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th Report:
The CMO/OAA Observations made during a fortnight period
from
16 September 2003 (262°Ls)
to
30 September 2003 (270°Ls)
An OAA Mars Section article to be published in
CMO #280 (10 October 2003 issue)
Masatsugu MINAMI, Director of the OAA Mars
Section
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here review the fortnight period from 16 September 2003 to 30 September: The
season was λ=262°Ls on 16 September it reached the summer solstice
(λ=270°Ls) of the southern hemisphere on 29/30 September. The southern
polar region was under most insolation. The apparent
angular diameter δ was 23.4" on 16 September,
it went down to 20.9" at the end of September. The phase angle ι
increased from 16° to 25°. The central latitude was near φ=19°S ~ 20°S.
After
opposition the planet seems to have lost the interest of the casual observers,
while the Japanese observers looked more active though the seeing became
slightly poorer than expected this period when Typhoon 15 stayed at the
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total number of observers became down under 50, and those observers abroad who
made double figured observations are Don PARKER (DPk), Chris PELLIER (CPl)
and few, though still several important observations were made abroad. In
AKUTSU, Tomio (Ak) Tochigi, Japan
9
Sets of CCD Images (16, 17, 18 September 2003)
f/33×32cm
spec with a Bitran
BJ-41L
ASADA, Tadashi (As)
Munakata,
16
CCD Images (16, 17, 18 September 2003)
30cm SCT with a Panasonic NV-MX5000
BEISH, Jeffrey D (JBs)
1
Drawing (16 September 2003) 390, 590×41cm F/6.9 spec
BENAVIDES, Rafael (RBn) Córdova, España
6
CCD Images (17, 18, 22, 23 September 2003)
24cm SCT with
a ToUcam
BIVER, Nicolas (NBv)
4
Colour Drawings (16, 21, 25, 26 September 2003)
700×41cm speculum
near at the "Col
de la Bonette",
BUNGE, Robert (RBg)
2
Drawings (17, 26 September 2003)
480×43cm F/7.8 spec/270×15cm refr
CHAVEZ, Rolando (RCv)
1
CCD Image (21 September 2003)
20cm F/7 spec
with
a ToUcam
CRUSSAIRE, Daniel (DCr)
5
Sets of CCD Images (17, 19 September 2003)
10cm Fluorite L with
a Vesta Pro
6 CCD Images (16, 18, 20, 21
September 2003)
57cm spec (down to 20cm) with a KAF400
chip camera
DOBBINS, Thomas A (TDb)
OH,
3
CCD Images (16, 21, 26 September 2003)
f/28×35cm SCT with
a ToUcam
FRASSATI, Mario (MFr) Crescentino (VC), Italia
1
Drawing (17 September 2003) 400×20cm SCT
GRAFTON, Edward A (EGf)
1
Set of CCD Images (28 September 2003)
f/35×35cm SCT with
an ST-5C
HALL, George (GHl)
1
CCD Image (20 September 2003)
30cm SCT with
a ToUcam
HANON, David (DHn)
3
CCD Images (16, 17, 18 September 2003)
41cm spec with
Sony VX-2000
IWASAKI, Tohru (Iw)
28 Drawings (16, 18, 22, 23, 27, ~ 30 September 2003)
400×21cm speculum
KARRER, Michael (MKr) St Radegund, Österreich
3
CCD Images (17, 21, 25 September 2003)
f/35×18cm
Meade Refraktor with
a ToUcam
KOVACEVIC, Zlatko F (ZKv)
1
CCD Image (20 September 2003)
f/20×20cm SCT
with
a ToUcam
KOWOLLIK, Silvia (SKw)
6 CCD Images
(17, 19 September 2003)
18cm Starfire Refraktor with
a ToUcam Pro
KUMAMORI, Teruaki (Km) Sakai, Osaka,
Japan
10
CCD Images (16, 18#, 26#, 28 September 2003)
f/84×20cm Dall-Kirkham/f/30×60cm Cass# with a ToUcam
