 and 1984 [Beish and Parker 1988].
This feature appeared on images taken between late February (64  Ls)
and early March (68  Ls).


2. The Rima Tenuis.

Giovanni Schiaparelli, while using a 9-inch refractor in 1888, noted
that  the north polar cap of Mars was divided in two parts by a dark
rift or fissure. This observation was later confirmed by Terby and
Perrotin. This rift, crossing the cap at approximate longitudes 135
and 325 , is called the Rima Tenuis and was observed many times from
1901 through 1918. Records from  the  British Astronomical Association
(BAA) reveal that the Rima Tenuis had been observed during 1933 and
again in 1950. Then it apparently disappeared for nearly 30 years. C.F.
Capen  searched unsuccessfully for the feature during  the 1960's,even
though  he employed telescopes of 16, 30 and 82 inches  in aperture.
The Rima also eluded the Viking orbiters during the 1970s. It was not
until late 1979  that  the Rima Tenuis reappeared, when D. Troiani
detected a dark notch at the south edge of  the NPC near 335
areocentric longitude. R. Robotham,  J. Dragesco,  J.  Beish and D.
Parker observed the Rima Tenuis within days of the first observations
of  the notch.  Later, on February 22, 1980, P. Moore and C.F. Capen
observed the complete Rima Tenuis while using the Lowell Observatory's
24-inch refractor [Capen, 1980]. The first photograph of this elusive
feature was obtained by A. MacFarlane on 22 February, 1980. Visibility
of the Rima Tenuis has increased since 1979.  While this may be due in
part to improved observational technology and greater awareness of the
feature, there is evidence that the Rima is intrinsically more
conspicuous, since observers are detecting it with instruments as small
as 6 inches in aperture.

1994-1995 is the fifth consecutive aphelic apparition during which this
feature was observed. It may have been detected as early as December 2
(26  Ls), when D. Niechoy of Germany observed an NPC rift corresponding
in position to the Rima. A number of reports were made between 20
December  and 2 January (34 -40  Ls), when S.R. Whitby, D. Troiani, D.
Parker, G.  Cameron, T. Stryk, and M. Schmidt (CCD images)
independently observed both notches and the rift itself. The notches in
the cap edge were located at 80 and 332  areocentric longitudes. The
next observations of this rift were reported on January 26 (51  Ls)  by
D. Joyce and D. Troiani using the Cernan Space Center (Triton College)
10" f/8 Newtonian. Troiani made a drawing showing the complete rift
with his 17.5 f/4.5 scope on January 27, when M.. Schmidt and C. Tobias
obtained CCD images at the Racine Observatory (Wisconsin) that clearly
show the Rima Tenuis notch in the south edge of the NPC. Over the next
two nights a number of midwestern observers, including D. Drake, Jesse
Carroll, Troiani, and Joyce, saw the Rima Tenuis with telescopes
ranging from 6 inches to 17.5 inches in aperture. On January 30th, M.
Schmidt obtained excellent CCD images showing the Rima Tenuis starting
at the small notch in the NPC at 332 W and cutting across  the cap.
Images from the HST reveal a faint streak in the cap at the right
longitude. After opposition D.L. Lehman obtained quality CCD images of
the Rima Tenuis on March 8 (69  Ls), and D. Parker imaged the feature
between May 9 and May 23 (96 -102  Ls).


METEOROLOGY

     Clouds, clouds and more clouds. That's what many observers
reported on Mars from January through March of '95. It is most
gratifying that most observers employed blue filters 
and thus were able to make quality observations of MarsÆ
atmosphere. This is a most important part of the ALPO Mars
program and one that provides a valuable source of data 
for professional astronomers. The following meteorological
results for the 1994-1995 apparition are qualitative only,
because several hundred blue-light observations are being 
measured and statistically analyzed by Beish and Parker for
inclusion in their ongoing study of Martian clouds [Beish and
Parker 1990b]. The study now includes over 24,000 drawings, 
photographs , and CCD images observed since 1965!

Limb Clouds and Hazes.

Limb brightenings, or limb arcs, are caused by scattered light from
dust and dry ice particles high in the Martian atmosphere. They are
often brilliant in blue light but can also be bright in all
wavelengths. They were reported throughout the apparition.
Morning clouds are bright, isolated patches of surface fog or frosty
ground near the morning limb (Mars' western edge as seen on Earth's
sky).  The fogs usually dissipate by mid-morning, while the frosts may
persist most of the Martian day, depending on the season.

Evening clouds give the same appearance as morning clouds but are
usually larger and more numerous than morning clouds.  They appear as
isolated bright patches over light desert regions in the late Martian
afternoon and grow in size as they rotate into the late evening.
Morning and evening limb clouds are distinguished from localized clouds
in that they do not rotate with the planet. Limb clouds tend to cluster
in the Martian tropical regions, whereas limb hazes/arcs usually extend
from pole to pole.
There was an abundance of morning and evening limb clouds throughout
most of the apparition, with some of these clouds being very bright at
times. They became particularly prominent during late northern spring,
around 75 Ls, and were still detected during early summer (100  Ls),
after which observations became difficult due to Mars small apparent
diameter. A bright evening limb cloud appears on Parkers tricolor CCD
images taken from March 28 through April 5 (77 -81  Ls). It was
interesting to watch the Acidalium and Nilokeras albedo features
disappear as they rotated under this cloud. A particularly unusual
morning cloud was imaged by Parker between May 9 and May 19 (96 -100
Ls). This cloud had a peanut shape and appeared quite blue in color.
Unlike a localized cloud, however, it did not rotate with the planet.


