14 |
th Report:
The CMO/OAA Observations made during a fortnight period from
1 September 2003 (252°Ls) to 15 September 2003 (261°Ls)
An OAA Mars Section article to be published in
CMO #279 (25 September 2003 issue)
Masatsugu MINAMI, Director of the OAA Mars
Section
T |
HE
planet Mars being just after opposition, the biggest angular diameter δ
has begun to decrease. However even on 15 September, δ read 23.6",
and not so different from the maximal diameter = 23.8" in 1988. On 13
September, TSUNEMACHI (Ts) was still
able to detect the tiny Juventæ Fons
and the light Aurea Cherso
clearly by the use of a 12.5cm refractor (based upon her experiences in August
at
T |
HE
observers have begun decreased in number as suggested and a total is less than
sixty. As September came in, the weather in
AKUTSU, Tomio (Ak)
33 Sets of CCD Images (2, 4, 5, 9, 11, ~15 September 2003)
f/33×32cm spec with a Bitran BJ-41L
ASADA, Tadashi (As) Munakata,
50 CCD Images (18, ~23, 27 September 2003)
30cm
SCT with a
Panasonic NV-MX5000
BATES, Donald R (DBt)
3 CCD Images (1, 6, 7 September 2003)
f/24,32×25cm spec with a ToUcam Pro
BEISH, Jeffrey D (JBs)
1 Drawing (8 September 2003)
390, 590×41cm F/6.9 speculum
BENAVIDES, Rafael (RBn) Córdova, España
16 CCD Images (1, 2, 3, 10, 14, 15 September 2003)
24cm SCT with a ToUcam
2 CCD Images (3 September 2003) f/30×23cm SCT with a TRV-900
BUDA, Stefan (SBd)
4 CCD Images (1, 6, 12 September 2003)
f/48×25cm
Dall-Kirkhams with an evolved TC211
BUNGE, Robert (RBg)
2 Drawings (6, 7 September 2003) 480×43cm F/7.8 spec
CHAVEZ, Rolando (RCv)
3 CCD Images (1, 9, 13 September 2003)
20cm F/7 spec with a ToUcam
CRUSSAIRE, Daniel (DCr)
2 Sets of CCD Images (3*, 8 September 2003)
10cm Fluorite L with a Vesta Pro
*25cm Cass (named
Caroline) with a Vesta Pro at Meudon
DENNERL, Konrad
(KDn) München, Deutchland
1 CCD Image (4 September 2003) 11cm spec with a ToUcam Pro
DIJON, Jean (JDj) Sillans, Isêre, France
1 CCD Images (3 September 2003)
57cm spec (down to 20cm) with a KAF400 chip camera
DOBBINS, Thomas A (TDb)
1 CCD Image (7 September 2003) f/28×35cm SCT with a ToUcam
FRASSATI, Mario (MFr) Crescentino (VC), Italia
1 Drawing (14 September 2003)
400×20cm SCT
FUMEGA UCHA, Camilo
(CFm) Ourense, España
1 CCD Images (11 September 2003)
f/20×31cm spec with a ToUcam
GRAFTON, Edward A (EGf)
3 Sets of CCD Images (9, 11, 14 September 2003)
f/39,
34×35cm SCT with an ST-5C
HALL, George (GHl) Dallas, TX, USA
1 CCD Images (7 September 2003) 30cm SCT with a ToUcam
HANON, David (DHn)
5 CCD Images (2, 9, 10, 11, 12 September 2003)
41cm
spec with Sony VX-2000
HEATH, Alan W (AHt) Nottingham,
6 Drawings (1, 3, 4, 6, 10, 13 September 2003)
180, 280×25cm speculum
IWASAKI, Tohru
(Iw)
19 Drawings (1, 3, 4, 6, 7, 8
September 2003) 400×21cm speculum
KARRER, Michael (MKr) St Radegund, Österreich
1 CCD Image (7 September 2003)
f/35×18cm Meade Refraktor with
a ToUcam
KOWOLLIK, Silvia (SKw)
15 CCD Images (4, 3, 4/5, 8, 15
September 2003)
18cm Starfire Refraktor with a ToUcam Pro
KUMAMORI, Teruaki
(Km)
Sakai, Osaka, Japan
25 CCD Images (1, ~4, 8, 9#,