#
LAU, Patrick (PLa) Hong-Kong
2
Drawings (17, 19 September 2003) 300×25cm
Dobsonian
LAZZAROTTI, Paolo R (PLz) Massa,Toscana, Italia
3
Sets of CCD Images (19, 21, 22 September 2003)
25cm F/40 DL-252 Planewton with
Astromeccanica KC381
MASSÓ MILLEIRO, Félix (FMr) La
1
CCD Image (20 September 2003)
15cm refractor with a Quickcam 3000 pro
MELILLO, Frank J (FMl)
6 Red CCD Images (17, 22, 25, 30 September 2003)
20cm SCT with
a Starlight Xpress MX5
MINAMI, Masatsugu (Mn) Fukui,
47
Drawings (16, 17, 18, 21, 22, 26, 27, 28, 30 September 2003)
480, 400×20cm F/12 ED Goto refractor＊
＊Fukui
City Observatory, Fukui
MORITA, Yukio (Mo) Hatsuka-ichi,
17
Sets of CCD Images (16, 17, 22, 26, 27, 28 September 2003)
f/50×25cm speculum equipped
with an ST-5C
MURAKAMI, Masami (Mk)
25 Drawings (16, ~19, 28, 30 September 2003)
320, 400×20cm
speculum
NAKAJIMA, Takashi (Nj) Fukui,
20 Drawings
(16, 17, 22, 26, 28, 30 September 2003)
480, 400×20cm F/12 ED Goto refractor＊
＊Fukui
City Observatory, Fukui
NARITA, Hiroshi (Nr)
16 Drawings
(16, ~19, 22, 23, 28 September 2003)
290, 400×20cm
refractor
NG, Eric (ENg)
1
Set of CCD Images (17 September 2003)
f/34×32cm Royce spec with
ToUcam
OKANO, Kunihiko (Ok) Setagaya, Tokyo,
Japan
1
Set of CCD Images (18 September 2003)
31cm F/5 spec
with an ST-7XME
OSA, Kanehiro (Oa) Nonoichi, Ishikawa, Japan
1
Sets of CCD Images (28 September 2003)
15cm spec with
a COOLPIX990
PARKER, Donald C (DPk)
15
Sets of CCD Images (16, 19, 23, 27 September 2003)
f/55, 59×41cm F/6
spec equipped with an ST-9XE
PARKER, Timothy J (TPk) LA, CA,
2
CCD Images (28 September 2003)
15cm Jägers Achromat with
a ToUcam
PEACH, Damian A (DPc) Buckinghamshire,
7
CCD Images (24, 25, 28 September 2003)
f/31×28cm
SCT with a ToUcam
PELLIER, Christophe (CPl) Bruz,
14 Sets
of CCD Images (16, ~20, 23, 25, 29 September 2003)
18cm spec with a modified B&W ToUcam Pro
RODRÍGUEZ RAMÍREZ, Francisco A (FRd)
Gran
Canaria,
2
CCD Images (15/16 September 2003)
20cm SCT with
a ToUcam
SÁNCHEZ, Jesús R (JSc) Córdova, España
4
Sets of CCD Images (18, 22, 27 September 2003)
f/50×28cm SCT with
a ToUcam
SHERROD, P Clay (CSr) Aso Sky
10
CCD images (17,~20, 23, 24, 26, 27, 29 September 2003)
f/35×41cm SCT with
a ToUcam Pro
SIEGEL, Elisabeth (ESg) Malling, Danmark
7
Drawings (16, 18, 21, 23, 25, 27, 29 September 2003)
270×20cm F/10 SCT
TEICHERT, Gérard (GTc)
2
Drawings (21, 29 September 2003) 330×28cm SCT
TSUNEMACHI, Hitomi (Ts)
10
Drawings (21, 22 September 2003)
480, 400×20cm F/12
ED Goto refractor＊
＊Fukui
City Observatory, Fukui
VALIMBERTI, Maurice P (MVl)
6
CCD Images (21, 22, 27, 29 September 2003)
f/34×35cm SCT with
a ToUcam Pro
Van Der VELDEN, Erwin (EVl)
4
CCD Images (18, 22 September 2003)
f/31×20cm
SCT with a Vesta
Pro modified
WALLER, Skip (SWl)
1
CCD Image (16 September 2003)
f/50×25cm SCT (LX200) with a ToUcam Pro
WARELL, Johan (JWr)
2 Drawings (18, 28 September 2003) 260×25cm
SCT (LX200)
11
Sets of CCD Images (17, 18, 21, 26, 27, 28, 30 September 2003)
f/24×25cm
SCT with a ToUcam
WILLIAMSON, Thomas E (TWs)
2
CCD Images (26, 29 September 2003)
f/50×20cm spec with
a ToUcam
ZANOTTI, Ferruccio (FZt) Ostellato (FE), Italia
1
Set of CCD Images (18 September 2003)
45cm spec with
a ToUcam
Most Impressives: Among a