Localized Clouds, Topographic

Topographic  clouds are intense bright patches of limited extent that
occur seasonally over certain regions of  Mars.  Appearing white in
integrated light, these features are best viewed and photographed
through blue and blue-green filters. Occasionally they become more
prominent in green and even yellow-orange light, suggesting that they
may be combinations of water-ice and dust.

During the 1994-1995 apparition,  bright localized clouds became
prominent over Libya, Chryse, and Moab starting in late January, around
50  Ls. These clouds persisted and perhaps increased in size and
intensity well into northern summer. On February 18 (61  Ls), Beish
reported a localized cloud formation over Xanthe-Memnonia that he
called the "Capen wedge-cloud". By late February (64  Ls), discrete
clouds over Xanthe, Amazonis, Argyre I and Arabia-Moab had become very
conspicuous. On February 24th (63  Ls) Cameron saw a small bright spot
in the Solis Lacus region and clouds over Tharsis. Hellas had some
light fog in early March. On the 16th of March (72  Ls), there were a
few very small bright spots in Cebrenia and Utopia.

A specialized type of topographic cloud is the famous "Syrtis Blue
Cloud. This is a very localized cloud that had been traced for over a
century by C.F. Capen. It appears every Martian year around the
northern hemisphere summer solstice and persists through early summer.
This cloud circulates around the Libya Basin and then crosses over to
the Syrtis Major, where it changes the color of this albedo feature to
an intense blue. When Syrtis Major is viewed through a yellow filter it
turns a vivid green (yellow + blue = green). This cloud was first
observed in 1858 by Father Angelo Secchi, who called it the Blue
Scorpion. The cloud was next seen by J. N.  Lockyear in 1862 and again
in 1911 by members of the BAA. C. W.  Tombaugh and Capen observed the
cloud early in the Martian northern hemisphere summer during the
apparition of 1950. It was seen regularly in the 1960's and it was most
prominent in 1982.

D. Parker and J. Beish first reported the Syrtis Blue Cloud on Jan.
28th (51  Ls), and it was imaged on both morning and evening limbs
several times until April 20 (87  Ls). By May 23 (102  Ls) Libya still
displayed bright cloud cover with wispy tendrils extending over Syrtis
Major, but no coloration was detected. On May 30 (105  Ls), however,
Parker again noted the distinctive coloration. The next apparition will
again be favorable for viewing the Syrtis Blue Cloud. Since this is one
of the most spectacular features on Mars, we hope that observers avail
themselves of the opportunity.


Localized Clouds, Orographic

Orographic clouds, like those that form on Earth, are white discrete
clouds that are condensed from the moisture-laden air which is uplifted
over a mountain or volcano. They appear bright on Mars when viewed
through a blue (W#80A) or a violet (W#47) color filter.

Orographic clouds are discreet white clouds which develop as
moisture-laden air is uplifted over the peaks of the great volcanoes
located in the Martian tropics. They form when the Martian atmosphere
is high in water vapor especially in late spring or early summer of the
northern hemisphere, assembling as local noon approaches, when they are
best seen and photographed in blue and violet light.  They continue to
expand and brighten throughout  the  remainder  of the Martian day, and
by nightfall are best  discerned in the violet and ultraviolet regions
of the spectrum, suggesting that they are carried further aloft by
convection. The most spectacular orographic clouds occur over the
volcanoes of the Elysium Shield and the Tharsis Bulge. The latter
clouds sometimes appear  to coalesce to form the famed "W-cloud," first
reported by E.C. Slipher in 1954 [Slipher, 1962]. In 1971 the Mariner 9
spacecraft probe showed them to be water clouds near the large
volcanoes Olympus Mons (longitude 133  west, latitude 18  north),
Ascraeus Mons (104 W, 11 N), Pavonis Mons (112 W, 0 N), and Arsia Mons
(120 W, 9 S).

The Elysium cloud usually forms first, and that was the case in the
1994-95 apparition. Early in December (25  Ls) some brightening over
Elysium was reported, and by the months end (39 Ls) bright orographic
clouds were conspicuous over this volcanic shield. This is rather
normal for this region, as opposed to the 1992-93 apparition, during
which the Elysium cloud were very well formed by 28  Ls. Interestingly,
this appears to parallel the behavior of the NPC, which was
considerably smaller during the early northern spring of the 1992-93
apparition.

By mid-January (45  Ls), orographics were beginning to appear over the
Tharsis volcanoes and had become very conspicuous by mid-February (57
Ls). By February 19 (61  Ls) these clouds had coalesced to form the
W-Cloud. The Tharsis and Elysium orographics persisted and became
larger and brighter well into northern summer.


Polar Clouds, Hazes, and Hoods

During northern winter a thick mantle of cloud covers the Martian
arctic. Termed the North Polar Hood (NPH), this dull shroud generally
breaks up around the time of the vernal equinox, revealing the bright
pearly-white spring NPC. It is uncertain whether the NPC is formed from
the dissolving hood or was lying fully formed beneath the cloud layer
during northern winter. Near-infrared CCD images taken by Parker in
October, 1992, suggest the former state of affairs. These images, taken
during late northern winter (346 Ls), reveal named albedo features
beneath the NPH with no evidence of  the large spring cap which
appeared a few weeks later when the hood dissipated [Parker and Berry
1993].  Similar evidence was obtained from infrared observations from
Tokyo and from the University of Arizonas Catalina Telescope during the
period Ls=347 -354  [Ebisawa 1995b]. These investigators also imaged
the tiny permanent cap remnant beneath the hood, but found no trace of
the large surface cap spring surface cap that was to emerge only a few
weeks later.