11, ~13, 14#, 15 September 2003)
f/84×20cm Dall-Kirkham/f/30×60cm
Cass# with a ToUcam
#
LAU, Canon (CLa) Hong-Kong
6 CCD Images (9, 12 September 2003)
f/59×35cm SCT with a ToUcam
LAU, Patrick (PLa) Hong-Kong
3 Drawings (9, 12 September 2003) 300,
340, 400×25cm Dobsonian
LAZZAROTTI, Paolo R (PLz) Massa,Toscana,
Italia
1 Set of CCD Images (6 September 2003)
18cm F/15 Mak-Cass with
Astromeccanica KC381
MASSÓ MILLEIRO, Félix (FMr) La Corña, Galicia, España
1 CCD Image (12 September 2003) 25cm spec with a ToUcam
MELILLO, Frank J (FMl)
11 Red CCD Images
(1, 6, 7, 8, 10, 11 September 2003)
20cm SCT with a Starlight Xpress
MX5
MELKA, James T (JMl)
1 CCD Image (7 September 2003)
f/130×31cm speculum with Canon D60
MINAMI, Masatsugu (Mn)
Fukui,
65 Drawings (1, 2, 4, ~7, 9, 11, 13, 14, 15 September 2003)
480, 400×20cm F/12 ED Goto
refractor*
*
3 CCD Images (2, 3 September 2003)
f/50×40cm speculum with ToUcam Pro
MORITA, Yukio (Mo)
Hatsuka-ichi,
23
Sets of CCD Images (1, 6, 7, 8, 13, 14, 15 September 2003)
f/50×25cm speculum equipped with an ST-5C
MURAKAMI, Masami (Mk)
27 Drawings (5, 9*,
10, 11, 12*, 13 September 2003)
320, 400×20cm spec, 450, 320×15cm spec*, 350×15cm refr*
*Kudan HS
Observatory, Tokyo
NAKAJIMA, Takashi (Nj) Fukui,
12 Drawings (6, 7, 8, 15 September 2003)
400×20cm F/12 ED Goto refractor*
*
NARITA, Hiroshi (Nr)
12 Drawings (4, 5, 6, 11, 12 September 2003)
290, 400×20cm refractor
NG, Eric (ENg)
5 Sets of CCD Images (9, 11, 12 September 2003)
f/34×32cm Royce spec with ToUcam
OKANO, Kunihiko (Ok)
Setagaya, Tokyo, Japan
1 Set of CCD Images (5 September 2003)
31cm F/5 spec with an ST-7XME
PACE, Ben (BPc)
3 CCD Images (8, 13, 15 September 2003)
f/34×15cm Maksutov with
a ToUcam
PARKER, Donald C (DPk)
17 Sets of CCD Images (3, 7, 8, 10, 15 September 2003)
f/55, 59×41cm F/6 spec equipped with an ST-9XE
PARKER, Timothy J (TPk) LA, CA,
6 CCD Images (1, 14 September 2003)
15cm Jägers Achromat with
a ToUcam
1 CCD Image (12 September 2003) 20cm spec with a ToUcam Pro
PELLIER, Christophe
(CPl) Bruz,
11 Sets of CCD Images (1, 2, 13, 15 September 2003)
18cm spec with a modified B&W ToUcam Pro
RODRÍGUEZ RAMÍREZ, Francisco A (FRd) Gran Canaria,
3 CCD Images (9, 15/16 September 2003)
20cm SCT with a ToUcam
SÁNCHEZ, Jesús R (JSc) Córdova, España
1 CCD Image (10/11 September 2003)
f/40×28cm SCT with a ToUcam
SHEEHAN, William P (WSh) Mt Hamilton, CA, USA
14 Drawings (2, ~7, 11, 12 September 2003)
487,
655×91cm refractor at the Lick
Observatory
SHERROD, P Clay (CSr) Aso Sky
12 CCD images (4, ~11 September 2003)
f/35×41cm SCT with a ToUcam Pro
SIEGEL, Elisabeth (ESg) Malling, Danmark
8 Drawings (1, 4, 5, 7, 11, 12, 13, 14 September 2003)
270×20cm F/10 SCT
TAN, Wei-Leong (WTn)
2 Sets of CCD Images (3, 4 September 2003)
f/42×25cm Meulon with
a ToUcam Pro
TATUM, Randy (RTm)
1 CCD Image (10 September 2003) 25cm spec with a ToUcam
TEICHERT, Gérard (GTc)
4 Drawings (1, 2, 4, 13 September 2003) 330×28cm SCT
TSUNEMACHI, Hitomi
(Ts)
7 Drawings (13 September 2003)
260, 360×12.5cm Takahashi
Fluorite refractor
VALIMBERTI, Maurice P (MVl)
5 CCD Images (1, 3, 6 September