number of observations reported this period, the series produced by Don PARKER
(DPk) on 27 Sept 2003 (λ=269°Ls)
at ω=082°W ~ 114°W (made of 6 sets of R, G, B
images) was most impressive and important. Here was shown nicely reproduced the
phenomenon of the de-concentration of the morning mist at a special area which
was previously traced by Canon LAU (CLa) on 9 Sept 2003 (λ=257°Ls) from ω=061°W to 127°W.
The phase angle ι was 11° previously, while this time ι=24°, and
hence there was a local time difference of about one hour at the CM. So the
image of CLa
at ω=096°W might correspond to DPk’s
ω=114°W: So we are led to conclude that the special de-concentration patch
was therefore occurred at the same place. If it is located longitudinally at
Morning Mist (Frost): The season
proceeded and the water vapour moved much northwards,
and the morning mist (or frost) now looked conspicuous as the phase angle
increased. To the naked eyes, the morning side was largely covered by a white
mist including frost, while the evening side was rather yellowish and quite
different (eg: 18 Sept (λ=263°Ls) at
ω=340°W and so on by the present writer (Mn)). Refer also to BIVER
(NBv)’s LtE in #279. DPk’s images on 16 Sept (λ=262°Ls)
at ω=198°W~219°W describe delicately an uneven
expansion of the morning mist from M Tyrrhenum to Hellas before the rise of
Syrtis Mj. There are several spots in M Tyrrhenum on which the distribution of
mist is not uniform (note otherwise these DPk’s
images show well the tip of the very morning Novus Mons as well as the varied
Ætheria dark patch (now patches? with two wings)). Another set of images which
enhanced the morning mist at the similar place was taken by SHERROD (CSr) on 17 Sept (λ=262°Ls) at ω=218°W and so on. The morning white mist
over
Equatorial Band Mist?: The ccd expressions
deeply depend on the image processing so that sometimes the judgement is forced
to be ambivalent. However the image by HANON (DHn) on 18 Sept (λ=263°Ls)
at ω=185°W looks to show there exists a weak
white mist expansion inside the disk located to the north of M Cimmerium which
may also be connected with the preceding white Tharsis
region to the evening limb. The images by CSr
made on 20 Sept (λ=264°Ls) at ω=197°W may also show the band mist. Also
the previously cited images of DPk
made on 27 Sept may convey a white mist around Tharsis near the CM. The white mist over the Equatorial
Band (EB) is known to be conspicuous just before the northern hemisphere
reaches the summer solstice. As once touched in CMO #200, after the spring equinox of the
summer hemisphere, the warmed air mass comes down from the summer polar region,
at the same time by receiving the Coriolis effect,
towards the equatorial region, while since the equator loses the Coriolis force which makes a retardation of cooling, the
air is more cooled down to make a condensation mist belt. So this is also
possible to occur when the summer hemisphere is the southern. This time the
atmosphere was so mingled with airborne dust, that the equator band might have
been too critical to produce the thicker mist, but if the EB mist could have
been well detected, it might have given a barometer to show how much the dust
has been settled.