During the 1994-95 apparition the NPH became variable and thin near the
vernal equinox. Both Whitby and Niechoy reported a large, dull hood
between 346-347  Ls; but, by 354  Ls (Sept. 28), Niechoy detected the
cap largely free of the hood. By 356-358 Ls, Whitby, Warell, and Parker
all observed the NPC clear of the NPH, bordered by the dark Lowells
Band. As the NPC retreated a number of observers spotted polar clouds,
especially on the morning side of the cap. These were reported on Dec.
1 (25  Ls), Feb. 3-6 (54 -55  Ls), and on March 8 (68  Ls). J. Beish
saw a light haze over the cap, possibly the start of the "aphelic
chill" on the 8th of February. Micrometer and CCD measurements revealed
a small but significant re-growth of the NPC around the time of
aphelion at 70  Ls.


Equatorial Cloud Bands (ECBÆs)
     
Perhaps the most interesting formations, however, are the equatorial
cloud bands  (ECBs). These are faint veils of wispy white clouds with
variable shapes and transparencies that extend across the Martian disk
within 20  of the equator. Residing at high altitudes and probably
composed of CO2 ice crystals, ECBs are best detected with dark blue
(W47 or W47B) filters.

Until recently, cloud bands were thought to be exceedingly rare
phenomena that were most likely to occur during the Martian northern
summer. However, systematic tri-color CCD imaging has uncovered
evidence that these wisps of cloud bands may be more frequent and may
occur in all Martian seasons. They were seen and imaged on numerous
occasions during the latter half of the 1992-93 apparition, being much
more prominent on CCD images than they were visually or
photographically. The ability of the CCD camera to  reveal subtle cloud
structures that are only 1-2% brighter than the background demonstrates
the power of electronic image processing. This did create a problem,
however, since it was uncertain whether the increase in ECBs during the
last apparition was real or merely due to better imaging techniques. It
was hoped  that the 1994-95 apparition would clarify the matter.

While ECBs were not usually specifically mentioned, they do appear on a
few blue-light drawings from a number of observers, including J. Beish,
C. Hernandez, D. Lehman, R. McKim, D.  Niechoy, , R. Schmude, T. Stryk,
and S. Whitby. Parkers CCD images again revealed them on several
occasions. These delicate features were most prevalent over Tharsis and
Amazonis during February and March. More information on ECB prevalence
awaits Beishs statistical analysis.

                                                                 
Dust Clouds

As expected, no major dust clouds were reported during this apparition;
but some very minor dust activity was observed in 1994. Stryk reported
a small, transient dust cloud over Argyre on 5 June (290  Ls) [Stryk,
1994]. On 5 October (358  Ls), it appears that there was dust in the
atmosphere over Chryse making it very bright at times in red light. In
addition, a small thin dust cloud in Xanthe was first observed by
Whitby on Nov. 3 (12  Ls). It was again seen on the 13th and 14th by
Ted Stryk, who reported some expansion on 14 November.  Analysis of
color filter observations suggests that there was some dust mixed in
the clouds over the Chryse region in March and a small dusty spot near
Solis Lacus. This admixture of dust with the prevalent water-ice
crystal clouds was verified by polarization measurements of Ebisawa
[1995], who detected dust present in the Chryse-Xanthe-Tharsis clouds
in late January (50  Ls). In addition, a bar-like dust cloud was seen
at the same time over Arcadia-Tempe, similar to the more conspicuous
one observed in 1982 around 122  Ls [McKim 1985]. Finally, Ebisawas
polarization data revealed dust mixed with the Elysium shield clouds in
mid-January (45  Ls). It should be noted, however, that the phase angle
(the Earth-Sun angle as seen from Mars) in mid-January was about 25 .
This is where the signs of polarization of both water-ice clouds and
dust clouds changes, making differentiation of cloud types nearly
impossible with this method.


SURFACE FEATURES

Region I: 250 W-010 W

Syrtis Major was dark throughout the apparition, exhibiting little
change from 1992- 93. It displayed average width, with a blunted
northern border.  Osiridis Promontorium, at the northeast border of
Syrtis Major was again prominent. Moeris Lacus, a short streak just
south of Osiridis, was again seen jutting into Libya. The
Thoth-Nepenthes canal, so conspicuous from 1954 to 1967, was not seen.
The Laocoontis-Nubis Lacus complex was also absent, as it has been
since 1982, although Seigel and Falsarella drew it faintly in March.
Nodus Alcyonius, northeast of Syrtis Major, was extremely dark and
elongated NE- SW. To the south, Hellas was bright with cloud or fog
both before and after opposition. In February, however, the floor of
this great basin was cloud-free, revealing the Hellas Cross, consisting
of Peneus, Alpheus, and Zea Lacus. West of Syrtis, Astaborae Sinus was
faintly seen by Cave, Schmude, and Stryk. To the north, Nilosyrtis and
Astusapes were faint to absent, although the former was reported after
opposition by Cameron, Haas, Teichert, and Niechoy. Boreosyrtis and
Umbra were dark. Moving westward, Protonilus, Ismenius Lacus, and
Deuteronilus were fairly well defined on both CCD images and drawings
from several observers, including Cameron, Fabian, Teichert, and
Troiani. Sabaeus Sinus was quite dark, and its eastern end, which had
been faded since 1990, resumed a more normal aspect, as reported by
Cave, Lehman, and Cameron. Despite the markedly positive De, Pandorae
Fretum was very well seen by most observers. It was very dark and
appears to have shifted southward from its usual position. In late
January (52  LS), however, Hernandez found only the eastern half of
Pandorae Fr. to be dark, with the western portion halftone. He also
detected the dark Vulcani Pelagus projecting from the eastern border of
Erythraeum M.