2003)
f/34×35cm SCT with a ToUcam Pro
Van Der VELDEN, Erwin (EVl)
3 CCD Images (4, 5 September 2003)
f/31×20cm SCT with a Vesta
Pro modified
WALLER, Skip (SWl)
1 CCD Image (13 September 2003)
f/50×25cm SCT (LX200)
with a ToUcam Pro
WARELL, Johan (JWr)
2 Drawings (9, 11
September 2003) 260, 400×25cm SCT (LX200)
12 CCD Images (2, 3, 6, 9, ~13, 15 September 2003)
f/23×25cm SCT with a ToUcam
WILLIAMS, Bill (BWl) Ft
2 CCD Images (9 September 2003) 38cm Dob with
ToUcam
WILLIAMSON, Thomas E (TWs)
1 CCD Image (2 September 2003) f/45×20cm spec with a ToUcam
WILSON, Barbara (BWs)
2 CCD Images (7 September 2003)
20cm spec with a Nikon Coolpix 995
ZANOTTI, Ferruccio
(FZt) Ostellato (FE), Italia
2 Sets of CCD Images (4 September 2003) 45cm spec with a ToUcam
P |
reliminaries: Sorry to begin from personal affairs, but the present writer (Mn) re-started to observe at home at the
Observatory of the Fukui City Museum of Natural History (at about 36.1°N while
Naha at about 26.1°N) by the use of a 20 cm refractor; On 1 Sept, the angular
diameter being still 25.0", the Martian surface looked fresh from
Fukui, and starting from 12:10 GMT
(ω=112°W), we were able to check the familiar details of such linear
markings as Phasis and Agathodæmon;
the south polar cap (spc) appeared to locate totally inside the disk. Another
refreshed impression was that the surface was still dirty with the yellowish
global haze. In addition to that we got the renewed impression that the white
mists had quite prevailed equally at the morning terminator and the evening
limb. The season λ=252°Ls implied the sub-solar latitude DS was high up
nearly to 25°S, and hence the temperature in the daytime must have been quite
different from the night-time temperature at the southern middle latitudes
because the airborne particles absorb excessively the solar insolation
(and emit in the night-time). It was so quite possible that further
disturbances might be caused, and at least the settling of dust would have been
further delayed.
From our side, the range from Solis L to Syrtis
Mj was observed, while in
Disk’s Limb, Morning/Evening
Mists and the Southern High Latitudes: Since the
phase angle ι is small as time is not far from the opposition, the both
sides of the disk appeared unbiased. The water vapour being much toward
northward as the summer solstice was near, the condensed fogs or mists were
seen equally at dawn and evening limb quite rich. However the morning
terminator as well as the evening limb side at the southern high latitude
looked still quite dusty yellowish. For example, the image made by DENNERL (KDn) on 4 Sept
(λ=254°Ls) at ω=244°W well shows the white hood at the npr as well as the white fog or frost at the northern limb
and terminator sides, and at the same time the yellowish limb at the southern
high latitudes. OKANO (Ok)’s detailed
images on 5 Sept (λ=255°Ls) at ω=118°W also prove this phenomenon. The
morning mist or frost will vanish visually as the place rotates into more
inside, while the airborne yellowish haze will survive even at noon.