Wine-Coloured Grounds: The abundance of the
white mist or cloud does not necessarily imply the cease of excess of airborne
dust because the dusts are providing the nuclei needed in the formation of the
vapour-condensation. However the decolouring of the yellow tinge or the uneven
distribution of the white mists may imply the decay and/or lack of the airborne
distribution of dust. In this sense it is interesting to observe the
de-concentration of mist as well as to find the grounds which show the hue of
wine colour. If we look through one by one the excellent series of images made
by VALIMBERTI (MVl) on 21 Sept, 22 Sept, 27 Sept, and on 29 Sept, we are to be led to notice that the WE
dark band at around 60°S looks wine-coloured. In particular, the images on 27
Sept (λ=269°Ls) at ω=227°W & 241°W show that the colour at
M Chronium including Tiphys
Fr is conspicuous. Km’s images on 26
Sept (λ=268°Ls) at ω=259°W, and on 28 Sept (λ=269°Ls) at ω=225°W~287°W also prove vividly this. The
image by DOBBINS (TDb)
on 26 Sept (λ=268°Ls) at ω=123°W also suggests that the phenomenon
extended further eastwards, and it may be related with the occurrence of the
de-concentration at the area around Solis L previously reported in #279. CPl’s B images on 25 Sept
(λ=268°Ls) at ω=028°W & 038°W also well give signs of
this. The clearance of dust around the 60°S band may indicate that the new dust
disturbance from the spc or its perimeter has now been confined to no wider
than quite the south circumpolar narrower region.
Thyle: Such
a dark band as M Chronium proves to be conspicuous in
brownish-wine-colour to the naked eyes, and sometime looks the darkest. On 28 Sept
(λ=270°Ls), the present writer (Mn)
began to watch from ω=211°W (and then at ω=221°W, 230°W, 240°W,
250°W, 269°W and 279°W), and he noticed from the outset that the southern
perimeter of M Chronium is clearly shown, and Thyle to the south of it was rather bright. From
ω=221°W, the dark fringe of the spc looked denser. The area in Thyle corresponded to the one where BUDA (SBd) had once
found a disturbance on 19 Aug (λ=244°Ls) at ω=233°W. The angular diameter was already not enough
to see the details, but it was suspected that there was or had been an activity
of disturbance. Chasing the area to the limb side (~ω=269°W), we found the
area became brighter like a frosted or clouded area: This phenomenon at the
limb side was also seen previously on 26 Sept (λ=268°Ls) at
ω=239°W~268°W, as well as on 27 Sept (λ=269°Ls) at ω=259°W &
269°W. The series of MORITA (Mo)’s images
on 27 Sept (λ=269°Ls) at ω=254°W~286°W looks to confirm this.
IWASAKI (Iw)
also pointed out that Thyle looked clear and
conspicuous on 27 Sept at ω=232°W, as well as on 28 Sept at ω=233°W.
On 28 Sept, MURAKAMI (Mk) also
observed eight times from ω=191°W to 260°W, and at around ω=230°W he
caught the complex aspect of Thyle together with the
distinguished M Chronium.
We remark otherwise that
when the western part of Thyle was located near the
morning terminator, the place looked still yellowish as dusty as already
alluded in the preceding issues (as shown on the images by MVl on 1 Sept (λ=252°Ls)
at ω=110°W etc). See
for example images by CPl on 16 Sept
(λ=262°Ls) at ω=128°W~134°W, those by KOWOLLIK (SKw) on 17 Sept (λ=263°Ls) at ω=116°W~131°W. On 18 Sept (λ=263°Ls), CPl also showed it at ω=099°W
and JSc at ω=100°W
& 120°W and as well on
19 Sept (λ=264°Ls), SKw at ω=090°W
& 095°W and CPl at ω=099°W
& 109°W and so on. We
can similarly find other work showing the same phenomenon, but they prove it
gradually became not so conspicuous.
Dædalia: SIEGEL (ESg)’s sketch made on 16 Sept
(λ=262°Ls) at ω=106°W shows
Eridania, Ausonia, Trinacria
and
The South Polar Cap: The spc was regularly thawing, and it was seen totally inside the disk.