Classically, Syrtis Major broadens after northern summer solstice (90
Ls). No significant changes in its breadth were observed during this
apparition, agreeing with HST data [Lee et al. 1995]. This feature
demonstrated a high degree of variability during the 1970s and early
1980s, but it has remained fairly stable since the 1984 apparition.


Region II: 010 W-130 W

Margaritifer S. And Aurorae S. were well defined and of normal
intensity. Oxia Palus was prominent, as it has been for several years.
The delicate filament Cantabras, joining the western fork of Meridiani
S. With Oxia P. was seen on CCD images. At least four small, dark,
round features were seen in southern Chryse-Xanthe, including  Hydapsis
S., Iamunae S., Hydrae P.,  and Clytaemnestrae L. These were also
conspicuous in the 1992-1993 apparition. These features do not
correspond well with those on classical maps   it would appear that the
areography of the northern Chryse-Xanthe region is somewhat
inconsistent. To the west, in Candor, Juventae Fons was again prominent
and Ganges was broad but only dusky.  McKim reported that Lunae L., so
noticeable in the early 1980s, was again faint. Several observers found
western Nilokeras to be faint, while at its eastern end it appeared
double (Nilokeras I and II). Idaeus Fons and Achillus F. presented as
two dark nodules west of Niliacus. Prior to opposition, Niliacus was
darker than Acidalium M., but by March Crocker and Parker found that it
had lightened somewhat.

To the south, Agathadaemon, Melas L., and the Tithonius L.  Complex
were distinct. Solis Lacus was dark and elongated E-W. It has undergone
little change since the 1986 apparition. Gallinaria Silva was a
distinct dark dot west of Solis L. The canal Phasis, joining Gallinaria
to Aonius S. was not imaged or reported. This variable feature had
resumed prominence in May, 1984, darkened in 1986, but had faded during
the 1988 apparition. Then, in 1990, it became very prominent after the
early November dust storm [McKim 1992] but was barely perceptible
during the 1992-93 apparition. Acampsis, linking Solis L. to Gallinaria
was drawn and imaged by several observers, and the unnamed dark streak
running west from Gallinaria to near Gomer S. was seen and imaged in
December and in March. Near opposition it had faded but was still
barely perceptible on CCD images. This streak, running along the
northern borders of Sirenum M. and Cimmerium M. was first detected in
August, 1988 by S. OMeara and D. Parker and has been reported
sporadically since. Like Eumenides to the north, this feature seems to
be most prominent when Mars phase angle is greatest, and may thus be
linked to shadow effects.

In addition to the numerous clouds in Tharsis, some albedo feature
changes were reported. In early December (28  Ls) Teichert recorded a
darkening of Ascraeus Lacus.  Again, in late March (75  Ls) Siegel,
Warell, Teichert, Lehman found this feature dark, with Cameron and
McKim reporting Uranius to be broad and dark. Whitby also observed a
darkening in Ceraunius in late January (48  Ls).


Region III: 130 W-250 W

T. Cave and W. Haas reported Laestrygonum Sinus well-detached from
Cimmerium M. in March, when Haas also sighted the canals Cyclops and
Cerberus II. The dark patch in eastern Aetheria, prominent since 1977
and termed the Hyblaeus Extension by C. Capen, remained dark during
1994-95.


Cerberus I, forming the southern border of the Elysium Shield,
displayed some interesting changes, proving that it is a highly
variable feature. In fact, this was one of the features targeted for
intensive study by the HST. It was a dark and conspicuous feature
throughout the 1950s and early 1960s, weakening in 1965 and more in
1967, but returning as a thin but dark feature in 1969. It remained
conspicuous until the 1975 apparition, when it reached near
invisibility. It recovered somewhat in 1977 and darkened dramatically
after opposition in 1980. After the February and May dust storms of
1982, Cerberus weakened, a trend that continued after the 1984 dust
events. Since 1984,Cerberus has remained faded, although there has been
some variations in its intensity.

In 1994-95 Cerberus was fairly dark and conspicuous early in the
apparition.  However it became fainter by late November and early
December (23-25  Ls) when Trivium-Cerberus appeared on CCD images as a
halftone streak with 2-3 diffuse nuclei.  >From 2-12 January (40-44
Ls) it had weakened considerably, becoming a weak thin streak with
Trivium a small dark dot. During mid-February (57-60  Ls) the complex
was barely visible, appearing as only three small dots. Parkers March
18-25 CCD images (both tricolor and red light) showed Cerberus still
weak, just three small dots, especially after local noon.

Interestingly, however, several very experienced ALPO observers
independently reported that Cerberus became quite dark and streak-like
around March 14. During April the feature darkened considerably as
noted on both drawings and CCD images. It maintained that aspect for
the remainder of the apparition, but was still not as conspicuous as it
had been during the 1970s.

CONCLUSIONS

Despite the unfavorable aspect that Mars presented during the 1994-1995
apparition, much useful data was obtained. This was largely due to the
high quality of the observations submitted. Many IMP astronomers
systematically observed Mars when it was less than 6 arc-seconds in
apparent size, thus significantly extending the seasonal coverage.
Over 50% of observers, both visual and photographic, regularly employed
color filters  this is the highest proportion to date, and we hope that
the trend continues. In addition, the vast majority of the observations
submitted were properly documented as to image orientation, dates,
times, CMs, etc., and the quality of the reports was, on the average,
the highest we have seen. Despite the high tech contributions of CCD
imaging and active optics assisted photography, the visual drawing
remains the backbone of Mars observations.  Cases in point areTroianis
1994-95 Mars maps (Figs. 4-5) that were highly praised by a number of
professionals at the MTO Workshop. Even though Troiani generated these
on a computer, they were produced entirely from the amateur
observations submitted to the A.L.P.O. Mars Section. Many thanks to all
our observers!