The morning mist or fog just after the daybreak
appeared slightly different from area to area: In this sense the thick fog at
the area of Solis L was quite interesting. For instance, on 2 Sept
(λ=253°Ls) HANON (DHn)’s
image at ω=356°W shows the mist over Solis L
beautifully (see also the yellowish haze at the southern high latitudes). Then
WILLIAMSON (TWs)’s
images at ω=030°W shows it quite deep inside the
disk. Otherwise, PELLIER (CPl)’s
images at ω=258°W ~ 263°W depict the thick morning
fog at Æria (as well SIEGEL (ESg)’s drawing on 1 Sept (λ=252°Ls) at ω=260°W
shows this), and AKUTSU (Ak)’s
images at ω=105°W ~ 144°W show also morning mists at
different region. WARREL (JWr)’s images on 3 Sept (λ=253°Ls) at ω=006°W show the thick nph as well as the
morning mist. VALIMBERTI (MVl)’s
images at ω=107°W/109°W show specifically an
interesting configuration of the morning mist. This case as well as the morning
mist over Solis L will be mentioned again later. The Solis L case in the latter
half of the period is compiled as follows: KUMAMORI (Km)’s on 12 Sept (λ=259°Ls) at ω=028°W; Ak’s on 13 Sept (λ=260°Ls) at ω=017°W, 027°W; MORITA (Mo)’s on 14 Sept (λ=261°Ls) at ω=011°W, 021°W, 031°W; Ak’s on 15 Sept (λ=261°Ls) at ω=019°W and so on.
As to the evening mist, the descriptions by Ak on 2 Sept
(λ=253°Ls) at ω=105°W~144°W and by Km on 3 Sept (λ=254°Ls) at ω=097°W, 124°W are good (equally with the
morning mist). At the latter part of the period, ι increased and the
balance became broken in general. We finally note that the Arsia white cloud
still prevailed this period.
Southern High Latitudes and Wine-Coloured Areas: The present writer (Mn) observed around 5 Sept (λ=255°Ls) and 6 Sept
(λ=256°Ls) that the southern circumpolar region had slightly decoloured
and quite showed a sandy tint. On 5 Sept ω=079°W ~ 108°W, he even noted
that it was impossible to detect the ruddy tint. On 11 Sept (λ=259°Ls)
however he observed at ω=036°W, 055°W et al the area showed a ruddy
colour, while at ω=084°W the area was rather brownish. It was thought so
that the water supply from the spc had been rather weakened and/or the yellow
haze was rather strong. On 9 Sept (λ=257°Ls), another interesting
observation was made at ω=061°W, though the seeing condition was not so
preferable after the thundershower, that the area at the morning higher latitudes
around the area from Aonius S to Depressio Pontica and further was quite dark, darker than the
preceding Solis L, and then at ω=080°W, 092°W, the area including Solis L
looked quite brownish or wine coloured. In contrast to this, the area of Auroræ S was rather dark bluish. On the day, KUMAMORI (Km) took a good image at ω=044°W by the 60cm Cassegrain,
and Ak also made a set of images at ω=050°W, 058°W: They all prove that a
tongue-like region from the area from Aonius S to Coracis Portus to Solis L
crossing Thaumasia Fœlix
was popped out of the large morning mist showing vividly a dark wine colour.