Visually this time the spc on 17 Sept (λ=262°Ls) sometimes
looked off-white, while on 28 Sept (λ=270°Ls), it looked very clear cut.
Thyles Mons, previously
an interesting topic, has thawed away.
Novus Mons: Novus Mons,
now at its final stage, was an object to be checked first at the Oceania-Asia’s
eastern hemisphere. The season λ=262°Ls was just the case where Mk took an image of Novus Mons in 1988
by the use of a 10cm Nikon refractor exposed on TP2415 (see CMO #116), and
fortunately Mk this time was able to
chase it on 16 Sept (λ=262°Ls) from ω=331°W to 013°W, and also caught
the sight on the following day. Visually also Iw observed it on 16 Sept and 18 Sept
every 40 minutes, and Mn also chased
it from 16 Sept to 18 Sept. As the CM came round to ω=030°W, its beyond part became dull near the evening limb. The ccd imagers were also active: On 16 Sept, Km took it at ω=340°W, 353°W, ASADA (As) at ω=350°W, Mo at ω=357°W, and
AKUTSU (Ak) at ω=014°W and so on. On 17 Sept
(λ=263°Ls) Ak
took from ω=334, Mo
at ω=354°W~017°W, and Eric NG (ENg) at ω=005°W. Novus Mons looked still brighter
on the early afternoon side. On 18 Sept (λ=263°Ls), Van der VELDEN (EVl) took it at ω=320°W, Km at ω=332°W, and OKANO (Ok) at ω=333°W: The former described it white but
the latter off-white. Visually Patrick LAU (PLa) in Hong-Kong detected a
final stage on 19 Sept (λ=264°Ls) at ω=032°W. Novus Mons more inside on the
images of MVl on 21 Sept
(λ=265°Ls) at ω=302°W, as well as on 22 Sept
(λ=268°Ls) at ω=293°W looks blurred though the images are
good in general. EVl’s images at ω=287°W, 299°W on 22 Sept show it more
clearly. The time was coming, and TSUNEMACHI (Ts) came down to Fukui to check it with Mn and Nj. Unfortunately
the seeing was not so preferable, but we saw the faint Novus Mons on 22 Sept
(λ=266°Ls): Ts observed from
ω=265°W to 330°W. The present writer (Mn)’s
chasing at
The North Polar Hood: Since the season now reached the northern
winter solstice, it might be interesting if we could catch well the behaviour
of the nph. However since φ=20°S it was hard in actuality. Around 17 Sept
(λ=262°Ls), the nph on the surface where
On 16 Sept (λ=262°Ls) and 17 Sept, there was
observed an interesting EW division by the nph fragment. The series of images
by Mo on 17 Sept (λ=262°Ls) up
until ω=017°W as well as ENg’s image at ω=005°W record the interesting activity.
Otherwise, MKr’s
ccd images on 21 Sept (λ=265°Ls) at ω=056°W, NBv’s drawing on 26 Sept
(λ=268°Ls) at ω=019°W, and JSc’s image on 27 Sept
(λ=269°Ls) at ω=041°W also show the similar angle and
similar phenomenon related with the nph.
Among the ccd images,
none can be found in particular that provides a particular protrusion this time
also. We expect always any image of the nph at the surface where Propontis I is
near the CM, but none until now. This season Propontis I (35°N~40°N) looked
divided into two, but it is unknown whether it was because of a fallout of dust
or it was casually caused by the dust behaviour of the nph. HALL (GHl)’s image on
20 Sept (λ=264°Ls) at ω=205°W may suggest Propontis I recovered,
but just 5 days before DPk produced a
usual split image of Propontis I on 15 Sept (λ=261°Ls) at ω=207°W, and so
we are not yet certain.
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he next issue shall treat
the observations made in the First Half of October 2003 from 1 October (λ=271°Ls) to 15 October 2003
(λ=280°Ls,
δ=17.9").
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