ACKNOWLEDGEMENTS

The Mars Section of the Association of Lunar and Planetary Observers
wishes to express its gratitude for the contributions of fellow
A.L.P.O. members as well as those of the British Astronomical
Association and the Oriental Astronomical Association.

REFERENCES

Beish, J.D. and Parker, D.C. (1988) "The 1983-85 Aphelic Apparition of
Mars - Report I", J.A.L.P.O., Vol. 32, Nos. 9-10, p. 192.

Beish, J.D. and D.C. Parker (1990a). "The 1983-85 Aphelic Apparition of
Mars-Part II" J.A.L.P.O., Vol. 34, Nos. 2, pp 62-79.

Beish, J.D., and D.C. Parker 1990b). "Meteorological Survey of Mars,
1968-1985," Journal of Geophysical Research, Vol. 95, B9, pp.
14567-14675. August 20.


Bell, J.F. III and J.E. Moersch, eds. (1995). Workshop on Mars
Telescopic Observations.  LPI Tech. Rpt. 95-04. Order from: Order
Dept.  Lunar and Planetary Institute, Houston, TX 77058-1113. No
charge, but send $5.00 (US) for S&H.

Capen, C.F. and V.W. Capen (1970). Martian North Polar Cap, 1962-68.
Icarus, 13:1, pp.  100-108.

Dobbins, T.A., D.C. Parker, and C.F. Capen (1986). Introduction to
Observing and Photographing the Solar System. Richmond: Willmann-Bell,
Inc. pp.  193-201.

Ebisawa, S. (1995a). Mars Observations During The Period of 1994-1995
Apparition.  Dust Storm Displays: A Quick Preliminary Report. Planetary
Res.  Obs. Contrib. No. 23, Feb.

Ebisawa, S. (1995b). Probable Existence of the Martian North Permanent
Cap Beneath the Winter Polar Hood and Beneath the Saesonal Ground Cap
in Spring-Summer Season: A Preliminary Report. Planetary Res. Obs.
Contrib. No. 24, Aug.

Iwasaki, K., T. Akabane, R. Sagar, K.K. Ghosh, M. Raharto, and F.
Dirghantara (1995).  Regression of Martian Polar Cap 1994-1995. Proc.
28th ISAS Lunar and Planetary Symp 1995.

Lee, S.W., M.J. Wolff, P.B. James, L.J. Martin, R.T. Clancy, and J.F.
Bell (1995). HST Observations of Time-variable Albedo Features on Mars.
Workshop on Mars Telescopic Observations, LPI Tech. Rpt. No. 95-04,
p.19.

McKim, R. (1985). The Opposition of Mars, 1982. J. Brit.  Astron.
Assoc. 96:1, 36-52.

McKim, R. (1992). The Opposition of Mars, 1990. J. Brit.  Astron.
Assoc. 102:5, 251.

Parker, D.C., Capen, C.F., and Beish, J.D. (1983). "Exploring the
Martian Arctic", Sky & Telescope Magazine, Vol. 65, No. 3, March.

Parker, D.C. and R. Berry (1993). Clear Skies on Mars.  Astronomy,
21:7, pp. 72-77, July.

Stryk, T. (1994). The Martian Dust Cloud of 1994 Jun 05:  Appearance
and Implications.  J.A.L.P.O., 38:2, 85-86.




Table 1. Members of the A.L.P.O. International Mars Patrol for the
1994-1995 Apparition


Observer       Location                        Observer           

Makoto Adachi           Ohtsu City, Japan
Osczr Arnal         	Ontario, Canada 
Greg Banialis       	Arlington Hts., IL
Jeff Beish          	Miami, FL
Phillip Budine      	Walton, NY
Gary Cameron        	Des Moines, IA
Lawrence Carlino    	Lockport, NY
Jesse Carroll       	Chicago, IL
Jim Carroll         	Chicago, IL
Thomas Cave         	Long Beach, CA
                    	Mt. Wilson, CA
Vanessa Cave        	Long Beach, CA
John Crocker        	Chicago, IL
Brian Cudnik        	Flagstaff, AZ
Tom Dobbins         	Coshocton, OH
Darren Drake        	Indian Head Pk., IL
Garry Dymond        	St. John, Canada
Karl Fabian         	Hickory Hills, IL
Nelson Falsarella   	San Jose, Brazil
Vincent Giovannone  	Latham, NY
David Graham        	N. Yorkshire, UK
David Gray          	County Durham, UK
Bob Gunnerson       	Loveland, CO
Walter Haas         	Las Cruces, NM
David Hanon         	Chattanooga, TN
Carlos Hernandez    	Miami, FL
Richard Hill        	Tucson, AZ
Hiroshi Ishado      	Okinawa, Japan
Tohru Iwasaki       	Morodomi, Japan
Chuck Jacobson 		Puyallup, WA
Daniel Joyce        	Chicago, IL
David Lehman        	Pinedale, CA
Michael Mattei          Littleton, MA
Richard McKim  		Oundle,	UK
Frank Melillo       	Holtsville, NY
Masatsugu Minami    	Fukui, Japan
Patrick Moore       	Selsey, UK
Yukio Morita        	Hatssuka, Japan
Mike Morrow         	Ewa Beach, HI
Masami Murakami     	Fujisawa, Japan
Takashi Nakajima    	Fukui, Japan
Detlev Niechoy           Goettingen, Germany
Gary Nowak          	Essex Jct., VT
Yoshio Ohba         	Yamagata, Japan
Don Parker          	Coral Gables, FL
Cecil Post          	Las Cruces, NM
Phil Plante         	Poland, OH
Terry Platt         	Binfield Berks, UK
Robert Robinson     	Morgantown, WV
Mark Schmidt        	Racine, WI
Richard Schmude     	Barnesville, GA
Elisabeth Siegel        Agertoften, Denmark
Robert Smith        	Huntville, AK
Chester Spell       	Woodstock, GA
Robert Soltis       	LaJolla, CA
Ted Stryk      		Bristol, VA
Gerard Teichert         Hattstatt, France
Greg Terrance       	Lima, NY
Chris Tobias        	Racine, WI
Daniel Troiani      	Schaumberg, IL
Robert Young        	Harrisburg, PA
Johan Warell        	Uppsala, Sweden
John Westfall       	San Francisco, CA
Samuel Whitby           Hopewell, VA
Matthew Will        	Springfield, IL
Pat Winemiller          Terre Haute, IN
Gene Witkowski          Buffalo, NY
Mike Zweifel        	Yorkville, WI