This configuration is evident in B images, and so the exceptional colour
difference was caused by a de-concentration of the water condensates mingled
with the airborne dusts. The images by PAU (KPa) at ω=042°W and by NG (ENg) at ω=046°W~067°W on 12 Sept (λ=259°Ls) also show the de-concentration similar to that seen
on 9 Sept, but this case, Solis L looked to be partially covered by a white
mist. Anyway the de-concentrations or uneven irregular configurations of the
floating
This
phenomenon seems not particularly rare, and in fact is seen for example on an
HST image taken on 14 December 1990 (λ=349°Ls, this year Mars was at
opposition on 27 November while closest on 20 November) here cited (from the
Site of Chris PELLIER (CPl) quoted in
CMO #276 Report #11). Since this was taken much
later in season, similar uneven configuration should be observable hereafter
also. Note that the de-concentration of misty expansion in the HST image also
occurred from Argyre to Solis L thru Thaumasia.
Canon LAU Phenomenon: The first
observation of the de-concentration on 9 September was slightly early to
Hong-Kong, while the second on 12 September was too late in
This spot was also detected by several other
observations: Early on 3 Sept (λ=253°Ls) MVl’s image at ω=107°W already shows it, and Mo’s
as well as ASADA (As)’s
images on 7 Sept (λ=256°Ls) at ω=095°W, 105°W, and Km’s on 8 Sept (λ=257°Ls) at ω=097°W, 113°W all suggest the same
temporary spot.
Trinacria to Hellas: There can be
witnessed a blurred light column from Trinacria to the eastern part of Hellas
straightforwardly on the images of CPl
made on 1 Sept (λ=252°Ls) at ω=307°W, and this is also seen on the
images made on 3 Sept (λ=254°Ls) by KOWOLLIK (SKw) at ω=246°W ~ 256°W, and by DIJON (JDj) at ω=247°W. We may also say that the images by
DOBBINS (TDb)
on 7 Sept (λ=256°Ls) at ω=308°W and by DHn on 11 Sept (λ=258°Ls) at
ω=261°W also suggest the vague different
coloured column. It is not known what it is made of, but it may be a deposit
made from a fallout since it seems to stand still
(maybe from an earlier period) days and nights. More detailed image was given
by GRAFTON (EGf)
on 11 Sept (λ=258°Ls) at ω=288°W in which the blurred part is not
remarkable. Surely markings including others
Osidis Promontrium?: A light spot is seen at the east coast of
Decay of Thyles Mons: The circumpolar area
around Thyles Mons has been the most interesting place to watch at this period.
From Oceania/Asia the place was seen near at the CM on 1 September when the
planet was high up at meridian and so the area was chased rather in details.
The ccd images by MVl
made on 1 Sept (λ=252°Ls) at ω=110°W, 146°W are most suggestive. Thyles
Mons exists as a weakened but still explicit projection and beyond it there is
seen an expansion of a yellowish dusty marking. The latter seems to come down
faintly to the east end of M Sirenum. BUDA (SBd)’s images at ω=130°W (134°W) also fulfilled the gap to
show this phenomenon but less colourfully. In
As to Thyles Mons at λ=254°Ls, we once
dealt with its 1988 case in comparison with the case in 1971 in CMO #087 (25
May 1990 issue) at p0731 as “1988 CMO
Note (12).” Figures
Since the MGS has been much interested in the
outburst of dust from the north polar region, and so we suppose they could have
never missed the chance to trace the decay of Thyles Mons as a phenomenon in
question ever since De VAUCOULEURS’ observation at the LPL, but unfortunately
we have not big ears.
Argenteus Mons and Rima Angusta: Argenteus
Mons, once very conspicuous, looked down to be normal. No decay was observed.