Table 2. NPC Residuals (Bright Projections, ôOutliers.ö) 

Observer, 	Years, 	 Ierne,  Lemuria,  Cecropia

Schiaparelli 	1879-88  121 	 208 	    310
Lowell   	1901-05  122     206        311
Antoniadi  	1903-29  122     208 	    309
Maggini 	1918-35  136     213        278
de Mottoni 	1941-52  137     200        297
Dollfus 	1946-52  142     227        292
Capen 		1962-68  140     196        290
Beish/Parker/   1981-82  132     205        280
Capen/Dragesco 	

Beish/Parker/	1983-85  142     205        282
Hernandez/Dragesco 

Mean 133 208 294
Range 121 -142 196 -227 278 -311
 

Captions for IMAGES 1-20

1. 1994 June 07, 09:55 UT, CM: 127 , Ls: 290 , 10-in (25-cm) Newt.
Filter: None. Ted Stryk. First observation of the apparition showing
prominent southern maria.  De: -17 . Diameter only 4.45 arc- sec.

2. 1994 Nov 02, 08:15 UT, CM: 106 , Ls: 012 , 16-in (41-cm) Newt.
Filter: W47. Don Parker.  Prominent evening limb cloud with terminator
projection; bright morning limb haze.

3. 1994 Nov 03, 10:45 UT, CM: 133 , Ls: 012 , 7-in. (17.8-cm) Refr.
Filter: W21. Samuel Whitby.  N. Polar collar dark in orange light;
morning limb haze.

4. 1994 Dec 01, 08:31 UT,  CM: 194 , Ls: 025 , 16-in (41-cm) Newt. Don
Parker. From tricolor CCD image showing dark streak along northern
border of Cimmerium M. Hyblaeus extension prominent; Trivium-Cerberus
halftone. Lynxx PC camera.

5. 1994 Dec 26, 06:40 UT, CM: 294 , Ls: 037 , 17.5-in (45-cm) Newt.
Filter: W25. Dan Troiani.  Rima notch at edge of NPC , bright spot in
Hellas.

6. 1994 Dec 30, 09:20 UT, Cm: 276 , Ls: 39 , 14.25-in (36-cm) Newt.
Gene Witkowski. From video image showing faint Rima Tenuis.

7. 1995 Jan 01, 07:30 UT, CM: 251  Ls: 39 , 8-in (20-cm) Newt.  Filter:
W30. Carlos Hernandez.  Elysium cloud on evening limb. Hyblaeus
extension, N. Alcyonius, and Cerberus prominent.

8. 1995 Jan 06, 08:40 UT, CM: 38 , Ls: 42 , 12.8-in (32.5-cm) Newt.
Filters: R,O,B. Thomas Cave.  Trivium-Cerberus still dark but thin.

9. 1995 Jan 10, 05:45 UT, CM: 144 , Ls: 043 , 8-in (20-cm) Newt.
Filter: W30 (magenta). Carlos Hernandez. Tractus Albus noted over
Tempe-Tharsis. Propontis complex prominent.

10. 1995 Jan 10, 05:55 UT, CM: 147 , Ls: 043 , 8-in (20-cm) Newt.
Filter: W38A. Carlos Hernandez. Equatorial Cloud Band (ECB) over
Memnonia-Tharsis.  Refer to red light observation Figure 9.

11. 1995 Jan 20, 06:00 UT CM: 059 , Ls: 048 , 4.25-in (11-cm) Schief.
Filters: W23A, 80A. Gary Cameron. Chryse-Xanthe bright. Lunae Lacus
dusky, not discrete.

12. 1995 Jan 21, 00:25 UT, CM: 328 , Ls: 048 , 15-in (38-cm) Newt.
Filters: None. Patrick Moore.  Hellas light; Pandorae Fr. noted.

13. 1995 Jan 26, 09:10 UT, CM: 052 , Ls: 050 , 8-in (20-cm) Newt.
Filters: None. Robert Smith.  Idaeus Fons dark; Lunae L. not noted.

14. 1995 Jan 27, 09:10 UT, CM: 096 , Ls: 048 , 10-in (25-cm) Newt.
Filters: None. Daniel Joyce.  Rima Tenuis visible. Again, Lunae L. not
noted.

15. 1995, Jan 28, 02:45 UT, CM: 300 , Ls: 051 , 8-in (20-cm) Newt.
Filters: R,O,G,B. Nelson Falsarella. Sabaeus Sinus dark along its
length; Pandorae Fr.  prominent.

16. 1995 Jan 29, 05:30 UT, CM: 326 , Ls: 052 , 17.5-in (45-cm) Newt.
Filter: None. Dan Troiani.  Rima Tenuis prominent.

17. 1995 Feb 02, 23:26 UT, CM: 199 , Ls: 054 , 12.5-in (32-cm)
Tri-schief. From color CCD camera (Starlight Xpress). Terry Platt.
Orographic clouds Arcadia-Tharsis on evening limb.  Propontis complex
prominent.

18. 1995 Feb 02, 07:20 UT, CM: 324 , Ls: 054 , 14-in (36-cm) Newt.
Filters: W25A. Richard Hill.  Numerous canals, including
Arosis-Sitacus, Astaboras, and Hiddekel noted.

19. 1995 Feb 03, 05:35 UT, CM: 289 , Ls: 054 , 16-in (41-cm) Newt.
Filters: Tricolor CCD image.  Lynxx PC camera. Don Parker. Hellas Cross
noted. Boreosyrtis prominent.

20. 1995 Feb 05, 05:05 UT, CM: 265 , Ls: 055 , 11-in (28-cm) SCT.
Filters: R,O,G.B. Gerard Teichert. Casius dark on CM; Nasamon seen
extending from northeastern Syrtis Major. Bright cloud over Aethiopis.

Captions for IMAGES 21-40


21. 1995 Feb 06, 03:50 UT, CM: 238 , Ls: 055 , 10-in (25-cm) Newt.
Filter: W23A. John Crocker.  Hyblaeus extension dark, broad;
Trivium-Cerberus very weak.

22. 1995 Feb 07, 03:45 UT, CM: 228 , Ls: 056 , 10-in (25-cm) Newt.
Filters: R,G,B,Y. Ted Stryk.  Detail of NPC outliers, Rima Borealis.

23. 1995 Feb 02, 02:59 UT, CM: 260 , Ls: 054 , 16-in (41-cm) Newt. Greg
Terrance. Integrated light Lynxx PC CCD image showing Hyblaeus
extension broad and dusky. Cerberus very weak on PM limb.

24. 1995 Feb 11, 06:37 UT, CM: 235 , Ls: 058 , 16-in (41-cm) Newt.
Filters: Tricolor CCD image.  Lynxx PC camera.  Don Parker.
Trivium-Cerberus now very weak.

25. 1995 Feb 12, 06:45 UT, CM: 228 , Ls: 058 , 14-in (36-cm) Newt.
Filter: W23A. Richard Hill.  Trivium-Cerberus more prominent.

26. 1995 Feb 18, 03:03 UT, CM: 122 , Ls: 061 , 16-in (41-cm) Newt.
Filters: Tricolor CCD image.  Lynxx PC camera. Don Parker. Prominent
orographic clouds over Tharsis.

27. 1995 Feb 20, 04:20 UT, CM: 123 , Ls: 062 , 10-in (25-cm) Newt.
Filter: W25, 38A. David Lehman. Clouds over Tharsis. Possible polar
cloud on CM (Ierne region).

28. 1995 Feb 22, 19:47 UT, CM: 332 , Ls: 062 , 11-in (28-cm) SCT.
Filters: R,O,Y,G,B. Gerard Teichert. Sabaeus S. dark throughout its
length; Pandorae Fr.  strong, broad.

29. 1995 Feb 22, 03:40 UT, CM: 095 , Ls: 062 , 12.8-in (32.5-cm) Newt.
Filters: R,O,B. Thomas Cave. Clouds over Xanthe, Arcadia, Tempe, and
near Olympus Mons.  Lunae Lacus weak.

30. 1995 Feb 26, 01:40 UT, CM: 031 , Ls: 064 , 4.25-in (11-cm) Schief.
Filters: W23A, 80A. Gary Cameron. Clouds over Candor on AM limb; clouds
over Chryse, Arabia-Moab, and south limb.  Lunae Lacus weak.

31. 1995 Feb 26, 04:30 UT, CM: 72 , Ls: 064 , 14-in (36-cm) Newt.
Filters: W25A. Richard Hill.  Lunae L. very weak; Ganges prominent.
Acidalius Fons dark at S.  border of NPC with Issedon joining it to
Nilokeras. Lunae Lacus not discrete. Blue light observation reveals AM
and PM limb clouds.

32. 1995 Feb 28, 02:48 UT, CM: 030 , Ls: 065 , 16-in (41-cm) Newt. Don
Parker. From tricolor CCD image. Lynxx PC camera. Bright cloud on AM
limb over western Tempe. Hazes across Chryse and Moab. Nuclei in Idaeus
F. Lunae L. weak.

33. 1995 Mar 01, 01:58 UT, CM: 009 , Ls: 065 , 7-in (18-cm) Refr.  ST-5
camera CCD image.  David Hanon. Achillus P. light. Ismenius L.,
Deuteronilus, Dirce F., and Gehon detected!

34. 1995 Mar 04, 21:00 UT CM: 262 , Ls: 067 , 8-in (20-cm) SCT.
Filters: None. Report with W25, 15, 58, 80A, 47. Elisabeth Siegel.
Hyblaeus extension prominent. Aeria, Ausonia, and PM limb brightest
with W80A.

35. 1995 Mar 04, 00:40 UT, CM: 324 , Ls: 067 , 6-in (15-cm) Refr.
Filter: W23A. Lawrence Carlino. Aeria bright (see observation # 34);
Sabaeus S. and Hellespontis dark.

36. 1995 Mar 11, 01:45 UT, CM: 278 , Ls: 070 , 7-in (18-cm) Newt.
Filters: W25, 23A. Gary Cameron. Rima Tenuis noted. Hellas bright in
red and blue light.  Clouds reported over Moab, Aethiopis, and
Elysium.