Furthermore we have few images showing the contour of the spc in a good balance
though any image at around ω=040°W suggest Argenteus Mons. Especially only
a few that shot the rift following Argenteus Mons. Rima
Angusta was visually caught around 6 and 7 Sept
(λ=256°Ls), as observed by IWASAKI (Iw) as well as by Mn,
but no ccd image was successful in
Novus Mons and Its Preceding
Area: Novus Mons was still present explicitly
even at the end of this period (λ=260°Ls). It was lucky for TDb to be able to
catch it by his first shot on 7 Sept (λ=256°Ls) at ω=308°W. Any image that took Novus Mons
near the CM might be all successful, and as well our MURAKAMI (Mk) was visually able to catch it
clearly on 11 Sept (λ=259°Ls) at the angle ω=031°W after these 15
years (his last shot of Novus Mons on TP2415 by a Nikon 10cm refractor was made
on 29 August 1988 at λ=262°Ls when
δ=21.8" --- cf CMO #116 p1017). Among many, the faint description of
WALLER (SWl)
from an oblique angle at ω=264°W on 13 Sept (λ=260°Ls) is
fantastic. From the similar angles WILLIAMS (BWl) gave further interesting
images on 9 Sept (λ=257°Ls) at ω=269°W, 285°W in which at the already
vanishing preceding area of Novus Mons there still remains a small isolated
piece of island. Standard series of images made by DPk on 8 Sept (λ=256°Ls) at ω=265°W(268°W), 278°W, 278°W(282°W), 287°W(289°W) show
Novus Mons quite well as well as the isolated BWl point (DPk’s at ω=287°W corresponds to BWl’s). EGf’s images on 9 Sept
(λ=257°Ls) at ω=269°W, and on 11 Sept (λ=258°Ls) at ω=283°W also show well Novus Mons.
B |
ill SHEEHAN (WSh) Observed at the Lick: SHEEHAN (WSh)
stayed at Mt Hamilton, California, from 28 August to 12 September together with
Tony MISCH, Laurie HATCH, & Rem STONE and
observed Mars securing a lot of drawings made by the use of the famous 91cm
refractor at the Lick Observatory: This refractor is the one used by E E BARNARD for example in 1894 when P LOWELL was first
chasing the planet at the same time at
http://mtham.ucolick.org/public/TwoWeeksOnMars/
During the fortnight, WSh watched the surfaces from
ω=084°W eastwardly to ω=265°W. The angular diameter was still
perfect, and the period corresponded to the good seeing season at Mt Hamilton.
We don’t exactly know how much Bill had already practised in observing Mars (we
know he gave several good drawings at the Pic du Midi), but we can readily judge the 91cm refractor
(maybe sometimes reduced to 50cm) gave him quite details from the outset. He
detected several minor dark spots following Solis L, and the complex structure
around Eos including the set of Electra and Orestes as well as Juventæ Fons. Furthermore he
depicted Aurea Cherso
clearly (2 Sept (λ=253°Ls) at ω=040°W). We suppose WSh must have minutely
investigated the area of Edom, and saw as byproducts
such a minor marking as Brangæna and the new big
marking of the expanded M Serpentis after the July
2003 dust (7 Sept (λ=256°Ls) at ω=326°W). Huygens Crater was spotted (11 Sept (λ=259°Ls), and there seem to be
visible several
In contrast to the limb-lacking images of ccd, WSh’s drawings
quite clearly show that the spc was totally inside the disk. WSh saw a
vanishing Thyles Mons on 29 August (λ=250°Ls) at ω=084°W.
Under a permission we here cite a Laurie
Hatch photo of William SHEEHAN at the eyepiece of the 91cm wearing a T-shirt of
another William S (© 2003-2004 Laurie Hatch, all rights reserved. Nobody should use or reproduce without her
permission).
Laurie HATCH is a professional
photographer at the Lick and, as remarked above, joined the Two Weeks observation
team. Her excellent colour drawings of the red planet are also found on a page
of the above URL.
I |
mpressives: Without hesitation, Canon LAU (CLa)’s set of images on 9 Sept (λ=257°Ls) at ω=061°W ~ 127°W
should be praiseworthy. The file is good in the sense it is composed of a long
series of images showing the de-concentration of the morning mist. Another image
that is very
T |
he next issue shall treat
the observations made in the second half of September 2003 from 16 September
(λ=262°Ls, δ=23.4") to 30 September 2003 (λ=270°Ls,
δ=20.9").
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