37. 1995 Mar 13, 03:00 UT, CM: 274 , Ls: 071 , 100-in (2.5-M) Mt.
Wilson Coud. Filters: R,M.  Thomas Cave. Bright PM limb cloud
(Elysium). Numerous small white areas in desert regions.  Edge of NPC
scalloped.

38. 1995 Mar 14, 02:25 UT, CM: 261 , Ls: 071 , 6-in (15-cm) Refr.
Filters: W25, 12, 80A, 38A.  Phillip Budine. Nilosyrtis prominent.
Cerberus darkening.

39. 1995 Mar 14, 01:55 UT, CM: 253 , Ls: 071 , 6-in (15-cm) Refr.
Filter: Y8, Phil Plante. Aeria very bright on AM limb; Trivium-Cerberus
reported as dusky.

40. 1995 Mar 14, 03:00 UT, CM: 267 , Ls: 071 , 12.8-in (32.5-cm) Newt.
Filters: R,O. Vanessa Cave. Trivium-Cerberus darkened. Albor bright in
NE Elysium.

Captions for IMAGES 41-56


41. 1995 Mar 21, 20:00 UT, CM: 095 , Ls: 074 , 8-in (20-cm) SCT.
Filters: None for drawing.  Report with W25, 15, 58, 80A, 47. Elisabeth
Siegel. Ascraeus L.  and Ceraunius prominent near CM.

42. 1995 Mar 21, 04:45 UT, CM: 231 , Ls: 074 , 12.5-in (32-cm) Newt.
Filter: W25A. Walter Haas. NPC peanut-shaped. Cerberus II extending
between Pambotis L. and Gomer S.  Symplegades Insula bright.

43. 1995 Mar 22, 22:32 UT, CM: 122 , Ls: 075 , 12.5-in (32-cm)
Tri-schief. From color CCD camera (Starlight Xpress). Terry Platt.
Numerous orographic clouds over Tharsis.

44. 1995 Mar 23, 03:55 UT, CM: 201 , Ls: 075 , 16-in (41-cm) Newt.
Filters: Tricolor CCD image.  Lynxx PC camera. Don Parker.
Trivium-Cerberus strengthening.  Tharsis orographics on PM limb.

45. 1995 Mar 31, 01:28 UT, CM: 092 , Ls: 079 , 16-in (41-cm) Newt.
Filters: Tricolor CCD image.  Lynxx PC camera. Don Parker. Bright cloud
on AM limb over Memnonia. Cloud wisps over Tharsis.

46. 1995 Mar 31, 01:15 UT CM: 089 , Ls: 078 , 16-in (41-cm) Newt.
Filters: W47, 47B. Jeff Beish. Band cloud and numerous discrete clouds
over Tharsis, Xanthe.

47. 1995 Apr 09, 20:05 UT CM: 281 , Ls: 083 , 6.3-in (16-cm) Refr.
Filters: W21. Johan Warell.  PM limb haze. Hellas bright. Pambotis
Lacus noted adjacent to bright PM limb.

48. 1995 Apr 12, 20:00 UT, CM: 252 , Ls: 084 , 8.5-in (21.6-cm) Newt.
Filters: None. Richard McKim. Trivium-Cerberus darkened. Brightening
over Libya-Isidis R.-Neith R.-Aeria (Blue Syrtis Cloud?). PM limb
bright.

49. 1995 Apr 13 20:40 UT, CM: 253 , Ls: 085 , 16-in (42-cm) Dall-Kirk.
Filters: I.L., W15. David Gray. Cerberus I and II visible. Elysium
complex well-defined.

50. 1995 Apr 28, 21:10 UT, CM: 119 , Ls: 091 , 16-in (42-cm) Dall-Kirk.
Filters: I.L., W15. David Gray. Tharsis features noted: Nodus Gordii,
Eumenides, Ascraeus L., Ascuris L., and dusky bands.

51. 1995 May 13 21:20 UT, CM: 339 , Ls: 097 , 16-in (42-cm) Dall-Kirk.
Filters: I.L., W15. David Gray. Hellas, Chryse bright; Protonilus,
Ismenius L., Deuteronilus, Hiddekel, and Gehon noted.

52. May 30, 02:05 UT, CM: 255 , Ls: 105 , 16-in (41-cm) Newt.  Filter:
W47. Don Parker. ECB over Aethiopis-Isidis. Bright limb clouds. Syrtis
Major covered with the Blue Syrtis Cloud.

NPC Outliers

53. 1995 Feb 18, 03:15 UT, CM: 125 , Ls: 060 , 16-in (41-cm) Newt.
Filters: Red light (Schott RG- 610) CCD image. Lynxx PC camera. Don
Parker. Outliers Ierne and Lemuria south of NPC, separated from it by
the Chasma Borealis.

54. 1995 Feb 18, 01:50 UT, CM: 104 , Ls: 060 , 16-in (41-cm) Newt.
Filters: W25, 22. Don Parker.  Ierne west of the NPC; small outlier
glimpsed on PM limb.

55. 1995 Feb 25, 02:33 UT, CM: 053 , Ls: 064 , 16-in (41-cm) Newt.
Filters: Red light (Schott RG- 610) CCD image. Lynxx PC camera. Ierne
west of NPC. Small outlier in northern Ortygia east of NPC.

56. 1995 Mar 23, 01:56 UT, CM: 172 , Ls: 075 , 16-in (41-cm) Newt.
Filters: Red light (Schott RG-610) CCD image. Lynxx PC camera. Lemuria
southwest of NPC.




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